Oganesson

<h2 id="introduction">Introduction</h2>
This section is an excerpt from <a href="/facts/Superheavy_element/9PjYvCc3">Superheavy element § Introduction</a>.[<a href="https://en.wikipedia.org/w/index.php?title=Superheavy_element&action=edit">edit</a>]
<h3>Synthesis of superheavy nuclei</h3>

A superheavy<a class="footnote-ref" id="fnref:6" href="#fn:6">6</a> <a href="/facts/Atomic_nucleus/orpIm5Xl">atomic nucleus</a> is created in a nuclear reaction that combines two other nuclei of unequal size<a class="footnote-ref" id="fnref:7" href="#fn:7">7</a> into one; roughly, the more unequal the two nuclei in terms of <a href="/facts/Mass/HHdc8XmF">mass</a>, the greater the possibility that the two react.<a class="footnote-ref" id="fnref:8" href="#fn:8">8</a> The material made of the heavier nuclei is made into a target, which is then bombarded by the <a href="/facts/Particle_beam/mg5EIlWb">beam</a> of lighter nuclei. Two nuclei can only <a href="/facts/Nuclear_fusion/hP0gLDqj">fuse</a> into one if they approach each other closely enough; normally, nuclei (all positively charged) repel each other due to <a href="/facts/Coulomb%2527s_law/V0lR5NKv">electrostatic repulsion</a>. The <a href="/facts/Strong_interaction/JjRsKcLg">strong interaction</a> can overcome this repulsion but only within a very short distance from a nucleus; beam nuclei are thus greatly <a href="/facts/Particle_accelerator/Pkuc08xC">accelerated</a> in order to make such repulsion insignificant compared to the velocity of the beam nucleus.[24] The energy applied to the beam nuclei to accelerate them can cause them to reach speeds as high as one-tenth of the <a href="/facts/Speed_of_light/sKSQwdNx">speed of light</a>. However, if too much energy is applied, the beam nucleus can fall apart.[24]
Coming close enough alone is not enough for two nuclei to fuse: when two nuclei approach each other, they usually remain together for about 10−20 seconds and then part ways (not necessarily in the same composition as before the reaction) rather than form a single nucleus.[24]<a class="footnote-ref" id="fnref:9" href="#fn:9">9</a> This happens because during the attempted formation of a single nucleus, electrostatic repulsion tears apart the nucleus that is being formed.[24] Each pair of a target and a beam is characterized by its <a href="/facts/Cross_section_(physics)/lo014h2D">cross section</a>—the probability that fusion will occur if two nuclei approach one another expressed in terms of the transverse area that the incident particle must hit in order for the fusion to occur.<a class="footnote-ref" id="fnref:10" href="#fn:10">10</a> This fusion may occur as a result of the quantum effect in which nuclei can <a href="/facts/Quantum_tunnelling/WU4NMrKx">tunnel</a> through electrostatic repulsion. If the two nuclei can stay close past that phase, multiple nuclear interactions result in redistribution of energy and an energy equilibrium.[24]

The resulting merger is an <a href="/facts/Excited_state/czcLYNnr">excited state</a><a class="footnote-ref" id="fnref:11" href="#fn:11">11</a>—termed a <a href="/facts/Nuclear_reaction/202yClUr">compound nucleus</a>—and thus it is very unstable.[24] To reach a more stable state, the temporary merger may <a href="/facts/Nuclear_fission/LfkIylvm">fission</a> without formation of a more stable nucleus.<a class="footnote-ref" id="fnref:12" href="#fn:12">12</a> Alternatively, the compound nucleus may eject a few <a href="/facts/Neutron/oRCM1geb">neutrons</a>, which would carry away the excitation energy; if the latter is not sufficient for a neutron expulsion, the merger would produce a <a href="/facts/Gamma_ray/5Drf913J">gamma ray</a>. This happens in about 10−16 seconds after the initial nuclear collision and results in creation of a more stable nucleus.<a class="footnote-ref" id="fnref:13" href="#fn:13">13</a> The definition by the <a href="/facts/IUPAC%2fIUPAP_Joint_Working_Party/1mKaf9UW">IUPAC/IUPAP Joint Working Party</a> (JWP) states that a <a href="/facts/Chemical_element/0jducgWD">chemical element</a> can only be recognized as discovered if a nucleus of it has not <a href="/facts/Radioactive_decay/Ya6FVjt4">decayed</a> within 10−14 seconds. This value was chosen as an estimate of how long it takes a nucleus to acquire <a href="/facts/Electron/L0KBo5cW">electrons</a> and thus display its chemical properties.<a class="footnote-ref" id="fnref:14" href="#fn:14">14</a><a class="footnote-ref" id="fnref:15" href="#fn:15">15</a>

<h3>Decay and detection</h3>
The beam passes through the target and reaches the next chamber, the separator; if a new nucleus is produced, it is carried with this beam.<a class="footnote-ref" id="fnref:16" href="#fn:16">16</a> In the separator, the newly produced nucleus is separated from other nuclides (that of the original beam and any other reaction products)<a class="footnote-ref" id="fnref:17" href="#fn:17">17</a> and transferred to a <a href="/facts/Semiconductor_detector/HzvpIobR">surface-barrier detector</a>, which stops the nucleus. The exact location of the upcoming impact on the detector is marked; also marked are its energy and the time of the arrival.<a class="footnote-ref" id="fnref:18" href="#fn:18">18</a> The transfer takes about 10−6 seconds; in order to be detected, the nucleus must survive this long.<a class="footnote-ref" id="fnref:19" href="#fn:19">19</a> The nucleus is recorded again once its decay is registered, and the location, the <a href="/facts/Decay_energy/g4wDGC8r">energy</a>, and the time of the decay are measured.<a class="footnote-ref" id="fnref:20" href="#fn:20">20</a>
Stability of a nucleus is provided by the strong interaction. However, its range is very short; as nuclei become larger, its influence on the outermost <a href="/facts/Nucleon/6fguU9Xk">nucleons</a> (<a href="/facts/Proton/clCjepXP">protons</a> and neutrons) weakens. At the same time, the nucleus is torn apart by electrostatic repulsion between protons, and its range is not limited.<a class="footnote-ref" id="fnref:21" href="#fn:21">21</a> Total <a href="/facts/Nuclear_binding_energy/PU8bREHW">binding energy</a> provided by the strong interaction increases linearly with the number of nucleons, whereas electrostatic repulsion increases with the square of the atomic number, i.e. the latter grows faster and becomes increasingly important for heavy and superheavy nuclei.<a class="footnote-ref" id="fnref:22" href="#fn:22">22</a><a class="footnote-ref" id="fnref:23" href="#fn:23">23</a> Superheavy nuclei are thus theoretically predicted<a class="footnote-ref" id="fnref:24" href="#fn:24">24</a> and have so far been observed<a class="footnote-ref" id="fnref:25" href="#fn:25">25</a> to predominantly decay via decay modes that are caused by such repulsion: <a href="/facts/Alpha_decay/rCsHNIUE">alpha decay</a> and <a href="/facts/Spontaneous_fission/0QuJoVKI">spontaneous fission</a>.<a class="footnote-ref" id="fnref:26" href="#fn:26">26</a> Almost all alpha emitters have over 210 nucleons,<a class="footnote-ref" id="fnref:27" href="#fn:27">27</a> and the lightest nuclide primarily undergoing spontaneous fission has 238.<a class="footnote-ref" id="fnref:28" href="#fn:28">28</a> In both decay modes, nuclei are inhibited from decaying by corresponding <a href="/facts/Rectangular_potential_barrier/Cer7zMUn">energy barriers</a> for each mode, but they can be tunneled through.<a class="footnote-ref" id="fnref:29" href="#fn:29">29</a><a class="footnote-ref" id="fnref:30" href="#fn:30">30</a>

Alpha particles are commonly produced in radioactive decays because the mass of an alpha particle per nucleon is small enough to leave some energy for the alpha particle to be used as kinetic energy to leave the nucleus.<a class="footnote-ref" id="fnref:31" href="#fn:31">31</a> Spontaneous fission is caused by electrostatic repulsion tearing the nucleus apart and produces various nuclei in different instances of identical nuclei fissioning.<a class="footnote-ref" id="fnref:32" href="#fn:32">32</a> As the atomic number increases, spontaneous fission rapidly becomes more important: spontaneous fission partial half-lives decrease by 23 orders of magnitude from <a href="/facts/Uranium/n2sGWBzU">uranium</a> (element 92) to <a href="/facts/Nobelium/syRkloSw">nobelium</a> (element 102),<a class="footnote-ref" id="fnref:33" href="#fn:33">33</a> and by 30 orders of magnitude from <a href="/facts/Thorium/ysdWH470">thorium</a> (element 90) to <a href="/facts/Fermium/Us3rnvG5">fermium</a> (element 100).<a class="footnote-ref" id="fnref:34" href="#fn:34">34</a> The earlier <a href="/facts/Liquid_drop_model/XQhTYz7e">liquid drop model</a> thus suggested that spontaneous fission would occur nearly instantly due to disappearance of the <a href="/facts/Fission_barrier/Xt5xoTpB">fission barrier</a> for nuclei with about 280 nucleons.<a class="footnote-ref" id="fnref:35" href="#fn:35">35</a><a class="footnote-ref" id="fnref:36" href="#fn:36">36</a> The later <a href="/facts/Nuclear_shell_model/1Qgep495">nuclear shell model</a> suggested that nuclei with about 300 nucleons would form an <a href="/facts/Island_of_stability/XuxQzqjL">island of stability</a> in which nuclei will be more resistant to spontaneous fission and will primarily undergo alpha decay with longer half-lives.<a class="footnote-ref" id="fnref:37" href="#fn:37">37</a><a class="footnote-ref" id="fnref:38" href="#fn:38">38</a> Subsequent discoveries suggested that the predicted island might be further than originally anticipated; they also showed that nuclei intermediate between the long-lived actinides and the predicted island are deformed, and gain additional stability from shell effects.<a class="footnote-ref" id="fnref:39" href="#fn:39">39</a> Experiments on lighter superheavy nuclei,<a class="footnote-ref" id="fnref:40" href="#fn:40">40</a> as well as those closer to the expected island,<a class="footnote-ref" id="fnref:41" href="#fn:41">41</a> have shown greater than previously anticipated stability against spontaneous fission, showing the importance of shell effects on nuclei.<a class="footnote-ref" id="fnref:42" href="#fn:42">42</a>
Alpha decays are registered by the emitted alpha particles, and the decay products are easy to determine before the actual decay; if such a decay or a series of consecutive decays produces a known nucleus, the original product of a reaction can be easily determined.<a class="footnote-ref" id="fnref:43" href="#fn:43">43</a> (That all decays within a decay chain were indeed related to each other is established by the location of these decays, which must be in the same place.)<a class="footnote-ref" id="fnref:44" href="#fn:44">44</a> The known nucleus can be recognized by the specific characteristics of decay it undergoes such as decay energy (or more specifically, the <a href="/facts/Kinetic_energy/aJRxUd4p">kinetic energy</a> of the emitted particle).<a class="footnote-ref" id="fnref:45" href="#fn:45">45</a> Spontaneous fission, however, produces various nuclei as products, so the original nuclide cannot be determined from its daughters.<a class="footnote-ref" id="fnref:46" href="#fn:46">46</a>

The information available to physicists aiming to synthesize a superheavy element is thus the information collected at the detectors: location, energy, and time of arrival of a particle to the detector, and those of its decay. The physicists analyze this data and seek to conclude that it was indeed caused by a new element and could not have been caused by a different nuclide than the one claimed. Often, provided data is insufficient for a conclusion that a new element was definitely created and there is no other explanation for the observed effects; errors in interpreting data have been made.<a class="footnote-ref" id="fnref:47" href="#fn:47">47</a>
<h2 id="history">History</h2>
See also: <a href="/facts/Timeline_of_chemical_element_discoveries/QY4X2RP3">Timeline of chemical element discoveries</a>
<h3>Early speculation</h3>
The possibility of a seventh <a href="/facts/Noble_gas/j0yHMEAE">noble gas</a>, after <a href="/facts/Helium/yRul93TG">helium</a>, <a href="/facts/Neon/5bF1FwGL">neon</a>, <a href="/facts/Argon/QX6NRH6d">argon</a>, <a href="/facts/Krypton/llkNlCke">krypton</a>, <a href="/facts/Xenon/9E3XR69R">xenon</a>, and <a href="/facts/Radon/0V9arWKl">radon</a>, was considered almost as soon as the noble gas group was discovered. Danish chemist <a href="/facts/Hans_Peter_J%25C3%25B8rgen_Julius_Thomsen/QINr2v4E">Hans Peter Jørgen Julius Thomsen</a> predicted in April 1895, the year after the discovery of argon, that there was a whole series of chemically inert gases similar to argon that would bridge the <a href="/facts/Halogen/YeFgWHeA">halogen</a> and <a href="/facts/Alkali_metal/IkWbCLk2">alkali metal</a> groups: he expected that the seventh of this series would end a 32-element period which contained <a href="/facts/Thorium/ysdWH470">thorium</a> and <a href="/facts/Uranium/n2sGWBzU">uranium</a> and have an atomic weight of 292, close to the 294 now known for the first and only confirmed <a href="/facts/Isotope/KD9B1y6o">isotope</a> of oganesson.<a class="footnote-ref" id="fnref:48" href="#fn:48">48</a> Danish physicist <a href="/facts/Niels_Bohr/ydLPvQXT">Niels Bohr</a> noted in 1922 that this seventh noble gas should have atomic number 118 and predicted its electronic structure as 2, 8, 18, 32, 32, 18, 8, matching modern predictions.<a class="footnote-ref" id="fnref:49" href="#fn:49">49</a> Following this, German chemist <a href="/facts/Aristid_von_Grosse/Ed81bS6j">Aristid von Grosse</a> wrote an article in 1965 predicting the likely properties of element 118.<a class="footnote-ref" id="fnref:50" href="#fn:50">50</a> It was 107 years from Thomsen's prediction before oganesson was successfully synthesized, although its chemical properties have not been investigated to determine if it behaves as the heavier <a href="/facts/Congener_(chemistry)/8qy2rvGG">congener</a> of radon.<a class="footnote-ref" id="fnref:51" href="#fn:51">51</a> In a 1975 article, American chemist <a href="/facts/Kenneth_Pitzer/oIjnuHrA">Kenneth Pitzer</a> suggested that element 118 should be a <a href="/facts/Gas/hVVAoodV">gas</a> or <a href="/facts/Volatility_(chemistry)/90r3ep6w">volatile</a> <a href="/facts/Liquid/t9GkLWzt">liquid</a> due to <a href="/facts/Relativistic_quantum_chemistry/8A1se1CS">relativistic effects</a>.<a class="footnote-ref" id="fnref:52" href="#fn:52">52</a>

<h3>Unconfirmed discovery claims</h3>
In late 1998, Polish physicist <a href="/facts/Robert_Smola%25C5%2584czuk/qHwnDaCE">Robert Smolańczuk</a> published calculations on the fusion of atomic nuclei towards the synthesis of <a href="/facts/Superheavy_element/9PjYvCc3">superheavy atoms</a>, including oganesson.<a class="footnote-ref" id="fnref:53" href="#fn:53">53</a> His calculations suggested that it might be possible to make element 118 by fusing <a href="/facts/Lead/EYljasJN">lead</a> with <a href="/facts/Krypton/llkNlCke">krypton</a> under carefully controlled conditions, and that the fusion probability (<a href="/facts/Cross_section_(physics)/lo014h2D">cross section</a>) of that reaction would be close to the lead–<a href="/facts/Chromium/6sVk6Uu7">chromium</a> reaction that had produced element 106, <a href="/facts/Seaborgium/ejs0Ap6P">seaborgium</a>. This contradicted predictions that the cross sections for reactions with lead or <a href="/facts/Bismuth/75FLjkoX">bismuth</a> targets would go down exponentially as the atomic number of the resulting elements increased.<a class="footnote-ref" id="fnref:54" href="#fn:54">54</a>
In 1999, researchers at <a href="/facts/Lawrence_Berkeley_National_Laboratory/tvjPSwC9">Lawrence Berkeley National Laboratory</a> made use of these predictions and announced the discovery of elements 118 and <a href="/facts/Livermorium/nQc1FE6E">116</a>, in a paper published in <a href="/facts/Physical_Review_Letters/rNP3XvYq">Physical Review Letters</a>,<a class="footnote-ref" id="fnref:55" href="#fn:55">55</a> and very soon after the results were reported in <a href="/facts/Science_(journal)/uTyzjkwD">Science</a>.<a class="footnote-ref" id="fnref:56" href="#fn:56">56</a> The researchers reported that they had performed the <a href="/facts/Nuclear_reaction/202yClUr">reaction</a>

<a href="/facts/Lead-208/V9JFUTRo">20882Pb</a> + <a href="/facts/Krypton-86/8hRKYepJ">8636Kr</a> → 293118Og + <a href="/facts/Neutron/oRCM1geb">n</a>.
In 2001, they published a retraction after researchers at other laboratories were unable to duplicate the results and the Berkeley lab could not duplicate them either.<a class="footnote-ref" id="fnref:57" href="#fn:57">57</a> In June 2002, the director of the lab announced that the original claim of the discovery of these two elements had been based on data fabricated by principal author <a href="/facts/Victor_Ninov/G9wpbGj9">Victor Ninov</a>.<a class="footnote-ref" id="fnref:58" href="#fn:58">58</a><a class="footnote-ref" id="fnref:59" href="#fn:59">59</a> Newer experimental results and theoretical predictions have confirmed the exponential decrease in cross sections with lead and bismuth targets as the atomic number of the resulting nuclide increases.<a class="footnote-ref" id="fnref:60" href="#fn:60">60</a>

<h3>Discovery reports</h3>

The first genuine decay of atoms of oganesson was observed in 2002 at the <a href="/facts/Joint_Institute_for_Nuclear_Research/JrSF8sQQ">Joint Institute for Nuclear Research</a> (JINR) in <a href="/facts/Dubna/mn37rc4l">Dubna</a>, Russia, by a joint team of Russian and American scientists. Headed by <a href="/facts/Yuri_Oganessian/69TJ9VyW">Yuri Oganessian</a>, a Russian nuclear physicist of Armenian ethnicity, the team included American scientists from the <a href="/facts/Lawrence_Livermore_National_Laboratory/WuXIbIKz">Lawrence Livermore National Laboratory</a> in California.<a class="footnote-ref" id="fnref:61" href="#fn:61">61</a> The discovery was not announced immediately, because the decay energy of 294Og matched that of <a href="/facts/Isotopes_of_polonium/bIdUTjCm">212mPo</a>, a common impurity produced in fusion reactions aimed at producing superheavy elements, and thus announcement was delayed until after a 2005 confirmatory experiment aimed at producing more oganesson atoms.<a class="footnote-ref" id="fnref:62" href="#fn:62">62</a> The 2005 experiment used a different beam energy (251 MeV instead of 245 MeV) and target thickness (0.34 mg/cm2 instead of 0.23 mg/cm2).<a class="footnote-ref" id="fnref:63" href="#fn:63">63</a> On 9 October 2006, the researchers announced<a class="footnote-ref" id="fnref:64" href="#fn:64">64</a> that they had indirectly detected a total of three (possibly four) nuclei of oganesson-294 (one or two in 2002<a class="footnote-ref" id="fnref:65" href="#fn:65">65</a> and two more in 2005) produced via collisions of <a href="/facts/Californium/AJVjoVut">californium</a>-249 atoms and <a href="/facts/Calcium-48/cqqfNkMY">calcium-48</a> ions.<a class="footnote-ref" id="fnref:66" href="#fn:66">66</a><a class="footnote-ref" id="fnref:67" href="#fn:67">67</a><a class="footnote-ref" id="fnref:68" href="#fn:68">68</a><a class="footnote-ref" id="fnref:69" href="#fn:69">69</a><a class="footnote-ref" id="fnref:70" href="#fn:70">70</a>

<a href="/facts/Californium-249/tX06MlFX">24998Cf</a> + <a href="/facts/Calcium-48/cqqfNkMY">4820Ca</a> → <a href="/facts/Oganesson-294/pkoyugEy">294118Og</a> + 3 <a href="/facts/Neutron/oRCM1geb">n</a>.
In 2011, <a href="/facts/IUPAC/2AV6myCK">IUPAC</a> evaluated the 2006 results of the Dubna–Livermore collaboration and concluded: "The three events reported for the Z = 118 isotope have very good internal
redundancy but with no anchor to known nuclei do not satisfy the criteria for discovery".<a class="footnote-ref" id="fnref:71" href="#fn:71">71</a>
Because of the very small <a href="/facts/Fusion_reaction/hP0gLDqj">fusion reaction</a> probability (the fusion <a href="/facts/Nuclear_cross_section/AtghNytD">cross section</a> is ~0.3–0.6 <a href="/facts/Barn_(unit)/0yCEtKJ9">pb</a> or (3–6)×10−41 m2) the experiment took four months and involved a beam dose of 2.5×1019 <a href="/facts/Calcium/hf252CC0">calcium</a> ions that had to be shot at the <a href="/facts/Californium/AJVjoVut">californium</a> target to produce the first recorded event believed to be the synthesis of oganesson.<a class="footnote-ref" id="fnref:72" href="#fn:72">72</a> Nevertheless, researchers were highly confident that the results were not a <a href="/facts/False_positive/jkC44hML">false positive</a>, since the chance that the detections were random events was estimated to be less than one part in 100000.<a class="footnote-ref" id="fnref:73" href="#fn:73">73</a>
In the experiments, the alpha-decay of three atoms of oganesson was observed. A fourth decay by direct <a href="/facts/Spontaneous_fission/0QuJoVKI">spontaneous fission</a> was also proposed. A <a href="/facts/Half-life/kGVH8BAB">half-life</a> of 0.89 ms was calculated: 294Og decays into <a href="/facts/Isotopes_of_livermorium/GVATCnsS">290Lv</a> by <a href="/facts/Alpha_decay/rCsHNIUE">alpha decay</a>. Since there were only three nuclei, the half-life derived from observed lifetimes has a large uncertainty: 0.89+1.07−0.31 ms.<a class="footnote-ref" id="fnref:74" href="#fn:74">74</a>

294118Og → 290116Lv + <a href="/facts/Helium-4/vNsL5qhC">42He</a>
The identification of the 294Og nuclei was verified by separately creating the putative <a href="/facts/Decay_product/hT0obfLv">daughter nucleus</a> 290Lv directly by means of a bombardment of <a href="/facts/Curium-245/WnMh6VLE">245Cm</a> with <a href="/facts/Calcium-48/cqqfNkMY">48Ca</a> ions,

24596Cm + 4820Ca → 290116Lv + 3 <a href="/facts/Neutron/oRCM1geb">n</a>,
and checking that the 290Lv decay matched the <a href="/facts/Decay_chain/JvTwPNBn">decay chain</a> of the 294Og nuclei.<a class="footnote-ref" id="fnref:75" href="#fn:75">75</a> The daughter nucleus 290Lv is very unstable, decaying with a lifetime of 14 milliseconds into <a href="/facts/Flerovium-286/6zApqu7L">286Fl</a>, which may experience either spontaneous fission or alpha decay into <a href="/facts/Copernicium-282/ReN9zfcv">282Cn</a>, which will undergo spontaneous fission.<a class="footnote-ref" id="fnref:76" href="#fn:76">76</a>

<h3>Confirmation</h3>
In December 2015, the <a href="/facts/IUPAC%2fIUPAP_Joint_Working_Party/1mKaf9UW">Joint Working Party</a> of international scientific bodies <a href="/facts/International_Union_of_Pure_and_Applied_Chemistry/2AV6myCK">International Union of Pure and Applied Chemistry</a> (IUPAC) and <a href="/facts/International_Union_of_Pure_and_Applied_Physics/ah3BodlS">International Union of Pure and Applied Physics</a> (IUPAP) recognized the element's discovery and assigned the priority of the discovery to the Dubna–Livermore collaboration.<a class="footnote-ref" id="fnref:77" href="#fn:77">77</a> This was on account of two 2009 and 2010 confirmations of the properties of the granddaughter of 294Og, 286Fl, at the <a href="/facts/Lawrence_Berkeley_National_Laboratory/tvjPSwC9">Lawrence Berkeley National Laboratory</a>, as well as the observation of another consistent decay chain of 294Og by the Dubna group in 2012. The goal of that experiment had been the synthesis of 294Ts via the reaction 249Bk(48Ca,3n), but the short half-life of 249Bk resulted in a significant quantity of the target having decayed to 249Cf, resulting in the synthesis of oganesson instead of <a href="/facts/Tennessine/eGCBDvEr">tennessine</a>.<a class="footnote-ref" id="fnref:78" href="#fn:78">78</a>
From 1 October 2015 to 6 April 2016, the Dubna team performed a similar experiment with 48Ca projectiles aimed at a mixed-isotope californium target containing 249Cf, 250Cf, and 251Cf, with the aim of producing the heavier oganesson isotopes 295Og and 296Og. Two beam energies at 252 MeV and 258 MeV were used. Only one atom was seen at the lower beam energy, whose decay chain fitted the previously known one of 294Og (terminating with spontaneous fission of 286Fl), and none were seen at the higher beam energy. The experiment was then halted, as the glue from the sector frames covered the target and blocked evaporation residues from escaping to the detectors.<a class="footnote-ref" id="fnref:79" href="#fn:79">79</a> The production of 293Og and its daughter 289Lv, as well as the even heavier isotope 297Og, is also possible using this reaction. The isotopes 295Og and 296Og may also be produced in the fusion of 248Cm with 50Ti projectiles.<a class="footnote-ref" id="fnref:80" href="#fn:80">80</a><a class="footnote-ref" id="fnref:81" href="#fn:81">81</a><a class="footnote-ref" id="fnref:82" href="#fn:82">82</a> A search beginning in summer 2016 at RIKEN for 295Og in the 3n channel of this reaction was unsuccessful, though the study is planned to resume; a detailed analysis and cross section limit were not provided. These heavier and likely more stable isotopes may be useful in probing the chemistry of oganesson.<a class="footnote-ref" id="fnref:83" href="#fn:83">83</a><a class="footnote-ref" id="fnref:84" href="#fn:84">84</a>

<h3>Naming</h3>

Using <a href="/facts/Mendeleev%2527s_predicted_elements/C4vgW0uy">Mendeleev's nomenclature for unnamed and undiscovered elements</a>, oganesson is sometimes known as eka-radon (until the 1960s as eka-emanation, emanation being the old name for <a href="/facts/Radon/0V9arWKl">radon</a>).<a class="footnote-ref" id="fnref:85" href="#fn:85">85</a> In 1979, IUPAC assigned the <a href="/facts/Systematic_element_name/vJt86yzX">systematic</a> <a href="/facts/Placeholder_name/zf6Whtye">placeholder name</a> ununoctium to the undiscovered element, with the corresponding symbol of Uuo,<a class="footnote-ref" id="fnref:86" href="#fn:86">86</a> and recommended that it be used until after confirmed discovery of the element.<a class="footnote-ref" id="fnref:87" href="#fn:87">87</a> Although widely used in the chemical community on all levels, from chemistry classrooms to advanced textbooks, the recommendations were mostly ignored among scientists in the field, who called it "element 118", with the symbol of E118, (118), or simply 118.<a class="footnote-ref" id="fnref:88" href="#fn:88">88</a>
Before the retraction in 2001, the researchers from Berkeley had intended to name the element ghiorsium (Gh), after <a href="/facts/Albert_Ghiorso/jP5gHCwp">Albert Ghiorso</a> (a leading member of the research team).<a class="footnote-ref" id="fnref:89" href="#fn:89">89</a>
The Russian discoverers reported their synthesis in 2006. According to IUPAC recommendations, the discoverers of a new element have the right to suggest a name.<a class="footnote-ref" id="fnref:90" href="#fn:90">90</a> In 2007, the head of the Russian institute stated the team were considering two names for the new element: flyorium, in honor of <a href="/facts/Georgy_Flyorov/qhcQHs2q">Georgy Flyorov</a>, the founder of the research laboratory in Dubna; and moskovium, in recognition of the <a href="/facts/Moscow_Oblast/699h9DNN">Moscow Oblast</a> where Dubna is located.<a class="footnote-ref" id="fnref:91" href="#fn:91">91</a> He also stated that although the element was discovered as an American collaboration, who provided the californium target, the element should rightly be named in honor of Russia since the <a href="/facts/Flyorov_Laboratory_of_Nuclear_Reactions/JrSF8sQQ">Flyorov Laboratory of Nuclear Reactions</a> at JINR was the only facility in the world which could achieve this result.<a class="footnote-ref" id="fnref:92" href="#fn:92">92</a> These names were later suggested for <a href="/facts/Flerovium/Aa7uGMuG">element 114</a> (flerovium) and <a href="/facts/Livermorium/nQc1FE6E">element 116</a> (moscovium).<a class="footnote-ref" id="fnref:93" href="#fn:93">93</a> Flerovium became the name of element 114; the final name proposed for element 116 was instead livermorium,<a class="footnote-ref" id="fnref:94" href="#fn:94">94</a> with moscovium later being proposed and accepted for <a href="/facts/Moscovium/QhSEr0H5">element 115</a> instead.<a class="footnote-ref" id="fnref:95" href="#fn:95">95</a>
Traditionally, the names of all <a href="/facts/Noble_gas/j0yHMEAE">noble gases</a> end in "-on", with the exception of <a href="/facts/Helium/yRul93TG">helium</a>, which was not known to be a noble gas when discovered. The IUPAC guidelines valid at the moment of the discovery approval however required all new elements be named with the ending "-ium", even if they turned out to be <a href="/facts/Halogen/YeFgWHeA">halogens</a> (traditionally ending in "-ine") or noble gases (traditionally ending in "-on").<a class="footnote-ref" id="fnref:96" href="#fn:96">96</a> While the provisional name ununoctium followed this convention, a new IUPAC recommendation published in 2016 recommended using the "-on" ending for new <a href="/facts/Group_18_element/j0yHMEAE">group 18 elements</a>, regardless of whether they turn out to have the chemical properties of a noble gas.<a class="footnote-ref" id="fnref:97" href="#fn:97">97</a>
The scientists involved in the discovery of element 118, as well as those of <a href="/facts/Tennessine/eGCBDvEr">117</a> and <a href="/facts/Moscovium/QhSEr0H5">115</a>, held a conference call on 23 March 2016 to decide their names. Element 118 was the last to be decided upon; after Oganessian was asked to leave the call, the remaining scientists unanimously decided to have the element "oganesson" after him. Oganessian was a pioneer in superheavy element research for sixty years reaching back to the field's foundation: his team and his proposed techniques had led directly to the synthesis of elements <a href="/facts/Bohrium/epvp3GWM">107</a> through 118. Mark Stoyer, a nuclear chemist at the LLNL, later recalled, "We had intended to propose that name from Livermore, and things kind of got proposed at the same time from multiple places. I don't know if we can claim that we actually proposed the name, but we had intended it."<a class="footnote-ref" id="fnref:98" href="#fn:98">98</a>
In internal discussions, IUPAC asked the JINR if they wanted the element to be spelled "oganeson" to match the Russian spelling more closely. Oganessian and the JINR refused this offer, citing the Soviet-era practice of transliterating names into the Latin alphabet under the rules of the French language ("Oganessian" is such a transliteration) and arguing that "oganesson" would be easier to link to the person.<a class="footnote-ref" id="fnref:99" href="#fn:99">99</a><a class="footnote-ref" id="fnref:100" href="#fn:100">100</a>
In June 2016, IUPAC announced that the discoverers planned to give the element the name oganesson (symbol: Og). The name became official on 28 November 2016.<a class="footnote-ref" id="fnref:101" href="#fn:101">101</a> In 2017, Oganessian commented on the naming:<a class="footnote-ref" id="fnref:102" href="#fn:102">102</a>

<blockquote>For me, it is an honour. The discovery of element 118 was by scientists at the Joint Institute for Nuclear Research in Russia and at the Lawrence Livermore National Laboratory in the US, and it was my colleagues who proposed the name oganesson. My children and grandchildren have been living in the US for decades, but my daughter wrote to me to say that she did not sleep the night she heard because she was crying.<a class="footnote-ref" id="fnref:103" href="#fn:103">103</a>— Yuri Oganessian</blockquote>
The naming ceremony for moscovium, tennessine, and oganesson was held on 2 March 2017 at the <a href="/facts/Russian_Academy_of_Sciences/RuUqhtFb">Russian Academy of Sciences</a> in Moscow.<a class="footnote-ref" id="fnref:104" href="#fn:104">104</a>
In a 2019 interview, when asked what it was like to see his name in the periodic table next to <a href="/facts/Albert_Einstein/CNTet8qu">Einstein</a>, <a href="/facts/Dmitry_Mendeleev/xdouRrx8">Mendeleev</a>, <a href="/facts/Curie_family/zQYAkhK7">the Curies</a>, and <a href="/facts/Ernest_Rutherford/hjjMEskl">Rutherford</a>, Oganessian responded:<a class="footnote-ref" id="fnref:105" href="#fn:105">105</a>

<blockquote>Not like much! You see, not like much. It is customary in science to name something new after its discoverer. It's just that there are few elements, and this happens rarely. But look at how many equations and theorems in mathematics are named after somebody. And in medicine? <a href="/facts/Alzheimer%2527s_disease/w7Ad6tdg">Alzheimer</a>, <a href="/facts/Parkinson%2527s_disease/xpekKj6x">Parkinson</a>. There's nothing special about it.</blockquote>
<h2 id="characteristics">Characteristics</h2>
Other than nuclear properties, no properties of oganesson or its compounds have been measured; this is due to its extremely limited and expensive production<a class="footnote-ref" id="fnref:106" href="#fn:106">106</a> and the fact that it decays very quickly. Thus only predictions are available.

<h3>Nuclear stability and isotopes</h3>
Main article: <a href="/facts/Isotopes_of_oganesson/pkoyugEy">Isotopes of oganesson</a>

The stability of nuclei quickly decreases with the increase in atomic number after <a href="/facts/Curium/LMyWXg8l">curium</a>, element 96, whose most stable isotope, <a href="/facts/Isotopes_of_curium/WnMh6VLE">247Cm</a>, has a half-life four orders of magnitude longer than that of any subsequent element. All nuclides with an atomic number above <a href="/facts/Mendelevium/bEHBu18F">101</a> undergo radioactive decay with half-lives shorter than 30 hours. No elements with atomic numbers above 82 (after <a href="/facts/Lead/EYljasJN">lead</a>) have stable isotopes.<a class="footnote-ref" id="fnref:107" href="#fn:107">107</a> This is because of the ever-increasing <a href="/facts/Coulomb_repulsion/V0lR5NKv">Coulomb repulsion</a> of protons, so that the <a href="/facts/Strong_nuclear_force/JjRsKcLg">strong nuclear force</a> cannot hold the nucleus together against <a href="/facts/Spontaneous_fission/0QuJoVKI">spontaneous fission</a> for long. Calculations suggest that in the absence of other stabilizing factors, elements with more than <a href="/facts/Rutherfordium/44LSnv9p">104 protons</a> should not exist.<a class="footnote-ref" id="fnref:108" href="#fn:108">108</a> However, researchers in the 1960s suggested that the closed <a href="/facts/Nuclear_shell_model/1Qgep495">nuclear shells</a> around 114 protons and 184 neutrons should counteract this instability, creating an <a href="/facts/Island_of_stability/XuxQzqjL">island of stability</a> in which nuclides could have half-lives reaching thousands or millions of years. While scientists have still not reached the island, the mere existence of the <a href="/facts/Superheavy_element/9PjYvCc3">superheavy elements</a> (including oganesson) confirms that this stabilizing effect is real, and in general the known superheavy nuclides become exponentially longer-lived as they approach the predicted location of the island.<a class="footnote-ref" id="fnref:109" href="#fn:109">109</a><a class="footnote-ref" id="fnref:110" href="#fn:110">110</a> Oganesson is <a href="/facts/Radioactive/Ya6FVjt4">radioactive</a>, decaying via <a href="/facts/Alpha_decay/rCsHNIUE">alpha decay</a> and spontaneous fission,<a class="footnote-ref" id="fnref:111" href="#fn:111">111</a><a class="footnote-ref" id="fnref:112" href="#fn:112">112</a> with a <a href="/facts/Half-life/kGVH8BAB">half-life</a> that appears to be less than a <a href="/facts/Millisecond/xHCyv235">millisecond</a>. Nonetheless, this is still longer than some predicted values.<a class="footnote-ref" id="fnref:113" href="#fn:113">113</a><a class="footnote-ref" id="fnref:114" href="#fn:114">114</a>
Calculations using a quantum-tunneling model predict the existence of several heavier isotopes of oganesson with alpha-decay half-lives close to 1 ms.<a class="footnote-ref" id="fnref:115" href="#fn:115">115</a><a class="footnote-ref" id="fnref:116" href="#fn:116">116</a>
Theoretical calculations done on the synthetic pathways for, and the half-life of, other <a href="/facts/Isotopes_of_oganesson/pkoyugEy">isotopes</a> have shown that some could be slightly more <a href="/facts/Stable_isotope/vgcdxgjA">stable</a> than the synthesized isotope 294Og, most likely 293Og, 295Og, 296Og, 297Og, 298Og, 300Og and 302Og (the last reaching the N = 184 shell closure).<a class="footnote-ref" id="fnref:117" href="#fn:117">117</a><a class="footnote-ref" id="fnref:118" href="#fn:118">118</a> Of these, 297Og might provide the best chances for obtaining longer-lived nuclei,<a class="footnote-ref" id="fnref:119" href="#fn:119">119</a><a class="footnote-ref" id="fnref:120" href="#fn:120">120</a> and thus might become the focus of future work with this element. Some isotopes with many more neutrons, such as some located around 313Og, could also provide longer-lived nuclei.<a class="footnote-ref" id="fnref:121" href="#fn:121">121</a> The isotopes from 291Og to 295Og might be produced as daughters of <a href="/facts/Unbinilium/gUvSSHzd">element 120</a> isotopes that can be reached in the reactions 249–251Cf+50Ti, 245Cm+48Ca, and 248Cm+48Ca.<a class="footnote-ref" id="fnref:122" href="#fn:122">122</a>
In a <a href="/facts/Quantum_tunneling/WU4NMrKx">quantum-tunneling model</a>, the alpha decay half-life of 294Og was predicted to be 0.66+0.23−0.18 ms<a class="footnote-ref" id="fnref:123" href="#fn:123">123</a> with the experimental <a href="/facts/Q_value_(nuclear_science)/HwpEN30F">Q-value</a> published in 2004.<a class="footnote-ref" id="fnref:124" href="#fn:124">124</a> Calculation with theoretical Q-values from the macroscopic-microscopic model of Muntian–Hofman–Patyk–Sobiczewski gives somewhat lower but comparable results.<a class="footnote-ref" id="fnref:125" href="#fn:125">125</a>

<h3>Calculated atomic and physical properties</h3>
Oganesson is a member of <a href="/facts/Noble_gas/j0yHMEAE">group 18</a>, the zero-<a href="/facts/Valency_(chemistry)/ck7cHByj">valence</a> elements. The members of this group are usually inert to most common chemical reactions (for example, combustion) because the outer <a href="/facts/Valence_shell/mXPA15VP">valence shell</a> is completely filled with <a href="/facts/Octet_rule/X9jxSsos">eight electrons</a>. This produces a stable, minimum energy configuration in which the outer electrons are tightly bound.<a class="footnote-ref" id="fnref:126" href="#fn:126">126</a> It is thought that similarly, oganesson has a <a href="/facts/Closed_shell/TQjRr22P">closed</a> outer valence shell in which its <a href="/facts/Valence_electron/mXPA15VP">valence electrons</a> are arranged in a 7s27p6 <a href="/facts/Electron_configuration/TQjRr22P">configuration</a>.<a class="footnote-ref" id="fnref:127" href="#fn:127">127</a>
Consequently, some expect oganesson to have similar physical and chemical properties to other members of its group, most closely resembling the noble gas above it in the periodic table, <a href="/facts/Radon/0V9arWKl">radon</a>.<a class="footnote-ref" id="fnref:128" href="#fn:128">128</a>
Following the <a href="/facts/Periodic_trend/dI0mkSju">periodic trend</a>, oganesson would be expected to be slightly more reactive than radon. However, theoretical calculations have shown that it could be significantly more reactive.<a class="footnote-ref" id="fnref:129" href="#fn:129">129</a> In addition to being far more reactive than radon, oganesson may be even more reactive than the elements <a href="/facts/Flerovium/Aa7uGMuG">flerovium</a> and <a href="/facts/Copernicium/EhgyBkg0">copernicium</a>, which are heavier homologs of the more chemically active elements <a href="/facts/Lead/EYljasJN">lead</a> and <a href="/facts/Mercury_(element)/WlxfoHva">mercury</a>, respectively.<a class="footnote-ref" id="fnref:130" href="#fn:130">130</a> The reason for the possible enhancement of the chemical activity of oganesson relative to radon is an energetic destabilization and a radial expansion of the last occupied 7p-<a href="/facts/Electron_shell/QxI30eh9">subshell</a>.<a class="footnote-ref" id="fnref:131" href="#fn:131">131</a> More precisely, considerable <a href="/facts/Spin%25E2%2580%2593orbit_interaction/Pv6maL1S">spin–orbit interactions</a> between the 7p electrons and the inert 7s electrons effectively lead to a second valence shell closing at <a href="/facts/Flerovium/Aa7uGMuG">flerovium</a>, and a significant decrease in stabilization of the closed shell of oganesson.<a class="footnote-ref" id="fnref:132" href="#fn:132">132</a> It has also been calculated that oganesson, unlike the other noble gases, binds an electron with release of energy, or in other words, it exhibits positive <a href="/facts/Electron_affinity/1mf4A396">electron affinity</a>,<a class="footnote-ref" id="fnref:133" href="#fn:133">133</a><a class="footnote-ref" id="fnref:134" href="#fn:134">134</a> due to the relativistically stabilized 8s energy level and the destabilized 7p3/2 level,<a class="footnote-ref" id="fnref:135" href="#fn:135">135</a> whereas copernicium and flerovium are predicted to have no electron affinity.<a class="footnote-ref" id="fnref:136" href="#fn:136">136</a><a class="footnote-ref" id="fnref:137" href="#fn:137">137</a> Nevertheless, <a href="/facts/Quantum_electrodynamic/zPteAr6G">quantum electrodynamic</a> corrections have been shown to be quite significant in reducing this affinity by decreasing the binding in the <a href="/facts/Anion/wrbwhF3z">anion</a> Og− by 9%, thus confirming the importance of these corrections in <a href="/facts/Superheavy_element/9PjYvCc3">superheavy elements</a>.<a class="footnote-ref" id="fnref:138" href="#fn:138">138</a> 2022 calculations expect the electron affinity of oganesson to be 0.080(6) eV.<a class="footnote-ref" id="fnref:139" href="#fn:139">139</a>
<a href="/facts/Monte_Carlo_method/AkHjY7jc">Monte Carlo simulations</a> of oganesson's <a href="/facts/Molecular_dynamics/yR3DNt6U">molecular dynamics</a> predict it has a melting point of 325±15 K and a boiling point of 450±10 K due to <a href="/facts/Relativistic_quantum_chemistry/8A1se1CS">relativistic effects</a> (if these effects are ignored, oganesson would melt at ≈220 K). Thus oganesson would probably be a solid rather than a gas under <a href="/facts/Standard_conditions/JhJv9KFJ">standard conditions</a>, though still with a rather low melting point.<a class="footnote-ref" id="fnref:140" href="#fn:140">140</a><a class="footnote-ref" id="fnref:141" href="#fn:141">141</a>
Oganesson is expected to have an extremely broad <a href="/facts/Polarizability/0XRkXwUu">polarizability</a>, almost double that of radon.<a class="footnote-ref" id="fnref:142" href="#fn:142">142</a> Because of its tremendous polarizability, oganesson is expected to have an anomalously low first <a href="/facts/Ionization_energy/lezUajfA">ionization energy</a> of about 860 kJ/mol, similar to that of <a href="/facts/Cadmium/wXkV2eIX">cadmium</a> and less than those of <a href="/facts/Iridium/cB4n6MbQ">iridium</a>, <a href="/facts/Platinum/qJC6lQf7">platinum</a>, and <a href="/facts/Gold/1znknojp">gold</a>. This is significantly smaller than the values predicted for <a href="/facts/Darmstadtium/etmwTLmP">darmstadtium</a>, <a href="/facts/Roentgenium/LEhvJaJQ">roentgenium</a>, and copernicium, although it is greater than that predicted for flerovium.<a class="footnote-ref" id="fnref:143" href="#fn:143">143</a> Its second ionization energy should be around 1560 kJ/mol.<a class="footnote-ref" id="fnref:144" href="#fn:144">144</a> Even the shell structure in the nucleus and electron cloud of oganesson is strongly impacted by relativistic effects: the valence and core electron subshells in oganesson are expected to be "smeared out" in a homogeneous <a href="/facts/Fermi_gas/D00lFTqW">Fermi gas</a> of electrons, unlike those of the "less relativistic" radon and xenon (although there is some incipient delocalisation in radon), due to the very strong spin–orbit splitting of the 7p orbital in oganesson.<a class="footnote-ref" id="fnref:145" href="#fn:145">145</a> A similar effect for nucleons, particularly neutrons, is incipient in the closed-neutron-shell nucleus 302Og and is strongly in force at the hypothetical superheavy closed-shell nucleus 472164, with 164 protons and 308 neutrons.<a class="footnote-ref" id="fnref:146" href="#fn:146">146</a> Studies have also predicted that due to increasing electrostatic forces, oganesson may have a semibubble structure in proton density, having few protons at the center of its nucleus.<a class="footnote-ref" id="fnref:147" href="#fn:147">147</a><a class="footnote-ref" id="fnref:148" href="#fn:148">148</a> Moreover, spin–orbit effects may cause bulk oganesson to be a <a href="/facts/Semiconductor/zFf3mGTE">semiconductor</a>, with a <a href="/facts/Band_gap/IjIeh95l">band gap</a> of 1.5±0.6 eV predicted. All the lighter noble gases are <a href="/facts/Insulator_(electricity)/SfSXkrh5">insulators</a> instead: for example, the band gap of bulk <a href="/facts/Radon/0V9arWKl">radon</a> is expected to be 7.1±0.5 eV.<a class="footnote-ref" id="fnref:149" href="#fn:149">149</a>

<h3>Predicted compounds</h3>

The only confirmed isotope of oganesson, 294Og, has much too short a half-life to be chemically investigated experimentally. Therefore, no compounds of oganesson have been synthesized yet.<a class="footnote-ref" id="fnref:150" href="#fn:150">150</a> Nevertheless, calculations on <a href="/facts/Theoretical_chemistry/uqcyS5KH">theoretical compounds</a> have been performed since 1964.<a class="footnote-ref" id="fnref:151" href="#fn:151">151</a> It is expected that if the <a href="/facts/Ionization_energy/lezUajfA">ionization energy</a> of the element is high enough, it will be difficult to <a href="/facts/Oxidize/Pyd5RVcj">oxidize</a> and therefore, the most common <a href="/facts/Oxidation_state/W53W6s6V">oxidation state</a> would be 0 (as for the noble gases);<a class="footnote-ref" id="fnref:152" href="#fn:152">152</a> nevertheless, this appears not to be the case.<a class="footnote-ref" id="fnref:153" href="#fn:153">153</a>
Calculations on the <a href="/facts/Diatomic_molecule/hkfKAC7m">diatomic molecule</a> Og2 showed a <a href="/facts/Chemical_bond/ArNUMnIB">bonding</a> interaction roughly equivalent to that calculated for Hg2, and a <a href="/facts/Dissociation_energy/wdDb5yHN">dissociation energy</a> of 6 kJ/mol, roughly 4 times of that of Rn2.<a class="footnote-ref" id="fnref:154" href="#fn:154">154</a> Most strikingly, it was calculated to have a <a href="/facts/Bond_length/rHHIBH6q">bond length</a> shorter than in Rn2 by 0.16 Å, which would be indicative of a significant bonding interaction.<a class="footnote-ref" id="fnref:155" href="#fn:155">155</a> On the other hand, the compound OgH+ exhibits a dissociation energy (in other words <a href="/facts/Proton_affinity/ypQdxqNR">proton affinity</a> of oganesson) that is smaller than that of RnH+.<a class="footnote-ref" id="fnref:156" href="#fn:156">156</a>
The bonding between oganesson and <a href="/facts/Hydrogen/BoYHjl0J">hydrogen</a> in OgH is predicted to be very weak and can be regarded as a pure <a href="/facts/Van_der_Waals_interaction/jyGU8Vh9">van der Waals interaction</a> rather than a true <a href="/facts/Chemical_bond/ArNUMnIB">chemical bond</a>.<a class="footnote-ref" id="fnref:157" href="#fn:157">157</a> On the other hand, with highly electronegative elements, oganesson seems to form more stable compounds than for example <a href="/facts/Copernicium/EhgyBkg0">copernicium</a> or <a href="/facts/Flerovium/Aa7uGMuG">flerovium</a>.<a class="footnote-ref" id="fnref:158" href="#fn:158">158</a> The stable oxidation states +2 and +4 have been predicted to exist in the <a href="/facts/Fluoride/LpqNMzwa">fluorides</a> OgF2 and OgF4.<a class="footnote-ref" id="fnref:159" href="#fn:159">159</a> The +6 state would be less stable due to the strong binding of the 7p1/2 subshell.<a class="footnote-ref" id="fnref:160" href="#fn:160">160</a> This is a result of the same spin–orbit interactions that make oganesson unusually reactive. For example, it was shown that the reaction of oganesson with F2 to form the compound OgF2 would release an energy of 106 kcal/mol of which about 46 kcal/mol come from these interactions.<a class="footnote-ref" id="fnref:161" href="#fn:161">161</a> For comparison, the spin–orbit interaction for the similar molecule RnF2 is about 10 kcal/mol out of a formation energy of 49 kcal/mol.<a class="footnote-ref" id="fnref:162" href="#fn:162">162</a> The same interaction stabilizes the <a href="/facts/Tetrahedral_molecular_geometry/583AL1sP">tetrahedral Td configuration</a> for OgF4, as distinct from the <a href="/facts/Square_planar/2mLqCvd0">square planar D4h one</a> of <a href="/facts/Xenon_tetrafluoride/blYIn0x7">XeF4</a>, which RnF4 is also expected to have;<a class="footnote-ref" id="fnref:163" href="#fn:163">163</a> this is because OgF4 is expected to have two <a href="/facts/Inert_pair/bqREzIAU">inert electron pairs</a> (7s and 7p1/2). As such, OgF6 is expected to be unbound, continuing an expected trend in the destabilisation of the +6 oxidation state (RnF6 is likewise expected to be much less stable than <a href="/facts/Xenon_hexafluoride/QU16jh1g">XeF6</a>).<a class="footnote-ref" id="fnref:164" href="#fn:164">164</a><a class="footnote-ref" id="fnref:165" href="#fn:165">165</a> The Og–F bond will most probably be <a href="/facts/Ionic_bond/R6nUJI5u">ionic</a> rather than <a href="/facts/Covalent_bond/EzMLf3Pz">covalent</a>, rendering the oganesson fluorides non-volatile.<a class="footnote-ref" id="fnref:166" href="#fn:166">166</a><a class="footnote-ref" id="fnref:167" href="#fn:167">167</a> OgF2 is predicted to be partially <a href="/facts/Ionic_bonding/R6nUJI5u">ionic</a> due to oganesson's high <a href="/facts/Electropositivity/H7Vq7Uah">electropositivity</a>.<a class="footnote-ref" id="fnref:168" href="#fn:168">168</a> Oganesson is predicted to be sufficiently electropositive<a class="footnote-ref" id="fnref:169" href="#fn:169">169</a> to form an Og–Cl bond with <a href="/facts/Chlorine/y27UwYBM">chlorine</a>.<a class="footnote-ref" id="fnref:170" href="#fn:170">170</a>
A compound of oganesson and <a href="/facts/Tennessine/eGCBDvEr">tennessine</a>, OgTs4, has been predicted to be potentially stable chemically.<a class="footnote-ref" id="fnref:171" href="#fn:171">171</a>

<h2 id="see-also">See also</h2>
<ul><li><a href="/facts/Island_of_stability/XuxQzqjL">Island of stability</a></li>
<li><a href="/facts/Superheavy_element/9PjYvCc3">Superheavy element</a></li>
<li><a href="/facts/Transuranium_element/a12PwdAw">Transuranium element</a></li>
<li><a href="/facts/Extended_periodic_table/Q3rg3qLA">Extended periodic table</a></li></ul>
<h2 id="notes">Notes</h2>

<h2 id="bibliography">Bibliography</h2>
<ul><li>Audi, G.; Kondev, F. G.; Wang, M.; et al. (2017). "The NUBASE2016 evaluation of nuclear properties". Chinese Physics C. 41 (3): 030001. <a href="/facts/Bibcode_(identifier)/9HtdQSGB">Bibcode</a>:<a href="https://ui.adsabs.harvard.edu/abs/2017ChPhC..41c0001A">2017ChPhC..41c0001A</a>. <a href="/facts/Doi_(identifier)/muM9Etpq">doi</a>:<a href="https://doi.org/10.1088%2F1674-1137%2F41%2F3%2F030001">10.1088/1674-1137/41/3/030001</a>.</li>
<li>Beiser, A. (2003). Concepts of modern physics (6th ed.). McGraw-Hill. <a href="/facts/ISBN_(identifier)/15AdSPa9">ISBN</a> 978-0-07-244848-1. <a href="/facts/OCLC_(identifier)/Yqad8waq">OCLC</a> <a href="https://search.worldcat.org/oclc/48965418">48965418</a>.</li>
<li><a href="/facts/Darleane_C._Hoffman/2gX65TCu">Hoffman, D. C.</a>; <a href="/facts/Albert_Ghiorso/jP5gHCwp">Ghiorso, A.</a>; Seaborg, G. T. (2000). The Transuranium People: The Inside Story. <a href="/facts/World_Scientific/qJPTP0Yk">World Scientific</a>. <a href="/facts/ISBN_(identifier)/15AdSPa9">ISBN</a> 978-1-78-326244-1.</li>
<li><a href="/facts/Helge_Kragh/j8RzFcow">Kragh, H.</a> (2018). From Transuranic to Superheavy Elements: A Story of Dispute and Creation. <a href="/facts/Springer_Science%252BBusiness_Media/nAesf6nT">Springer</a>. <a href="/facts/ISBN_(identifier)/15AdSPa9">ISBN</a> 978-3-319-75813-8.</li>
<li>Zagrebaev, V.; Karpov, A.; Greiner, W. (2013). "Future of superheavy element research: Which nuclei could be synthesized within the next few years?". <a href="/facts/Journal_of_Physics%3a_Conference_Series/b5bIJ4kE">Journal of Physics: Conference Series</a>. 420 (1): 012001. <a href="/facts/ArXiv_(identifier)/H6EtgnBe">arXiv</a>:<a href="https://arxiv.org/abs/1207.5700">1207.5700</a>. <a href="/facts/Bibcode_(identifier)/9HtdQSGB">Bibcode</a>:<a href="https://ui.adsabs.harvard.edu/abs/2013JPhCS.420a2001Z">2013JPhCS.420a2001Z</a>. <a href="/facts/Doi_(identifier)/muM9Etpq">doi</a>:<a href="https://doi.org/10.1088%2F1742-6596%2F420%2F1%2F012001">10.1088/1742-6596/420/1/012001</a>. <a href="/facts/ISSN_(identifier)/DPAflDvU">ISSN</a> <a href="https://search.worldcat.org/issn/1742-6588">1742-6588</a>. <a href="/facts/S2CID_(identifier)/ldJsHa2Y">S2CID</a> <a href="https://api.semanticscholar.org/CorpusID:55434734">55434734</a>.</li></ul>
<h2 id="further-reading">Further reading</h2>
<ul><li>Scerri, Eric (2007). <a href="https://archive.org/details/periodictableits0000scer">The Periodic Table, Its Story and Its Significance</a>. New York: Oxford University Press. <a href="/facts/ISBN_(identifier)/15AdSPa9">ISBN</a> 978-0-19-530573-9.</li></ul>
<h2 id="external-links">External links</h2>
<ul><li><a href="https://www.sciencenews.org/article/5-ways-heaviest-element-periodic-table-really-bizarre">5 ways the heaviest element on the periodic table is really bizarre</a>, <a href="/facts/Science_News/pEPc4HwI">ScienceNews.org</a></li>
<li><a href="https://web.archive.org/web/20061129112314/https://flerovlab.jinr.ru/flnr/elm118.html">Element 118: Experiments on discovery</a>, archive of discoverers' official web page</li>
<li><a href="https://www.nytimes.com/2006/10/17/science/17heavy.html">Element 118, Heaviest Ever, Reported for 1,000th of a Second</a>, <a href="/facts/The_New_York_Times/T9marWVX">The New York Times</a>.</li>
<li><a href="https://education.jlab.org/itselemental/ele118.html">It's Elemental: Oganesson</a></li>
<li><a href="https://www.periodicvideos.com/videos/118.htm">Oganesson</a> at <a href="/facts/The_Periodic_Table_of_Videos/vC5kbN0M">The Periodic Table of Videos</a> (University of Nottingham)</li>
<li><a href="https://iupac.org/publications/pac/75/10/1601/">On the Claims for Discovery of Elements 110, 111, 112, 114, 116, and 118 (IUPAC Technical Report)</a></li>
<li><a href="https://www.webelements.com/oganesson/">WebElements: Oganesson</a></li></ul>

<h2 id="references">References</h2>

<ol>
<li id="fn:1">"IUPAC Announces the Names of the Elements 113, 115, 117, and 118". IUPAC. 30 November 2016. Archived from the original on 30 November 2016. Retrieved 1 December 2015. <a href="https://iupac.org/iupac-announces-the-names-of-the-elements-113-115-117-and-118/" target="_blank">https://iupac.org/iupac-announces-the-names-of-the-elements-113-115-117-and-118/</a> <a href="#fnref:1" class="footnote-back-ref">↩</a></li>
<li id="fn:2">St. Fleur, Nicholas (1 December 2016). "Four New Names Officially Added to the Periodic Table of Elements". The New York Times. Retrieved 1 December 2016. <a href="https://www.nytimes.com/2016/12/01/science/periodic-table-new-elements.html" target="_blank">https://www.nytimes.com/2016/12/01/science/periodic-table-new-elements.html</a> <a href="#fnref:2" class="footnote-back-ref">↩</a></li>
<li id="fn:3">Smits, Odile R.; Mewes, Jan-Michael; Jerabek, Paul; Schwerdtfeger, Peter (2020). "Oganesson: A Noble Gas Element That Is Neither Noble Nor a Gas". Angewandte Chemie International Edition. 59 (52): 23636–23640. doi:10.1002/anie.202011976. PMC 7814676. PMID 32959952. <a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC7814676" target="_blank">https://www.ncbi.nlm.nih.gov/pmc/articles/PMC7814676</a> <a href="#fnref:3" class="footnote-back-ref">↩</a></li>
<li id="fn:4">Nash, Clinton S. (2005). "Atomic and Molecular Properties of Elements 112, 114, and 118". Journal of Physical Chemistry A. 109 (15): 3493–3500. Bibcode:2005JPCA..109.3493N. doi:10.1021/jp050736o. PMID 16833687. <a href="/wiki/Bibcode_(identifier)" target="_blank">/wiki/Bibcode_(identifier)</a> <a href="#fnref:4" class="footnote-back-ref">↩</a></li>
<li id="fn:5">Smits, Odile R.; Mewes, Jan-Michael; Jerabek, Paul; Schwerdtfeger, Peter (2020). "Oganesson: A Noble Gas Element That Is Neither Noble Nor a Gas". Angewandte Chemie International Edition. 59 (52): 23636–23640. doi:10.1002/anie.202011976. PMC 7814676. PMID 32959952. <a href="https://www.ncbi.nlm.nih.gov/pmc/articles/PMC7814676" target="_blank">https://www.ncbi.nlm.nih.gov/pmc/articles/PMC7814676</a> <a href="#fnref:5" class="footnote-back-ref">↩</a></li>
<li id="fn:6">In nuclear physics, an element is called heavy if its atomic number is high; lead (element 82) is one example of such a heavy element. The term "superheavy elements" typically refers to elements with atomic number greater than 103 (although there are other definitions, such as atomic number greater than 100[18] or 112;[19] sometimes, the term is presented an equivalent to the term "transactinide", which puts an upper limit before the beginning of the hypothetical superactinide series).[20] Terms "heavy isotopes" (of a given element) and "heavy nuclei" mean what could be understood in the common language—isotopes of high mass (for the given element) and nuclei of high mass, respectively. <a href="/wiki/Nuclear_physics" target="_blank">/wiki/Nuclear_physics</a> <a href="#fnref:6" class="footnote-back-ref">↩</a></li>
<li id="fn:7">In 2009, a team at the JINR led by Oganessian published results of their attempt to create hassium in a symmetric 136Xe + 136Xe reaction. They failed to observe a single atom in such a reaction, putting the upper limit on the cross section, the measure of probability of a nuclear reaction, as 2.5 pb.[21] In comparison, the reaction that resulted in hassium discovery, 208Pb + 58Fe, had a cross section of ~20 pb (more specifically, 19+19-11 pb), as estimated by the discoverers.[22] <a href="/wiki/Picobarn" target="_blank">/wiki/Picobarn</a> <a href="#fnref:7" class="footnote-back-ref">↩</a></li>
<li id="fn:8">Subramanian, S. (28 August 2019). "Making New Elements Doesn't Pay. Just Ask This Berkeley Scientist". Bloomberg Businessweek. Retrieved 18 January 2020. <a href="/wiki/Samanth_Subramanian" target="_blank">/wiki/Samanth_Subramanian</a> <a href="#fnref:8" class="footnote-back-ref">↩</a></li>
<li id="fn:9">Hinde, D. (2017). "Something new and superheavy at the periodic table". The Conversation. Retrieved 30 January 2020. <a href="https://theconversation.com/something-new-and-superheavy-at-the-periodic-table-26286" target="_blank">https://theconversation.com/something-new-and-superheavy-at-the-periodic-table-26286</a> <a href="#fnref:9" class="footnote-back-ref">↩</a></li>
<li id="fn:10">The amount of energy applied to the beam particle to accelerate it can also influence the value of cross section. For example, in the 2814Si + 10n → 2813Al + 11p reaction, cross section changes smoothly from 370 mb at 12.3 MeV to 160 mb at 18.3 MeV, with a broad peak at 13.5 MeV with the maximum value of 380 mb.[26] <a href="#fnref:10" class="footnote-back-ref">↩</a></li>
<li id="fn:11">"Nuclear Reactions" (PDF). pp. 7–8. Retrieved 27 January 2020. Published as Loveland, W. D.; Morrissey, D. J.; Seaborg, G. T. (2005). "Nuclear Reactions". Modern Nuclear Chemistry. John Wiley & Sons, Inc. pp. 249–297. doi:10.1002/0471768626.ch10. ISBN 978-0-471-76862-3. <a href="978-0-471-76862-3" target="_blank">978-0-471-76862-3</a> <a href="#fnref:11" class="footnote-back-ref">↩</a></li>
<li id="fn:12">Krása, A. (2010). "Neutron Sources for ADS" (PDF). Faculty of Nuclear Sciences and Physical Engineering. Czech Technical University in Prague: 4–8. S2CID 28796927 – via Wayback Machine. <a href="https://web.archive.org/web/20170918062244/http://ojs.ujf.cas.cz/~krasa/ZNTT/SpallationReactions-text.pdf" target="_blank">https://web.archive.org/web/20170918062244/http://ojs.ujf.cas.cz/~krasa/ZNTT/SpallationReactions-text.pdf</a> <a href="#fnref:12" class="footnote-back-ref">↩</a></li>
<li id="fn:13">Krása, A. (2010). "Neutron Sources for ADS" (PDF). Faculty of Nuclear Sciences and Physical Engineering. Czech Technical University in Prague: 4–8. S2CID 28796927 – via Wayback Machine. <a href="https://web.archive.org/web/20170918062244/http://ojs.ujf.cas.cz/~krasa/ZNTT/SpallationReactions-text.pdf" target="_blank">https://web.archive.org/web/20170918062244/http://ojs.ujf.cas.cz/~krasa/ZNTT/SpallationReactions-text.pdf</a> <a href="#fnref:13" class="footnote-back-ref">↩</a></li>
<li id="fn:14">Wapstra, A. H. (1991). "Criteria that must be satisfied for the discovery of a new chemical element to be recognized" (PDF). Pure and Applied Chemistry. 63 (6): 883. doi:10.1351/pac199163060879. ISSN 1365-3075. S2CID 95737691. <a href="/wiki/Aaldert_Wapstra" target="_blank">/wiki/Aaldert_Wapstra</a> <a href="#fnref:14" class="footnote-back-ref">↩</a></li>
<li id="fn:15">This figure also marks the generally accepted upper limit for lifetime of a compound nucleus.[31] <a href="#fnref:15" class="footnote-back-ref">↩</a></li>
<li id="fn:16">Chemistry World (2016). "How to Make Superheavy Elements and Finish the Periodic Table [Video]". Scientific American. Retrieved 27 January 2020. <a href="/wiki/Chemistry_World" target="_blank">/wiki/Chemistry_World</a> <a href="#fnref:16" class="footnote-back-ref">↩</a></li>
<li id="fn:17">This separation is based on that the resulting nuclei move past the target more slowly then the unreacted beam nuclei. The separator contains electric and magnetic fields whose effects on a moving particle cancel out for a specific velocity of a particle.[33] Such separation can also be aided by a time-of-flight measurement and a recoil energy measurement; a combination of the two may allow to estimate the mass of a nucleus.[34] <a href="#fnref:17" class="footnote-back-ref">↩</a></li>
<li id="fn:18">Chemistry World (2016). "How to Make Superheavy Elements and Finish the Periodic Table [Video]". Scientific American. Retrieved 27 January 2020. <a href="/wiki/Chemistry_World" target="_blank">/wiki/Chemistry_World</a> <a href="#fnref:18" class="footnote-back-ref">↩</a></li>
<li id="fn:19">Zagrebaev, Karpov & Greiner 2013, p. 3. - Zagrebaev, V.; Karpov, A.; Greiner, W. (2013). "Future of superheavy element research: Which nuclei could be synthesized within the next few years?". Journal of Physics: Conference Series. 420 (1): 012001. arXiv:1207.5700. Bibcode:2013JPhCS.420a2001Z. doi:10.1088/1742-6596/420/1/012001. ISSN 1742-6588. S2CID 55434734. <a href="https://arxiv.org/abs/1207.5700" target="_blank">https://arxiv.org/abs/1207.5700</a> <a href="#fnref:19" class="footnote-back-ref">↩</a></li>
<li id="fn:20">Chemistry World (2016). "How to Make Superheavy Elements and Finish the Periodic Table [Video]". Scientific American. Retrieved 27 January 2020. <a href="/wiki/Chemistry_World" target="_blank">/wiki/Chemistry_World</a> <a href="#fnref:20" class="footnote-back-ref">↩</a></li>
<li id="fn:21">Beiser 2003, p. 432. - Beiser, A. (2003). Concepts of modern physics (6th ed.). McGraw-Hill. ISBN 978-0-07-244848-1. OCLC 48965418. <a href="https://search.worldcat.org/oclc/48965418" target="_blank">https://search.worldcat.org/oclc/48965418</a> <a href="#fnref:21" class="footnote-back-ref">↩</a></li>
<li id="fn:22">Pauli, N. (2019). "Alpha decay" (PDF). Introductory Nuclear, Atomic and Molecular Physics (Nuclear Physics Part). Université libre de Bruxelles. Retrieved 16 February 2020. <a href="http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_5.pdf" target="_blank">http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_5.pdf</a> <a href="#fnref:22" class="footnote-back-ref">↩</a></li>
<li id="fn:23">Pauli, N. (2019). "Nuclear fission" (PDF). Introductory Nuclear, Atomic and Molecular Physics (Nuclear Physics Part). Université libre de Bruxelles. Retrieved 16 February 2020. <a href="http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_8.pdf" target="_blank">http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_8.pdf</a> <a href="#fnref:23" class="footnote-back-ref">↩</a></li>
<li id="fn:24">Staszczak, A.; Baran, A.; Nazarewicz, W. (2013). "Spontaneous fission modes and lifetimes of superheavy elements in the nuclear density functional theory". Physical Review C. 87 (2): 024320–1. arXiv:1208.1215. Bibcode:2013PhRvC..87b4320S. doi:10.1103/physrevc.87.024320. ISSN 0556-2813. <a href="https://doi.org/10.1103%2Fphysrevc.87.024320" target="_blank">https://doi.org/10.1103%2Fphysrevc.87.024320</a> <a href="#fnref:24" class="footnote-back-ref">↩</a></li>
<li id="fn:25">Audi et al. 2017, pp. 030001-129–030001-138. - Audi, G.; Kondev, F. G.; Wang, M.; et al. (2017). "The NUBASE2016 evaluation of nuclear properties". Chinese Physics C. 41 (3): 030001. Bibcode:2017ChPhC..41c0001A. doi:10.1088/1674-1137/41/3/030001. <a href="https://ui.adsabs.harvard.edu/abs/2017ChPhC..41c0001A" target="_blank">https://ui.adsabs.harvard.edu/abs/2017ChPhC..41c0001A</a> <a href="#fnref:25" class="footnote-back-ref">↩</a></li>
<li id="fn:26">Not all decay modes are caused by electrostatic repulsion. For example, beta decay is caused by the weak interaction.[41] <a href="/wiki/Beta_decay" target="_blank">/wiki/Beta_decay</a> <a href="#fnref:26" class="footnote-back-ref">↩</a></li>
<li id="fn:27">Beiser 2003, p. 433. - Beiser, A. (2003). Concepts of modern physics (6th ed.). McGraw-Hill. ISBN 978-0-07-244848-1. OCLC 48965418. <a href="https://search.worldcat.org/oclc/48965418" target="_blank">https://search.worldcat.org/oclc/48965418</a> <a href="#fnref:27" class="footnote-back-ref">↩</a></li>
<li id="fn:28">Audi et al. 2017, p. 030001-125. - Audi, G.; Kondev, F. G.; Wang, M.; et al. (2017). "The NUBASE2016 evaluation of nuclear properties". Chinese Physics C. 41 (3): 030001. Bibcode:2017ChPhC..41c0001A. doi:10.1088/1674-1137/41/3/030001. <a href="https://ui.adsabs.harvard.edu/abs/2017ChPhC..41c0001A" target="_blank">https://ui.adsabs.harvard.edu/abs/2017ChPhC..41c0001A</a> <a href="#fnref:28" class="footnote-back-ref">↩</a></li>
<li id="fn:29">Pauli, N. (2019). "Alpha decay" (PDF). Introductory Nuclear, Atomic and Molecular Physics (Nuclear Physics Part). Université libre de Bruxelles. Retrieved 16 February 2020. <a href="http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_5.pdf" target="_blank">http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_5.pdf</a> <a href="#fnref:29" class="footnote-back-ref">↩</a></li>
<li id="fn:30">Pauli, N. (2019). "Nuclear fission" (PDF). Introductory Nuclear, Atomic and Molecular Physics (Nuclear Physics Part). Université libre de Bruxelles. Retrieved 16 February 2020. <a href="http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_8.pdf" target="_blank">http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_8.pdf</a> <a href="#fnref:30" class="footnote-back-ref">↩</a></li>
<li id="fn:31">Beiser 2003, p. 432–433. - Beiser, A. (2003). Concepts of modern physics (6th ed.). McGraw-Hill. ISBN 978-0-07-244848-1. OCLC 48965418. <a href="https://search.worldcat.org/oclc/48965418" target="_blank">https://search.worldcat.org/oclc/48965418</a> <a href="#fnref:31" class="footnote-back-ref">↩</a></li>
<li id="fn:32">Pauli, N. (2019). "Nuclear fission" (PDF). Introductory Nuclear, Atomic and Molecular Physics (Nuclear Physics Part). Université libre de Bruxelles. Retrieved 16 February 2020. <a href="http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_8.pdf" target="_blank">http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_8.pdf</a> <a href="#fnref:32" class="footnote-back-ref">↩</a></li>
<li id="fn:33">Oganessian, Yu. (2012). "Nuclei in the "Island of Stability" of Superheavy Elements". Journal of Physics: Conference Series. 337 (1): 012005-1 – 012005-6. Bibcode:2012JPhCS.337a2005O. doi:10.1088/1742-6596/337/1/012005. ISSN 1742-6596. <a href="https://doi.org/10.1088%2F1742-6596%2F337%2F1%2F012005" target="_blank">https://doi.org/10.1088%2F1742-6596%2F337%2F1%2F012005</a> <a href="#fnref:33" class="footnote-back-ref">↩</a></li>
<li id="fn:34">Moller, P.; Nix, J. R. (1994). Fission properties of the heaviest elements (PDF). Dai 2 Kai Hadoron Tataikei no Simulation Symposium, Tokai-mura, Ibaraki, Japan. University of North Texas. Retrieved 16 February 2020. <a href="https://digital.library.unt.edu/ark:/67531/metadc674703/m2/1/high_res_d/32502.pdf" target="_blank">https://digital.library.unt.edu/ark:/67531/metadc674703/m2/1/high_res_d/32502.pdf</a> <a href="#fnref:34" class="footnote-back-ref">↩</a></li>
<li id="fn:35">Pauli, N. (2019). "Nuclear fission" (PDF). Introductory Nuclear, Atomic and Molecular Physics (Nuclear Physics Part). Université libre de Bruxelles. Retrieved 16 February 2020. <a href="http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_8.pdf" target="_blank">http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_8.pdf</a> <a href="#fnref:35" class="footnote-back-ref">↩</a></li>
<li id="fn:36">Oganessian, Yu. Ts. (2004). "Superheavy elements". Physics World. 17 (7): 25–29. doi:10.1088/2058-7058/17/7/31. Retrieved 16 February 2020. <a href="https://physicsworld.com/a/superheavy-elements/" target="_blank">https://physicsworld.com/a/superheavy-elements/</a> <a href="#fnref:36" class="footnote-back-ref">↩</a></li>
<li id="fn:37">Pauli, N. (2019). "Nuclear fission" (PDF). Introductory Nuclear, Atomic and Molecular Physics (Nuclear Physics Part). Université libre de Bruxelles. Retrieved 16 February 2020. <a href="http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_8.pdf" target="_blank">http://metronu.ulb.ac.be/npauly/Pauly/physnu/chapter_8.pdf</a> <a href="#fnref:37" class="footnote-back-ref">↩</a></li>
<li id="fn:38">Oganessian, Yu. Ts. (2004). "Superheavy elements". Physics World. 17 (7): 25–29. doi:10.1088/2058-7058/17/7/31. Retrieved 16 February 2020. <a href="https://physicsworld.com/a/superheavy-elements/" target="_blank">https://physicsworld.com/a/superheavy-elements/</a> <a href="#fnref:38" class="footnote-back-ref">↩</a></li>
<li id="fn:39">Schädel, M. (2015). "Chemistry of the superheavy elements". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences. 373 (2037): 20140191. Bibcode:2015RSPTA.37340191S. doi:10.1098/rsta.2014.0191. ISSN 1364-503X. PMID 25666065. <a href="https://doi.org/10.1098%2Frsta.2014.0191" target="_blank">https://doi.org/10.1098%2Frsta.2014.0191</a> <a href="#fnref:39" class="footnote-back-ref">↩</a></li>
<li id="fn:40">Hulet, E. K. (1989). Biomodal spontaneous fission. 50th Anniversary of Nuclear Fission, Leningrad, USSR. Bibcode:1989nufi.rept...16H. <a href="/wiki/Bibcode_(identifier)" target="_blank">/wiki/Bibcode_(identifier)</a> <a href="#fnref:40" class="footnote-back-ref">↩</a></li>
<li id="fn:41">Oganessian, Yu. (2012). "Nuclei in the "Island of Stability" of Superheavy Elements". Journal of Physics: Conference Series. 337 (1): 012005-1 – 012005-6. Bibcode:2012JPhCS.337a2005O. doi:10.1088/1742-6596/337/1/012005. ISSN 1742-6596. <a href="https://doi.org/10.1088%2F1742-6596%2F337%2F1%2F012005" target="_blank">https://doi.org/10.1088%2F1742-6596%2F337%2F1%2F012005</a> <a href="#fnref:41" class="footnote-back-ref">↩</a></li>
<li id="fn:42">It was already known by the 1960s that ground states of nuclei differed in energy and shape as well as that certain magic numbers of nucleons corresponded to greater stability of a nucleus. However, it was assumed that there was no nuclear structure in superheavy nuclei as they were too deformed to form one.[46] <a href="#fnref:42" class="footnote-back-ref">↩</a></li>
<li id="fn:43">Since mass of a nucleus is not measured directly but is rather calculated from that of another nucleus, such measurement is called indirect. Direct measurements are also possible, but for the most part they have remained unavailable for superheavy nuclei.[51] The first direct measurement of mass of a superheavy nucleus was reported in 2018 at LBNL.[52] Mass was determined from the location of a nucleus after the transfer (the location helps determine its trajectory, which is linked to the mass-to-charge ratio of the nucleus, since the transfer was done in presence of a magnet).[53] <a href="#fnref:43" class="footnote-back-ref">↩</a></li>
<li id="fn:44">Chemistry World (2016). "How to Make Superheavy Elements and Finish the Periodic Table [Video]". Scientific American. Retrieved 27 January 2020. <a href="/wiki/Chemistry_World" target="_blank">/wiki/Chemistry_World</a> <a href="#fnref:44" class="footnote-back-ref">↩</a></li>
<li id="fn:45">If the decay occurred in a vacuum, then since total momentum of an isolated system before and after the decay must be preserved, the daughter nucleus would also receive a small velocity. The ratio of the two velocities, and accordingly the ratio of the kinetic energies, would thus be inverse to the ratio of the two masses. The decay energy equals the sum of the known kinetic energy of the alpha particle and that of the daughter nucleus (an exact fraction of the former).[42] The calculations hold for an experiment as well, but the difference is that the nucleus does not move after the decay because it is tied to the detector. <a href="/wiki/Momentum#Conservation" target="_blank">/wiki/Momentum#Conservation</a> <a href="#fnref:45" class="footnote-back-ref">↩</a></li>
<li id="fn:46">Spontaneous fission was discovered by Soviet physicist Georgy Flerov,[54] a leading scientist at JINR, and thus it was a "hobbyhorse" for the facility.[55] In contrast, the LBL scientists believed fission information was not sufficient for a claim of synthesis of an element. They believed spontaneous fission had not been studied enough to use it for identification of a new element, since there was a difficulty of establishing that a compound nucleus had only ejected neutrons and not charged particles like protons or alpha particles.[31] They thus preferred to link new isotopes to the already known ones by successive alpha decays.[54] <a href="/wiki/Georgy_Flerov" target="_blank">/wiki/Georgy_Flerov</a> <a href="#fnref:46" class="footnote-back-ref">↩</a></li>
<li id="fn:47">For instance, element 102 was mistakenly identified in 1957 at the Nobel Institute of Physics in Stockholm, Stockholm County, Sweden.[56] There were no earlier definitive claims of creation of this element, and the element was assigned a name by its Swedish, American, and British discoverers, nobelium. It was later shown that the identification was incorrect.[57] The following year, RL was unable to reproduce the Swedish results and announced instead their synthesis of the element; that claim was also disproved later.[57] JINR insisted that they were the first to create the element and suggested a name of their own for the new element, joliotium;[58] the Soviet name was also not accepted (JINR later referred to the naming of the element 102 as "hasty").[59] This name was proposed to IUPAC in a written response to their ruling on priority of discovery claims of elements, signed 29 September 1992.[59] The name "nobelium" remained unchanged on account of its widespread usage.[60] <a href="/wiki/Stockholm" target="_blank">/wiki/Stockholm</a> <a href="#fnref:47" class="footnote-back-ref">↩</a></li>
<li id="fn:48">Kragh 2018, p. 6. - Kragh, H. (2018). From Transuranic to Superheavy Elements: A Story of Dispute and Creation. Springer. ISBN 978-3-319-75813-8. <a href="#fnref:48" class="footnote-back-ref">↩</a></li>
<li id="fn:49">Leach, Mark R. "The INTERNET Database of Periodic Tables". Retrieved 8 July 2016. <a href="https://www.meta-synthesis.com/webbook/35_pt/pt_database.php?PT_id=285" target="_blank">https://www.meta-synthesis.com/webbook/35_pt/pt_database.php?PT_id=285</a> <a href="#fnref:49" class="footnote-back-ref">↩</a></li>
<li id="fn:50">Grosse, A. V. (1965). "Some physical and chemical properties of element 118 (Eka-Em) and element 86 (Em)". Journal of Inorganic and Nuclear Chemistry. 27 (3). Elsevier Science Ltd.: 509–19. doi:10.1016/0022-1902(65)80255-X. <a href="/wiki/Doi_(identifier)" target="_blank">/wiki/Doi_(identifier)</a> <a href="#fnref:50" class="footnote-back-ref">↩</a></li>
<li id="fn:51">Fricke, Burkhard (1975). "Superheavy elements: a prediction of their chemical and physical properties". Recent Impact of Physics on Inorganic Chemistry. Structure and Bonding. 21: 89–144. doi:10.1007/BFb0116498. ISBN 978-3-540-07109-9. Retrieved 4 October 2013.
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<li id="fn:52">Pitzer, Kenneth (1975). "Are elements 112, 114, and 118 relatively inert gases?". The Journal of Chemical Physics. 2 (63): 1032–1033. doi:10.1063/1.431398. <a href="/wiki/Kenneth_Pitzer" target="_blank">/wiki/Kenneth_Pitzer</a> <a href="#fnref:52" class="footnote-back-ref">↩</a></li>
<li id="fn:53">Smolanczuk, R. (1999). "Production mechanism of superheavy nuclei in cold fusion reactions". Physical Review C. 59 (5): 2634–2639. Bibcode:1999PhRvC..59.2634S. doi:10.1103/PhysRevC.59.2634. <a href="/wiki/Bibcode_(identifier)" target="_blank">/wiki/Bibcode_(identifier)</a> <a href="#fnref:53" class="footnote-back-ref">↩</a></li>
<li id="fn:54">Smolanczuk, R. (1999). "Production mechanism of superheavy nuclei in cold fusion reactions". Physical Review C. 59 (5): 2634–2639. Bibcode:1999PhRvC..59.2634S. doi:10.1103/PhysRevC.59.2634. <a href="/wiki/Bibcode_(identifier)" target="_blank">/wiki/Bibcode_(identifier)</a> <a href="#fnref:54" class="footnote-back-ref">↩</a></li>
<li id="fn:55">Ninov, Viktor (1999). "Observation of Superheavy Nuclei Produced in the Reaction of 86Kr with 208Pb". Physical Review Letters. 83 (6): 1104–1107. Bibcode:1999PhRvL..83.1104N. doi:10.1103/PhysRevLett.83.1104. (Retracted, see doi:10.1103/PhysRevLett.89.039901) <a href="https://zenodo.org/record/1233919" target="_blank">https://zenodo.org/record/1233919</a> <a href="#fnref:55" class="footnote-back-ref">↩</a></li>
<li id="fn:56">Service, R. F. (1999). "Berkeley Crew Bags Element 118". Science. 284 (5421): 1751. doi:10.1126/science.284.5421.1751. S2CID 220094113. <a href="/wiki/Doi_(identifier)" target="_blank">/wiki/Doi_(identifier)</a> <a href="#fnref:56" class="footnote-back-ref">↩</a></li>
<li id="fn:57">Public Affairs Department, Lawrence Berkeley Laboratory (21 July 2001). "Results of element 118 experiment retracted". Archived from the original on 29 January 2008. Retrieved 18 January 2008. <a href="https://web.archive.org/web/20080129191344/https://enews.lbl.gov/Science-Articles/Archive/118-retraction.html" target="_blank">https://web.archive.org/web/20080129191344/https://enews.lbl.gov/Science-Articles/Archive/118-retraction.html</a> <a href="#fnref:57" class="footnote-back-ref">↩</a></li>
<li id="fn:58">Dalton, R. (2002). "Misconduct: The stars who fell to Earth". Nature. 420 (6917): 728–729. Bibcode:2002Natur.420..728D. doi:10.1038/420728a. PMID 12490902. S2CID 4398009. <a href="/wiki/Nature_(journal)" target="_blank">/wiki/Nature_(journal)</a> <a href="#fnref:58" class="footnote-back-ref">↩</a></li>
<li id="fn:59">"Element 118 disappears two years after it was discovered". Physics World. 2 August 2001. Retrieved 2 April 2012. <a href="https://physicsworld.com/a/element-118-disappears-two-years-after-it-was-discovered/" target="_blank">https://physicsworld.com/a/element-118-disappears-two-years-after-it-was-discovered/</a> <a href="#fnref:59" class="footnote-back-ref">↩</a></li>
<li id="fn:60">Zagrebaev, Karpov & Greiner 2013. - Zagrebaev, V.; Karpov, A.; Greiner, W. (2013). "Future of superheavy element research: Which nuclei could be synthesized within the next few years?". Journal of Physics: Conference Series. 420 (1): 012001. arXiv:1207.5700. Bibcode:2013JPhCS.420a2001Z. doi:10.1088/1742-6596/420/1/012001. ISSN 1742-6588. S2CID 55434734. <a href="https://arxiv.org/abs/1207.5700" target="_blank">https://arxiv.org/abs/1207.5700</a> <a href="#fnref:60" class="footnote-back-ref">↩</a></li>
<li id="fn:61">Oganessian, Yu. T.; et al. (2002). "Results from the first 249Cf+48Ca experiment" (PDF). JINR Communication. Archived from the original (PDF) on 13 December 2004. Retrieved 13 June 2009. <a href="https://web.archive.org/web/20041213100709/https://www.jinr.ru/publish/Preprints/2002/287%28D7-2002-287%29e.pdf" target="_blank">https://web.archive.org/web/20041213100709/https://www.jinr.ru/publish/Preprints/2002/287%28D7-2002-287%29e.pdf</a> <a href="#fnref:61" class="footnote-back-ref">↩</a></li>
<li id="fn:62">Moody, Ken (30 November 2013). "Synthesis of Superheavy Elements". In Schädel, Matthias; Shaughnessy, Dawn (eds.). The Chemistry of Superheavy Elements (2nd ed.). Springer Science & Business Media. pp. 24–8. ISBN 9783642374661. <a href="9783642374661" target="_blank">9783642374661</a> <a href="#fnref:62" class="footnote-back-ref">↩</a></li>
<li id="fn:63">Oganessian, Yu. Ts.; Utyonkov, V. K.; Lobanov, Yu. V.; Abdullin, F. Sh.; Polyakov, A. N.; Sagaidak, R. N.; Shirokovsky, I. V.; Tsyganov, Yu. S.; et al. (9 October 2006). "Synthesis of the isotopes of elements 118 and 116 in the 249Cf and 245Cm+48Ca fusion reactions". Physical Review C. 74 (4): 044602. Bibcode:2006PhRvC..74d4602O. doi:10.1103/PhysRevC.74.044602. Retrieved 18 January 2008. <a href="http://link.aps.org/abstract/PRC/v74/e044602" target="_blank">http://link.aps.org/abstract/PRC/v74/e044602</a> <a href="#fnref:63" class="footnote-back-ref">↩</a></li>
<li id="fn:64">Oganessian, Yu. Ts.; Utyonkov, V. K.; Lobanov, Yu. V.; Abdullin, F. Sh.; Polyakov, A. N.; Sagaidak, R. N.; Shirokovsky, I. V.; Tsyganov, Yu. S.; et al. (9 October 2006). "Synthesis of the isotopes of elements 118 and 116 in the 249Cf and 245Cm+48Ca fusion reactions". Physical Review C. 74 (4): 044602. Bibcode:2006PhRvC..74d4602O. doi:10.1103/PhysRevC.74.044602. Retrieved 18 January 2008. <a href="http://link.aps.org/abstract/PRC/v74/e044602" target="_blank">http://link.aps.org/abstract/PRC/v74/e044602</a> <a href="#fnref:64" class="footnote-back-ref">↩</a></li>
<li id="fn:65">Oganessian, Yu. T.; et al. (2002). "Element 118: results from the first 249Cf + 48Ca experiment". Communication of the Joint Institute for Nuclear Research. Archived from the original on 22 July 2011. <a href="https://web.archive.org/web/20110722060249/https://159.93.28.88/linkc/118/anno.html" target="_blank">https://web.archive.org/web/20110722060249/https://159.93.28.88/linkc/118/anno.html</a> <a href="#fnref:65" class="footnote-back-ref">↩</a></li>
<li id="fn:66">"Livermore scientists team with Russia to discover element 118". Livermore press release. 3 December 2006. Archived from the original on 17 October 2011. Retrieved 18 January 2008. <a href="https://web.archive.org/web/20111017105348/https://www.llnl.gov/news/newsreleases/2006/NR-06-10-03.html" target="_blank">https://web.archive.org/web/20111017105348/https://www.llnl.gov/news/newsreleases/2006/NR-06-10-03.html</a> <a href="#fnref:66" class="footnote-back-ref">↩</a></li>
<li id="fn:67">Oganessian, Yu. T. (2006). "Synthesis and decay properties of superheavy elements". Pure Appl. Chem. 78 (5): 889–904. doi:10.1351/pac200678050889. S2CID 55782333. <a href="https://doi.org/10.1351%2Fpac200678050889" target="_blank">https://doi.org/10.1351%2Fpac200678050889</a> <a href="#fnref:67" class="footnote-back-ref">↩</a></li>
<li id="fn:68">Sanderson, K. (2006). "Heaviest element made – again". Nature News. doi:10.1038/news061016-4. S2CID 121148847. <a href="/wiki/Doi_(identifier)" target="_blank">/wiki/Doi_(identifier)</a> <a href="#fnref:68" class="footnote-back-ref">↩</a></li>
<li id="fn:69">Schewe, P. & Stein, B. (17 October 2006). "Elements 116 and 118 Are Discovered". Physics News Update. American Institute of Physics. Archived from the original on 1 January 2012. Retrieved 18 January 2008. <a href="https://web.archive.org/web/20120101144201/https://www.aip.org/pnu/2006/797.html" target="_blank">https://web.archive.org/web/20120101144201/https://www.aip.org/pnu/2006/797.html</a> <a href="#fnref:69" class="footnote-back-ref">↩</a></li>
<li id="fn:70">Weiss, R. (17 October 2006). "Scientists Announce Creation of Atomic Element, the Heaviest Yet". The Washington Post. Retrieved 18 January 2008. <a href="https://www.washingtonpost.com/wp-dyn/content/article/2006/10/16/AR2006101601083.html" target="_blank">https://www.washingtonpost.com/wp-dyn/content/article/2006/10/16/AR2006101601083.html</a> <a href="#fnref:70" class="footnote-back-ref">↩</a></li>
<li id="fn:71">Barber, Robert C.; Karol, Paul J.; Nakahara, Hiromichi; Vardaci, Emanuele; Vogt, Erich W. (2011). "Discovery of the elements with atomic numbers greater than or equal to 113 (IUPAC Technical Report)". Pure and Applied Chemistry. 83 (7): 1. doi:10.1351/PAC-REP-10-05-01. <a href="https://doi.org/10.1351%2FPAC-REP-10-05-01" target="_blank">https://doi.org/10.1351%2FPAC-REP-10-05-01</a> <a href="#fnref:71" class="footnote-back-ref">↩</a></li>
<li id="fn:72">"Oganesson". WebElements Periodic Table. Retrieved 19 August 2019. <a href="https://www.webelements.com/oganesson/" target="_blank">https://www.webelements.com/oganesson/</a> <a href="#fnref:72" class="footnote-back-ref">↩</a></li>
<li id="fn:73">Jacoby, Mitch (17 October 2006). "Element 118 Detected, With Confidence". Chemical & Engineering News. 84 (43): 11. doi:10.1021/cen-v084n043.p011. Retrieved 18 January 2008. I would say we're very confident. <a href="https://pubs.acs.org/cen/news/84/i43/8443element118.html" target="_blank">https://pubs.acs.org/cen/news/84/i43/8443element118.html</a> <a href="#fnref:73" class="footnote-back-ref">↩</a></li>
<li id="fn:74">Oganessian, Yu. Ts.; Utyonkov, V. K.; Lobanov, Yu. V.; Abdullin, F. Sh.; Polyakov, A. N.; Sagaidak, R. N.; Shirokovsky, I. V.; Tsyganov, Yu. S.; et al. (9 October 2006). "Synthesis of the isotopes of elements 118 and 116 in the 249Cf and 245Cm+48Ca fusion reactions". Physical Review C. 74 (4): 044602. Bibcode:2006PhRvC..74d4602O. doi:10.1103/PhysRevC.74.044602. Retrieved 18 January 2008. <a href="http://link.aps.org/abstract/PRC/v74/e044602" target="_blank">http://link.aps.org/abstract/PRC/v74/e044602</a> <a href="#fnref:74" class="footnote-back-ref">↩</a></li>
<li id="fn:75">Oganessian, Yu. Ts.; Utyonkov, V. K.; Lobanov, Yu. V.; Abdullin, F. Sh.; Polyakov, A. N.; Sagaidak, R. N.; Shirokovsky, I. V.; Tsyganov, Yu. S.; et al. (9 October 2006). "Synthesis of the isotopes of elements 118 and 116 in the 249Cf and 245Cm+48Ca fusion reactions". Physical Review C. 74 (4): 044602. Bibcode:2006PhRvC..74d4602O. doi:10.1103/PhysRevC.74.044602. Retrieved 18 January 2008. <a href="http://link.aps.org/abstract/PRC/v74/e044602" target="_blank">http://link.aps.org/abstract/PRC/v74/e044602</a> <a href="#fnref:75" class="footnote-back-ref">↩</a></li>
<li id="fn:76">Oganessian, Yu. Ts.; Utyonkov, V. K.; Lobanov, Yu. V.; Abdullin, F. Sh.; Polyakov, A. N.; Sagaidak, R. N.; Shirokovsky, I. V.; Tsyganov, Yu. S.; et al. (9 October 2006). "Synthesis of the isotopes of elements 118 and 116 in the 249Cf and 245Cm+48Ca fusion reactions". Physical Review C. 74 (4): 044602. Bibcode:2006PhRvC..74d4602O. doi:10.1103/PhysRevC.74.044602. Retrieved 18 January 2008. <a href="http://link.aps.org/abstract/PRC/v74/e044602" target="_blank">http://link.aps.org/abstract/PRC/v74/e044602</a> <a href="#fnref:76" class="footnote-back-ref">↩</a></li>
<li id="fn:77">Discovery and Assignment of Elements with Atomic Numbers 113, 115, 117 and 118. IUPAC (30 December 2015) <a href="https://www.iupac.org/news/news-detail/article/discovery-and-assignment-of-elements-with-atomic-numbers-113-115-117-and-118.html" target="_blank">https://www.iupac.org/news/news-detail/article/discovery-and-assignment-of-elements-with-atomic-numbers-113-115-117-and-118.html</a> <a href="#fnref:77" class="footnote-back-ref">↩</a></li>
<li id="fn:78">Karol, Paul J.; Barber, Robert C.; Sherrill, Bradley M.; Vardaci, Emanuele; Yamazaki, Toshimitsu (29 December 2015). "Discovery of the element with atomic number Z = 118 completing the 7th row of the periodic table (IUPAC Technical Report)". Pure Appl. Chem. 88 (1–2): 155–160. doi:10.1515/pac-2015-0501. S2CID 102228960. <a href="https://zenodo.org/record/6472870" target="_blank">https://zenodo.org/record/6472870</a> <a href="#fnref:78" class="footnote-back-ref">↩</a></li>
<li id="fn:79">Voinov, A. A.; Oganessian, Yu. Ts; Abdullin, F. Sh.; Brewer, N. T.; Dmitriev, S. N.; Grzywacz, R. K.; Hamilton, J. H.; Itkis, M. G.; Miernik, K.; Polyakov, A. N.; Roberto, J. B.; Rykaczewski, K. P.; Sabelnikov, A. V.; Sagaidak, R. N.; Shriokovsky, I. V.; Shumeiko, M. V.; Stoyer, M. A.; Subbotin, V. G.; Sukhov, A. M.; Tsyganov, Yu. S.; Utyonkov, V. K.; Vostokin, G. K. (2016). "Results from the Recent Study of the 249–251Cf + 48Ca Reactions". In Peninozhkevich, Yu. E.; Sobolev, Yu. G. (eds.). Exotic Nuclei: EXON-2016 Proceedings of the International Symposium on Exotic Nuclei. Exotic Nuclei. pp. 219–223. ISBN 9789813226555. <a href="9789813226555" target="_blank">9789813226555</a> <a href="#fnref:79" class="footnote-back-ref">↩</a></li>
<li id="fn:80">Voinov, A. A.; Oganessian, Yu. Ts; Abdullin, F. Sh.; Brewer, N. T.; Dmitriev, S. N.; Grzywacz, R. K.; Hamilton, J. H.; Itkis, M. G.; Miernik, K.; Polyakov, A. N.; Roberto, J. B.; Rykaczewski, K. P.; Sabelnikov, A. V.; Sagaidak, R. N.; Shriokovsky, I. V.; Shumeiko, M. V.; Stoyer, M. A.; Subbotin, V. G.; Sukhov, A. M.; Tsyganov, Yu. S.; Utyonkov, V. K.; Vostokin, G. K. (2016). "Results from the Recent Study of the 249–251Cf + 48Ca Reactions". In Peninozhkevich, Yu. E.; Sobolev, Yu. G. (eds.). Exotic Nuclei: EXON-2016 Proceedings of the International Symposium on Exotic Nuclei. Exotic Nuclei. pp. 219–223. ISBN 9789813226555. <a href="9789813226555" target="_blank">9789813226555</a> <a href="#fnref:80" class="footnote-back-ref">↩</a></li>
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<li id="fn:93">"Российские физики предложат назвать 116 химический элемент московием (Russian Physicians Will Suggest to Name Element 116 Moscovium)" (in Russian). rian.ru. 2011. Retrieved 8 May 2011. <a href="https://ria.ru/science/20110326/358081075.html" target="_blank">https://ria.ru/science/20110326/358081075.html</a> <a href="#fnref:93" class="footnote-back-ref">↩</a></li>
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<li id="fn:95">"IUPAC Is Naming The Four New Elements Nihonium, Moscovium, Tennessine, And Oganesson". IUPAC. 8 June 2016. Archived from the original on 8 June 2016. <a href="https://iupac.org/iupac-is-naming-the-four-new-elements-nihonium-moscovium-tennessine-and-oganesson/" target="_blank">https://iupac.org/iupac-is-naming-the-four-new-elements-nihonium-moscovium-tennessine-and-oganesson/</a> <a href="#fnref:95" class="footnote-back-ref">↩</a></li>
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<li id="fn:99">Tarasevich, Grigoriy; Lapenko, Igor (2019). "Юрий Оганесян о тайнах ядра, новых элементах и смысле жизни" [Yuri Oganessian about the secret of the nucleus, new elements and the meaning of life]. Kot Shryodingyera (in Russian). No. Special. Direktsiya Festivalya Nauki. p. 22. <a href="#fnref:99" class="footnote-back-ref">↩</a></li>
<li id="fn:100">In Russian, Oganessian's name is spelled Оганесян [ˈɐgənʲɪˈsʲan]; the transliteration in accordance with the rules of the English language would be Oganesyan, with one s. Similarly, the Russian name for the element is оганесон, letter-for-letter oganeson.
Oganessian is the Russified version of the Armenian last name Hovhannisyan (Armenian: Հովհաննիսյան [hɔvhɑnnisˈjɑn]).
It means "son of Hovhannes", i.e., "son of John".
It is one of the most common surnames in Armenia. <a href="/wiki/Help:IPA/Russian" target="_blank">/wiki/Help:IPA/Russian</a> <a href="#fnref:100" class="footnote-back-ref">↩</a></li>
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</ol>

Oganesson open-in-new

Oganesson