Rigel

<h2 id="nomenclature">Nomenclature</h2>

In 2016, the <a href="/facts/International_Astronomical_Union/GMFPImXo">International Astronomical Union</a> (IAU) included the name "Rigel" in the IAU Catalog of Star Names.<a class="footnote-ref" id="fnref:1" href="#fn:1">1</a><a class="footnote-ref" id="fnref:2" href="#fn:2">2</a> According to the IAU, this proper name applies only to the primary component A of the Rigel system. The system is listed variously in historical <a href="/facts/Astronomical_catalogs/et5KvreH">astronomical catalogs</a> as <a href="/facts/Herschel_Catalogue_of_Double_Stars/SsruaBvq">H II</a> 33, <a href="/facts/Struve_Double_Star_Catalog/ajPxYc1q">Σ</a> 668, <a href="/facts/Burnham_Double_Star_Catalogue/ETJKXvSn">β</a> 555, or <a href="/facts/Aitken_Double_Star_Catalogue/fmjJ9d0A">ADS</a> 3823. For simplicity, Rigel's companions are referred to as Rigel B,<a class="footnote-ref" id="fnref:3" href="#fn:3">3</a> C, and D;<a class="footnote-ref" id="fnref:4" href="#fn:4">4</a><a class="footnote-ref" id="fnref:5" href="#fn:5">5</a> the IAU describes such names as "useful nicknames" that are "unofficial".<a class="footnote-ref" id="fnref:6" href="#fn:6">6</a> In modern comprehensive catalogs, the whole multiple star system is known as <a href="/facts/Washington_Double_Star_Catalog/U3xm5bKk">WDS</a> 05145-0812 or <a href="/facts/Catalog_of_Components_of_Double_and_Multiple_Stars/hqWgus5y">CCDM</a> 05145–0812.<a class="footnote-ref" id="fnref:7" href="#fn:7">7</a><a class="footnote-ref" id="fnref:8" href="#fn:8">8</a>
The designation of Rigel as β Orionis (<a href="/facts/Latinisation_of_names/69CA5FuQ">Latinized</a> to Beta Orionis) was made by <a href="/facts/Johann_Bayer/EIQFIELY">Johann Bayer</a> in 1603. The "beta" designation is commonly given to the second-brightest star in each constellation, but Rigel is almost always brighter than α Orionis (<a href="/facts/Betelgeuse/BsD9Ap7C">Betelgeuse</a>).<a class="footnote-ref" id="fnref:9" href="#fn:9">9</a> Astronomer <a href="/facts/James_B._Kaler/dCPF6Sr6">James B. Kaler</a> has speculated that Rigel was designated by Bayer during a rare period when it was outshone by the variable star Betelgeuse, resulting in the latter star being designated "alpha" and Rigel designated "beta".<a class="footnote-ref" id="fnref:10" href="#fn:10">10</a> Bayer did not strictly order the stars by brightness, instead grouping them by magnitude.<a class="footnote-ref" id="fnref:11" href="#fn:11">11</a> Rigel and Betelgeuse were both considered to be of the first magnitude class, and in Orion the stars of each class are thought to have been ordered north to south.<a class="footnote-ref" id="fnref:12" href="#fn:12">12</a> Rigel is included in the <a href="/facts/General_Catalogue_of_Variable_Stars/E0Q7I4bn">General Catalogue of Variable Stars</a>, but since it already has a <a href="/facts/Bayer_designation/KU2DVT47">Bayer designation</a> it has no separate <a href="/facts/Variable_star_designation/oAtUSb50">variable star designation</a>.<a class="footnote-ref" id="fnref:13" href="#fn:13">13</a>
Rigel has many other <a href="/facts/Stellar_designations_and_names/3rsQGseD">stellar designations</a> taken from various catalogs, including the <a href="/facts/Flamsteed_designation/wSHN0yNM">Flamsteed designation</a> 19 Orionis (19 Ori), the <a href="/facts/Bright_Star_Catalogue/P8nRWDfb">Bright Star Catalogue</a> entry HR 1713, and the <a href="/facts/Henry_Draper_Catalogue/BM9FaNQI">Henry Draper Catalogue</a> number HD 34085. These designations frequently appear in the scientific literature,<a class="footnote-ref" id="fnref:14" href="#fn:14">14</a><a class="footnote-ref" id="fnref:15" href="#fn:15">15</a><a class="footnote-ref" id="fnref:16" href="#fn:16">16</a> but rarely in popular writing.<a class="footnote-ref" id="fnref:17" href="#fn:17">17</a><a class="footnote-ref" id="fnref:18" href="#fn:18">18</a>

<h2 id="observation">Observation</h2>

Rigel is an <a href="/facts/Variable_star/Ac8mp2gy">intrinsic variable</a> star with an <a href="/facts/Apparent_magnitude/7pCTF1Me">apparent magnitude</a> ranging from 0.05 to 0.18.<a class="footnote-ref" id="fnref:19" href="#fn:19">19</a> It is typically the seventh-brightest star in the <a href="/facts/Celestial_sphere/TYAtXgor">celestial sphere</a>, excluding the Sun, although occasionally fainter than Betelgeuse.<a class="footnote-ref" id="fnref:20" href="#fn:20">20</a> It is fainter than <a href="/facts/Capella/bNQTaAjQ">Capella</a>, which may also vary slightly in brightness.<a class="footnote-ref" id="fnref:21" href="#fn:21">21</a> Rigel appears slightly blue-white and has a <a href="/facts/B-V_color/0SVRKKk0">B-V color</a> index of −0.06.<a class="footnote-ref" id="fnref:22" href="#fn:22">22</a> It contrasts strongly with reddish Betelgeuse.<a class="footnote-ref" id="fnref:23" href="#fn:23">23</a>
<a href="/facts/Culmination/qGHPjMRs">Culminating</a> every year at midnight on 12 December, and at 9:00 pm on 24 January, Rigel is visible on winter evenings in the <a href="/facts/Northern_Hemisphere/EFwyqL25">Northern Hemisphere</a> and on summer evenings in the <a href="/facts/Southern_Hemisphere/QfJ4z9L5">Southern Hemisphere</a>.<a class="footnote-ref" id="fnref:24" href="#fn:24">24</a> In the Southern Hemisphere, Rigel is the first bright star of Orion visible as the constellation rises.<a class="footnote-ref" id="fnref:25" href="#fn:25">25</a> Correspondingly, it is also the first star of Orion to set in most of the Northern Hemisphere. The star is a vertex of the "<a href="/facts/Winter_Hexagon/Ve7Rmvj0">Winter Hexagon</a>", an <a href="/facts/Asterism_(astronomy)/CFu0Qllg">asterism</a> that includes <a href="/facts/Aldebaran/PPa2xB93">Aldebaran</a>, Capella, <a href="/facts/Pollux_(star)/Gv5T0K3a">Pollux</a>, <a href="/facts/Procyon/43Nou3on">Procyon</a>, and <a href="/facts/Sirius/sHCkClse">Sirius</a>. Rigel is a prominent <a href="/facts/List_of_stars_for_navigation/NAcPQN9I">equatorial navigation star</a>, being easily located and readily visible in all the world's oceans (the exception is the area north of the <a href="/facts/82nd_parallel_north/Xn249doJ">82nd parallel north</a>).<a class="footnote-ref" id="fnref:26" href="#fn:26">26</a>

<h3>Spectroscopy</h3>
Rigel's <a href="/facts/Stellar_classification/dYrIuK9H">spectral type</a> is a defining point of the classification sequence for supergiants.<a class="footnote-ref" id="fnref:27" href="#fn:27">27</a><a class="footnote-ref" id="fnref:28" href="#fn:28">28</a> The overall spectrum is typical for a <a href="/facts/Late-type_star/dYrIuK9H">late</a> B class star, with strong <a href="/facts/Absorption_line/HuI4Bj5f">absorption lines</a> of the hydrogen <a href="/facts/Balmer_series/Vc4s4SIt">Balmer series</a> as well as neutral helium lines and some of heavier elements such as oxygen, calcium, and magnesium.<a class="footnote-ref" id="fnref:29" href="#fn:29">29</a> The <a href="/facts/Luminosity_class/dYrIuK9H">luminosity class</a> for B8 stars is estimated from the strength and narrowness of the hydrogen spectral lines, and Rigel is assigned to the <a href="/facts/Bright_supergiant/dYrIuK9H">bright supergiant</a> class Ia.<a class="footnote-ref" id="fnref:30" href="#fn:30">30</a> Variations in the spectrum have resulted in the assignment of different classes to Rigel, such as B8 Ia, B8 Iab, and B8 Iae.<a class="footnote-ref" id="fnref:31" href="#fn:31">31</a><a class="footnote-ref" id="fnref:32" href="#fn:32">32</a>
As early as 1888, the heliocentric <a href="/facts/Radial_velocity/B3NmbVLP">radial velocity</a> of Rigel, as estimated from the <a href="/facts/Doppler_shift/bzrK1BKf">Doppler shifts</a> of its spectral lines, was seen to vary. This was confirmed and interpreted at the time as being due to a spectroscopic companion with a period of about 22 days.<a class="footnote-ref" id="fnref:33" href="#fn:33">33</a> The radial velocity has since been measured to vary by about 10 <a href="/facts/Metre_per_second/hSEkho3J">km/s</a> around a mean of 21.5 km/s.<a class="footnote-ref" id="fnref:34" href="#fn:34">34</a>
In 1933, the <a href="/facts/H%CE%B1/Akk50rbI">Hα</a> line in Rigel's spectrum was seen to be unusually weak and shifted 0.1 <a href="/facts/Nanometre/a98sjHyu">nm</a> towards shorter wavelengths, while there was a narrow <a href="/facts/Emission_line/HuI4Bj5f">emission spike</a> about 1.5 nm to the long wavelength side of the main absorption line.<a class="footnote-ref" id="fnref:35" href="#fn:35">35</a> This is now known as a <a href="/facts/P_Cygni_profile/2DX0AFCD">P Cygni profile</a> after a star that shows this feature strongly in its spectrum. It is associated with <a href="/facts/Mass_loss/61jfD9bm">mass loss</a> where there is simultaneously emission from a dense wind close to the star and absorption from circumstellar material expanding away from the star.<a class="footnote-ref" id="fnref:36" href="#fn:36">36</a>
The unusual Hα line profile is observed to vary unpredictably. It is a normal absorption line around a third of the time. About a quarter of the time, it is a double-peaked line, that is, an absorption line with an emission core or an emission line with an absorption core. About a quarter of the time it has a P Cygni profile; most of the rest of the time, the line has an inverse P Cygni profile, where the emission component is on the short wavelength side of the line. Rarely, there is a pure emission Hα line.<a class="footnote-ref" id="fnref:37" href="#fn:37">37</a> The line profile changes are interpreted as variations in the quantity and velocity of material being expelled from the star. Occasional very high-velocity outflows have been inferred, and, more rarely, infalling material. The overall picture is one of large <a href="/facts/Coronal_loop/v3b2m7BK">looping structures</a> arising from the <a href="/facts/Photosphere/32a139LB">photosphere</a> and driven by magnetic fields.<a class="footnote-ref" id="fnref:38" href="#fn:38">38</a>

<h3>Variability</h3>

Rigel has been known to vary in brightness since at least 1930. The small amplitude of Rigel's brightness variation requires <a href="/facts/Photoelectric_sensor/Kvzf7YbQ">photoelectric</a> or <a href="/facts/CCD_photometry/fnV9JdSa">CCD photometry</a> to be reliably detected. This brightness variation has no obvious period. Observations over 18 nights in 1984 showed variations at red, blue, and yellow wavelengths of up to 0.13 magnitudes on timescales of a few hours to several days, but again no clear period. Rigel's <a href="/facts/Color_index/0SVRKKk0">color index</a> varies slightly, but this is not significantly correlated with its brightness variations.<a class="footnote-ref" id="fnref:39" href="#fn:39">39</a>
From analysis of <a href="/facts/Hipparcos/Th2HW7VN">Hipparcos</a> satellite photometry, Rigel is identified as belonging to the <a href="/facts/Alpha_Cygni_variable/xHf5J0Xe">Alpha Cygni</a> class of variable stars,<a class="footnote-ref" id="fnref:40" href="#fn:40">40</a> defined as "non-radially pulsating supergiants of the Bep–AepIa spectral types".<a class="footnote-ref" id="fnref:41" href="#fn:41">41</a> In those spectral types, the 'e' indicates that it displays emission lines in its spectrum, while the 'p' means it has an unspecified spectral peculiarity. Alpha Cygni type variables are generally considered to be irregular<a class="footnote-ref" id="fnref:42" href="#fn:42">42</a> or have <a href="/facts/Quasi-period/wgQDeW9s">quasi-periods</a>.<a class="footnote-ref" id="fnref:43" href="#fn:43">43</a> Rigel was added to the General Catalogue of Variable Stars in the 74th name-list of variable stars on the basis of the Hipparcos photometry,<a class="footnote-ref" id="fnref:44" href="#fn:44">44</a> which showed variations with a photographic amplitude of 0.039 magnitudes and a possible period of 2.075 days.<a class="footnote-ref" id="fnref:45" href="#fn:45">45</a> Rigel was observed with the Canadian <a href="/facts/Microvariability_and_Oscillations_of_STars_telescope/A2vjlJyT">MOST</a> satellite for nearly 28 days in 2009. Milli-magnitude variations were observed, and gradual changes in flux suggest the presence of long-period pulsation modes.<a class="footnote-ref" id="fnref:46" href="#fn:46">46</a>

<h3>Mass loss</h3>
From observations of the variable Hα spectral line, Rigel's mass-loss rate due to stellar wind is estimated be (1.5±0.4)×10−7 solar masses per year (<a href="/facts/Solar_mass/j6Auhku8">M☉</a>/yr)—about ten million times more than the mass-loss rate from the <a href="/facts/Sun/CadPCVHh">Sun</a>.<a class="footnote-ref" id="fnref:47" href="#fn:47">47</a> More detailed optical and <a href="/facts/K_band_(infrared)/1MPj6hJ3">K band</a> infrared spectroscopic observations, together with <a href="/facts/VLTI/xUQCLysQ">VLTI</a> interferometry, were taken from 2006 to 2010. Analysis of the Hα and <a href="/facts/H%CE%B3/Vc4s4SIt">Hγ</a> line profiles, and measurement of the regions producing the lines, show that Rigel's stellar wind varies greatly in structure and strength. Loop and arm structures were also detected within the wind. Calculations of mass loss from the Hγ line give (9.4±0.9)×10−7 M☉/yr in 2006-7 and (7.6±1.1)×10−7 M☉/yr in 2009–10. Calculations using the Hα line give lower results, around 1.5×10−7 M☉/yr. The terminal wind velocity is 300 km/s.<a class="footnote-ref" id="fnref:48" href="#fn:48">48</a> It is estimated that Rigel has lost about three solar masses (M☉) since beginning life as a star of 24±3 M☉ seven to nine million years ago.<a class="footnote-ref" id="fnref:49" href="#fn:49">49</a>

<h2 id="distance">Distance</h2>

Rigel's distance from the Sun is somewhat uncertain, different estimates being obtained by different methods. Old estimates placed it 166 parsecs (or 541 light years) away from the Sun.<a class="footnote-ref" id="fnref:50" href="#fn:50">50</a> The 2007 <a href="/facts/Hipparcos_new_reduction/Th2HW7VN">Hipparcos new reduction</a> of Rigel's <a href="/facts/Stellar_parallax/ywI9UWEJ">parallax</a> is 3.78±0.34 <a href="/facts/Milliarcsecond/tybs6YGC">mas</a>, giving a distance of 863 light-years (265 parsecs) with a <a href="/facts/Margin_of_error/BtnDQ0Iu">margin of error</a> of about 9%.<a class="footnote-ref" id="fnref:51" href="#fn:51">51</a> Rigel B, usually considered to be physically associated with Rigel and at the same distance, has a <a href="/facts/Gaia_Data_Release_3/dlvcdkoN">Gaia Data Release 3</a> parallax of 3.2352±0.0553 mas, suggesting a distance around 1,000 light-years (310 parsecs). However, the measurements for this object may be unreliable.<a class="footnote-ref" id="fnref:52" href="#fn:52">52</a>
Indirect distance estimation methods have also been employed. For example, Rigel is believed to be in a region of <a href="/facts/Nebulosity/hG6coklY">nebulosity</a>, its radiation illuminating several nearby clouds. Most notable of these is the 5°-long <a href="/facts/IC_2118/zvoklJEA">IC 2118</a> (Witch Head Nebula),<a class="footnote-ref" id="fnref:53" href="#fn:53">53</a><a class="footnote-ref" id="fnref:54" href="#fn:54">54</a> located at an <a href="/facts/Angular_separation/6ob2n0Wb">angular separation</a> of 2.5° from the star,<a class="footnote-ref" id="fnref:55" href="#fn:55">55</a> or a projected distance of 39 light-years (12 parsecs) away.<a class="footnote-ref" id="fnref:56" href="#fn:56">56</a> From measures of other nebula-embedded stars, IC 2118's distance is estimated to be 949 ± 7 light-years (291 ± 2 parsecs).<a class="footnote-ref" id="fnref:57" href="#fn:57">57</a>
Rigel is an outlying member of the <a href="/facts/Orion_OB1_association/sqzFE4S7">Orion OB1 association</a>, which is located at a distance of up to 1,600 light-years (500 parsecs) from Earth. It is a member of the loosely defined <a href="/facts/Taurus-Orion_R1_Association/sqzFE4S7">Taurus-Orion R1 Association</a>, somewhat closer at 1,200 light-years (360 parsecs).<a class="footnote-ref" id="fnref:58" href="#fn:58">58</a><a class="footnote-ref" id="fnref:59" href="#fn:59">59</a> Rigel is thought to be considerably closer than most of the members of Orion OB1 and the <a href="/facts/Orion_Nebula/6VWbcqzL">Orion Nebula</a>. Betelgeuse and <a href="/facts/Saiph/fmLAeQkf">Saiph</a> lie at a similar distance to Rigel, although Betelgeuse is a <a href="/facts/Runaway_star/6q1SRvDa">runaway star</a> with a complex history and might have originally formed in the main body of the association.<a class="footnote-ref" id="fnref:60" href="#fn:60">60</a>

<h2 id="stellar-system">Stellar system</h2>

<table><tbody><tr><td colspan="2" rowspan="2"></td><td></td><td></td><td colspan="6" rowspan="2">Rigel</td><td colspan="2" rowspan="2"></td></tr><tr><td></td><td></td></tr><tr><td colspan="2" rowspan="2"></td><td rowspan="2"></td><td rowspan="2"></td><td colspan="6" rowspan="2">Separation = 9.5″Period = 24,000 y</td></tr><tr></tr><tr><td colspan="2"></td><td></td><td rowspan="2"></td><td colspan="2" rowspan="2"></td><td></td><td></td><td colspan="2"></td><td colspan="6" rowspan="2">Ba</td></tr><tr><td colspan="2"></td><td></td><td></td><td></td><td colspan="2"></td></tr><tr><td colspan="2" rowspan="2"></td><td rowspan="2"></td><td rowspan="2"></td><td></td><td></td><td></td><td rowspan="2"></td><td colspan="6" rowspan="2">Separation = 0.58 masPeriod = 9.860 d</td></tr><tr><td></td><td></td><td></td></tr><tr><td colspan="2" rowspan="2"></td><td rowspan="2"></td><td rowspan="2"></td><td rowspan="2"></td><td rowspan="2"></td><td></td><td></td><td colspan="2"></td><td colspan="6" rowspan="2">Bb</td></tr><tr><td colspan="2"></td><td colspan="2"></td></tr><tr><td colspan="2" rowspan="2"></td><td></td><td></td><td></td><td rowspan="2"></td><td colspan="6" rowspan="2">Separation = 0.1″Period = 63 y</td></tr><tr><td colspan="2"></td><td></td></tr><tr><td colspan="2" rowspan="2"></td><td colspan="2" rowspan="2"></td><td></td><td></td><td colspan="6" rowspan="2">C</td><td colspan="2" rowspan="2"></td></tr><tr><td colspan="2"></td></tr></tbody></table>
<a href="/facts/Star_systems/1vX99BMV">Hierarchical scheme</a> for Rigel's components<a class="footnote-ref" id="fnref:61" href="#fn:61">61</a>

The <a href="/facts/Multiple_star_system/1vX99BMV">star system</a> of which Rigel is a part has at least four components. Rigel (sometimes called Rigel A to distinguish from the other components) has a <a href="/facts/Visual_double_star/3BNpoSVf">visual companion</a>, which is likely a close triple-star system. A fainter star at a wider separation might be a fifth component of the Rigel system.
<a href="/facts/William_Herschel/SsruaBvq">William Herschel</a> discovered Rigel to be a visual double star on 1 October 1781, cataloguing it as star 33 in the "second class of double stars" in his Catalogue of Double Stars,<a class="footnote-ref" id="fnref:62" href="#fn:62">62</a> usually abbreviated to H II 33, or as H 2 33 in the Washington Double Star Catalogue.<a class="footnote-ref" id="fnref:63" href="#fn:63">63</a> <a href="/facts/Friedrich_Georg_Wilhelm_von_Struve/ajPxYc1q">Friedrich Georg Wilhelm von Struve</a> first measured the relative position of the companion in 1822, cataloguing the visual pair as Σ 668.<a class="footnote-ref" id="fnref:64" href="#fn:64">64</a><a class="footnote-ref" id="fnref:65" href="#fn:65">65</a> The secondary star is often referred to as Rigel B or β Orionis B. The angular separation of Rigel B from Rigel A is 9.5 arc seconds to its south along <a href="/facts/Position_angle/TXCTArC6">position angle</a> 204°.<a class="footnote-ref" id="fnref:66" href="#fn:66">66</a><a class="footnote-ref" id="fnref:67" href="#fn:67">67</a> Although not particularly faint at <a href="/facts/Visual_magnitude/7pCTF1Me">visual magnitude</a> 6.7, the overall difference in brightness from Rigel A (about 6.6 magnitudes or 440 times fainter) makes it a challenging target for telescope apertures smaller than 15 cm (6 in).<a class="footnote-ref" id="fnref:68" href="#fn:68">68</a>
At Rigel's estimated distance, Rigel B's <a href="/facts/Projected_separation/k2uNIRzM">projected separation</a> from Rigel A is over 2,200 <a href="/facts/Astronomical_unit/gjsbu5xU">astronomical units</a> (AU). Since its discovery, there has been no sign of orbital motion, although both stars share a similar <a href="/facts/Proper_motion/ECByRQ8c">common proper motion</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> The pair would have an estimated orbital period of 24,000 years.<a class="footnote-ref" id="fnref:71" href="#fn:71">71</a> Gaia Data Release 3 (DR3) contains a probably unreliable parallax for Rigel B, placing it at about 1,010 light-years (309 parsecs), further away than the Hipparcos distance for Rigel, but similar to the Taurus-Orion R1 association. There is no parallax for Rigel in Gaia DR3. The Gaia DR3 proper motions for Rigel B and the Hipparcos proper motions for Rigel are both small, although not quite the same.<a class="footnote-ref" id="fnref:72" href="#fn:72">72</a>
In 1871, <a href="/facts/Sherburne_Wesley_Burnham/pBGUQJyT">Sherburne Wesley Burnham</a> suspected Rigel B to be a binary system, and in 1878, he resolved it into two components.<a class="footnote-ref" id="fnref:73" href="#fn:73">73</a> This visual companion is designated as component C (Rigel C), with a measured separation from component B that varies from less than 0.1″ to around 0.3″.<a class="footnote-ref" id="fnref:74" href="#fn:74">74</a><a class="footnote-ref" id="fnref:75" href="#fn:75">75</a> In 2009, <a href="/facts/Speckle_interferometric/wr4y6aX8">speckle interferometry</a> showed the two almost identical components separated by 0.124″,<a class="footnote-ref" id="fnref:76" href="#fn:76">76</a> with visual magnitudes of 7.5 and 7.6, respectively.<a class="footnote-ref" id="fnref:77" href="#fn:77">77</a> Their estimated orbital period is 63 years.<a class="footnote-ref" id="fnref:78" href="#fn:78">78</a> Burnham listed the Rigel multiple system as β 555 in his <a href="/facts/Burnham_Double_Star_Catalogue/ETJKXvSn">double star catalog</a><a class="footnote-ref" id="fnref:79" href="#fn:79">79</a> or BU 555 in modern use.<a class="footnote-ref" id="fnref:80" href="#fn:80">80</a>
Component B is a double-lined <a href="/facts/Spectroscopic_binary/TYlDe1bD">spectroscopic binary</a> system, which shows two sets of <a href="/facts/Spectral_line/HuI4Bj5f">spectral lines</a> combined within its single <a href="/facts/Stellar_spectrum/NDGQ7mmM">stellar spectrum</a>. Periodic changes observed in relative positions of these lines indicate an orbital period of 9.86 days. The two spectroscopic components Rigel Ba and Rigel Bb cannot be resolved in optical telescopes but are known to both be hot stars of spectral type around B9. This spectroscopic binary, together with the close visual component Rigel C, is likely a physical triple-star system,<a class="footnote-ref" id="fnref:81" href="#fn:81">81</a> although Rigel C cannot be detected in the spectrum, which is inconsistent with its observed brightness.<a class="footnote-ref" id="fnref:82" href="#fn:82">82</a>
In 1878, Burnham found another possibly associated star of approximately 13th magnitude. He listed it as component D of β 555,<a class="footnote-ref" id="fnref:83" href="#fn:83">83</a> although it is unclear whether it is physically related or a coincidental alignment. Its 2017 separation from Rigel was 44.5<a href="/facts/Second_of_arc/tybs6YGC">″</a>, almost due north at a position angle of 1°.<a class="footnote-ref" id="fnref:84" href="#fn:84">84</a> Gaia DR2 finds it to be a 12th magnitude sunlike star at approximately the same distance as Rigel.<a class="footnote-ref" id="fnref:85" href="#fn:85">85</a> Likely a <a href="/facts/K-type_main-sequence_star/loWHS8PD">K-type main-sequence star</a>, this star would have an orbital period of around 250,000 years, if it is part of the Rigel system.<a class="footnote-ref" id="fnref:86" href="#fn:86">86</a>
A spectroscopic companion to Rigel was reported on the basis of radial velocity variations, and its orbit was even calculated, but subsequent work suggests the star does not exist and that observed pulsations are intrinsic to Rigel itself.<a class="footnote-ref" id="fnref:87" href="#fn:87">87</a>

<h2 id="physical-characteristics">Physical characteristics</h2>

Rigel is a <a href="/facts/Blue_supergiant/8Bnl7Xpz">blue supergiant</a> that has exhausted the hydrogen fuel in its core, expanded and cooled as it moved away from the <a href="/facts/Main_sequence/DJ3Wq8kd">main sequence</a> across the upper part of the <a href="/facts/Hertzsprung%E2%80%93Russell_diagram/53YWnCvR">Hertzsprung–Russell diagram</a>.<a class="footnote-ref" id="fnref:88" href="#fn:88">88</a><a class="footnote-ref" id="fnref:89" href="#fn:89">89</a> When it was on the main sequence, its <a href="/facts/Effective_temperature/RY30DaSY">effective temperature</a> would have been around 30,000 <a href="/facts/Kelvin/E3trzC4C">K</a>.<a class="footnote-ref" id="fnref:90" href="#fn:90">90</a> Rigel's complex variability at <a href="/facts/Electromagnetic_spectrum/24LARvFY">visual wavelengths</a> is caused by <a href="/facts/Stellar_pulsations/g9dpv63g">stellar pulsations</a> similar to those of <a href="/facts/Deneb/L7dTfcog">Deneb</a>. Further observations of radial velocity variations indicate that it simultaneously oscillates in at least 19 non-radial modes with periods ranging from about 1.2 to 74 days.<a class="footnote-ref" id="fnref:91" href="#fn:91">91</a>
Estimation of many physical characteristics of blue supergiant stars, including Rigel, is challenging due to their rarity and uncertainty about how far they are from the Sun. As such, their characteristics are mainly estimated from theoretical <a href="/facts/Stellar_evolution/Qa4vAGmn">stellar evolution models</a>.<a class="footnote-ref" id="fnref:92" href="#fn:92">92</a> Its effective temperature can be estimated from the spectral type and color to be around 12,100 <a href="/facts/Kelvin/E3trzC4C">K</a>.<a class="footnote-ref" id="fnref:93" href="#fn:93">93</a> A mass of 21±3 M☉ at an age of 8±1 million years has been estimated by comparing evolutionary tracks, while atmospheric modeling from the spectrum gives a mass of 24±8 M☉.<a class="footnote-ref" id="fnref:94" href="#fn:94">94</a>
Although Rigel is often considered the most luminous star within 1,000 light-years of the Sun,<a class="footnote-ref" id="fnref:95" href="#fn:95">95</a><a class="footnote-ref" id="fnref:96" href="#fn:96">96</a> its energy output is poorly known. Using the Hipparcos distance of 860 light-years (264 parsecs), the estimated relative luminosity for Rigel is about 120,000 times that of the Sun (<a href="/facts/Solar_luminosity/CLG0r9bP">L☉</a>),<a class="footnote-ref" id="fnref:97" href="#fn:97">97</a> but another recently published distance of 1,170 ± 130 light-years (360 ± 40 parsecs) suggests an even higher luminosity of 219,000 L☉.<a class="footnote-ref" id="fnref:98" href="#fn:98">98</a> Other calculations based on theoretical stellar evolutionary models of Rigel's atmosphere give luminosities anywhere between 83,000 L☉ and 363,000 L☉,<a class="footnote-ref" id="fnref:99" href="#fn:99">99</a> while summing the <a href="/facts/Spectral_energy_distribution/6vC1Pnl6">spectral energy distribution</a> from historical photometry with the Hipparcos distance suggests a luminosity as low as 61,515±11,486 L☉.<a class="footnote-ref" id="fnref:100" href="#fn:100">100</a> A 2018 study using the <a href="/facts/Navy_Precision_Optical_Interferometer/3WWkA8ef">Navy Precision Optical Interferometer</a> measured the <a href="/facts/Angular_diameter/p2xv4vcQ">angular diameter</a> as 2.526 mas. After correcting for <a href="/facts/Limb_darkening/DIMsHUUs">limb darkening</a>, the angular diameter is found to be 2.606±0.009 mas, yielding a radius of 74.1+6.1−7.3 <a href="/facts/Solar_radius/5t1Xavju">R☉</a>.<a class="footnote-ref" id="fnref:101" href="#fn:101">101</a> An older measurement of the angular diameter gives 2.75±0.01 mas,<a class="footnote-ref" id="fnref:102" href="#fn:102">102</a> equivalent to a radius of 78.9 R☉ at 264 pc.<a class="footnote-ref" id="fnref:103" href="#fn:103">103</a> These radii are calculated assuming the Hipparcos distance of 264 pc; adopting a distance of 360 pc leads to a significantly larger size.<a class="footnote-ref" id="fnref:104" href="#fn:104">104</a> Older distance estimates were mostly far lower than modern estimates, leading to lower radius estimates; a 1922 estimate by <a href="/facts/John_Stanley_Plaskett/ND7o8SNo">John Stanley Plaskett</a> gave Rigel a diameter of 25 million miles, or approximately 28.9 R☉, smaller than its neighbor <a href="/facts/Aldebaran/PPa2xB93">Aldebaran</a>.<a class="footnote-ref" id="fnref:105" href="#fn:105">105</a>
Due to their closeness to each other and ambiguity of the spectrum, little is known about the intrinsic properties of the members of the Rigel BC triple system. All three stars seem to be near equally hot <a href="/facts/B-type_main-sequence_star/CKlAwIES">B-type main-sequence stars</a> that are three to four times as massive as the Sun.<a class="footnote-ref" id="fnref:106" href="#fn:106">106</a>

<h2 id="evolution">Evolution</h2>
<a href="/facts/Stellar_evolution/Qa4vAGmn">Stellar evolution</a> models suggest the pulsations of Rigel are powered by nuclear reactions in a hydrogen-burning shell that is at least partially non-convective. These pulsations are stronger and more numerous in stars that have evolved through a <a href="/facts/Red_supergiant/hPBWvABE">red supergiant</a> phase and then increased in temperature to again become a blue supergiant. This is due to the decreased mass and increased levels of fusion products at the surface of the star.<a class="footnote-ref" id="fnref:107" href="#fn:107">107</a>
Rigel is likely to be <a href="/facts/Triple-alpha_process/wV6lacSF">fusing helium</a> in its core.<a class="footnote-ref" id="fnref:108" href="#fn:108">108</a> Due to strong convection of helium produced in the core while Rigel was on the main sequence and in the hydrogen-burning shell since it became a supergiant, the fraction of helium at the surface has increased from 26.6% when the star formed to 32% now. The surface abundances of carbon, nitrogen, and oxygen seen in the spectrum are compatible with a post-red supergiant star only if its internal convection zones are modeled using non-homogeneous chemical conditions known as the <a href="/facts/Paul_Ledoux/bsDRoEVy">Ledoux Criteria</a>.<a class="footnote-ref" id="fnref:109" href="#fn:109">109</a>
Rigel is expected to eventually end its stellar life as a <a href="/facts/Type_II_supernova/623d9YYT">type II supernova</a>.<a class="footnote-ref" id="fnref:110" href="#fn:110">110</a> It is one of the closest known potential <a href="/facts/Supernova/Pfo2J23l">supernova</a> progenitors to Earth,<a class="footnote-ref" id="fnref:111" href="#fn:111">111</a> and would be expected to have a maximum apparent magnitude of around −11 (about the same brightness as a quarter Moon or around 300 times brighter than Venus ever gets).<a class="footnote-ref" id="fnref:112" href="#fn:112">112</a> The supernova would leave behind either a black hole or a neutron star.<a class="footnote-ref" id="fnref:113" href="#fn:113">113</a>

<h2 id="etymology-and-cultural-significance">Etymology and cultural significance</h2>

The earliest known recording of the name Rigel is in the <a href="/facts/Alfonsine_tables/P9Ddfn9a">Alfonsine tables</a> of 1521. It is derived from the Arabic name Rijl Jauzah al Yusrā, "the left leg (foot) of Jauzah" (i.e. rijl meaning "leg, foot"),<a class="footnote-ref" id="fnref:114" href="#fn:114">114</a> which can be traced to the 10th century.<a class="footnote-ref" id="fnref:115" href="#fn:115">115</a> "Jauzah" was a proper name for Orion; an alternative Arabic name was رجل الجبار rijl al-jabbār, "the foot of the great one", from which stems the rarely used variant names Algebar or Elgebar. The Alphonsine tables saw its name split into "Rigel" and "Algebar", with the note, et dicitur Algebar. Nominatur etiam Rigel.<a class="footnote-ref" id="fnref:116" href="#fn:116">116</a><a class="footnote-ref" id="fnref:117" href="#fn:117">117</a> Alternate spellings from the 17th century include Regel by Italian astronomer <a href="/facts/Giovanni_Battista_Riccioli/RjD2EPTw">Giovanni Battista Riccioli</a>, Riglon by German astronomer <a href="/facts/Wilhelm_Schickard/8e3EucNk">Wilhelm Schickard</a>, and Rigel Algeuze or Algibbar by English scholar <a href="/facts/Edmund_Chilmead/5jno0t39">Edmund Chilmead</a>.<a class="footnote-ref" id="fnref:118" href="#fn:118">118</a>
With the constellation representing the mythological Greek huntsman <a href="/facts/Orion_(mythology)/eekDxh9u">Orion</a>, Rigel is his knee or (as its name suggests) foot; with the nearby star <a href="/facts/Beta_Eridani/dmsmWR1q">Beta Eridani</a> marking Orion's footstool.<a class="footnote-ref" id="fnref:119" href="#fn:119">119</a> Rigel is presumably the star known as "<a href="/facts/Aurvandil/go5uGRsp">Aurvandil</a>'s toe" in <a href="/facts/Norse_mythology/hEKfeQql">Norse mythology</a>.<a class="footnote-ref" id="fnref:120" href="#fn:120">120</a> In the Caribbean, Rigel represented the severed leg of the folkloric figure Trois Rois, himself represented by the three stars of Orion's Belt. The leg had been severed with a cutlass by the maiden Bįhi (Sirius).<a class="footnote-ref" id="fnref:121" href="#fn:121">121</a> The <a href="/facts/Lacandon_people/Bc15rqw9">Lacandon people</a> of southern Mexico knew it as tunsel ("little woodpecker").<a class="footnote-ref" id="fnref:122" href="#fn:122">122</a>
Rigel was known as Yerrerdet-kurrk to the <a href="/facts/Wotjobaluk/33Pre0T2">Wotjobaluk</a> <a href="/facts/Koori/ljTKVvJL">koori</a> of southeastern Australia, and held to be the mother-in-law of Totyerguil (<a href="/facts/Altair/avsmInG0">Altair</a>). The distance between them signified the taboo preventing a man from approaching his mother-in-law.<a class="footnote-ref" id="fnref:123" href="#fn:123">123</a> The indigenous <a href="/facts/Wergaia/k563Imgy">Boorong</a> people of northwestern Victoria named Rigel as Collowgullouric Warepil.<a class="footnote-ref" id="fnref:124" href="#fn:124">124</a> The <a href="/facts/Wardaman_people/bDNDNCee">Wardaman people</a> of northern Australia know Rigel as the Red <a href="/facts/Kangaroo/gfYqeTRt">Kangaroo</a> Leader Unumburrgu and chief conductor of ceremonies in a songline when Orion is high in the sky. <a href="/facts/Eridanus_(constellation)/cvtlSUun">Eridanus</a>, the river, marks a line of stars in the sky leading to it, and the other stars of Orion are his ceremonial tools and entourage. Betelgeuse is Ya-jungin "Owl Eyes Flicking", watching the ceremonies.<a class="footnote-ref" id="fnref:125" href="#fn:125">125</a>
The <a href="/facts/M%C4%81ori_people/cvfbQmp8">Māori people</a> of New Zealand named Rigel as <a href="/facts/Puanga/RbKIGsgX">Puanga</a>, said to be a daughter of Rehua (<a href="/facts/Antares/adRhtq7X">Antares</a>), the chief of all-stars.<a class="footnote-ref" id="fnref:126" href="#fn:126">126</a> Its <a href="/facts/Heliacal_rising/U3qpNQN7">heliacal rising</a> presages the appearance of <a href="/facts/Matariki/RbKIGsgX">Matariki</a> (the <a href="/facts/Pleiades/tjwtx82z">Pleiades</a>) in the dawn sky, marking the Māori New Year in late May or early June. The <a href="/facts/Moriori_people/LdouxTq2">Moriori people</a> of the <a href="/facts/Chatham_Islands/rrjd670d">Chatham Islands</a>, as well as some Maori groups in New Zealand, mark the start of their New Year with Rigel rather than the Pleiades.<a class="footnote-ref" id="fnref:127" href="#fn:127">127</a> Puaka is a <a href="/facts/M%C4%81ori_language/pVhKfILB">southern name variant</a> used in the South Island.<a class="footnote-ref" id="fnref:128" href="#fn:128">128</a>
In Japan, the Minamoto or <a href="/facts/Genji_clan/zUhSp6e0">Genji clan</a> chose Rigel and its white color as its symbol, calling the star Genji-boshi (源氏星), while the Taira or <a href="/facts/Heike_clan/YQGyw1R1">Heike clan</a> adopted Betelgeuse and its red color. The two powerful families fought the <a href="/facts/Genpei_War/KUM8vgx4">Genpei War</a>; the stars were seen as facing off against each other and kept apart only by the three stars of <a href="/facts/Orion%27s_Belt/LDYvIgaJ">Orion's Belt</a>.<a class="footnote-ref" id="fnref:129" href="#fn:129">129</a><a class="footnote-ref" id="fnref:130" href="#fn:130">130</a><a class="footnote-ref" id="fnref:131" href="#fn:131">131</a>

<h2 id="in-modern-culture">In modern culture</h2>
The <a href="/facts/MS_Rigel/AFjyIPCe">MS Rigel</a> was originally a Norwegian ship, built in Copenhagen in 1924. It was requisitioned by the Germans during <a href="/facts/World_War_II/2efV5L1U">World War II</a> and sunk in 1944 while being used to transport prisoners of war.<a class="footnote-ref" id="fnref:132" href="#fn:132">132</a> Two US Navy ships have borne the name <a href="/facts/USS_Rigel/3nsTlPvf">USS Rigel</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><a class="footnote-ref" id="fnref:135" href="#fn:135">135</a> The <a href="/facts/SSM-N-6_Rigel/5su8dVkJ">SSM-N-6 Rigel</a> was a <a href="/facts/Cruise_missile/Frego9PF">cruise missile</a> program for the <a href="/facts/US_Navy/xYK0fUou">US Navy</a> that was cancelled in 1953 before reaching deployment.<a class="footnote-ref" id="fnref:136" href="#fn:136">136</a>

The <a href="/facts/Rigel_Skerries/Jeg62Rmn">Rigel Skerries</a> are a chain of small islands in <a href="/facts/Antarctica/bEM5Lem5">Antarctica</a>, renamed after originally being called Utskjera. They were given their current name as Rigel was used as an <a href="/facts/Astrofix/pCpbhzJt">astrofix</a>.<a class="footnote-ref" id="fnref:137" href="#fn:137">137</a> <a href="/facts/Mount_Rigel/h83pG2td">Mount Rigel</a>, elevation 1,910 m (6,270 ft), is also in Antarctica.<a class="footnote-ref" id="fnref:138" href="#fn:138">138</a>
<h2 id="see-also">See also</h2>
<ul><li><a href="/facts/Orion_in_Chinese_astronomy/qURaB5du">Orion in Chinese astronomy</a></li></ul>
<h2 id="notes">Notes</h2>

<h2 id="external-links">External links</h2>

Wikimedia Commons has media related to Rigel.

<ul><li><a href="https://apod.nasa.gov/apod/ap180115.html">NASA Astronomy Picture of the Day: Rigel and the Witch Head Nebula (15 January 2018)</a></li>
<li><a href="https://apod.nasa.gov/apod/ap151116.html">NASA Astronomy Picture of the Day: A Blazing Fireball between the Orion Nebula and Rigel (16 November 2015)</a></li>
<li><a href="http://assa.saao.ac.za/sections/deep-sky/double-stars/news-and-articles/december-double-star-of-the-month-beta-orionis/">December double star of the month – beta Orionis</a> Astronomical Society of Southern Africa</li>
<li><a href="https://www.aavso.org/my-favorite-double-star">My Favorite Double Star</a> AAVSO</li></ul>

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<li id="fn:116">lit."... and it is called Algebar. It is also named Rigel." <a href="#fnref:116" class="footnote-back-ref">↩</a></li>
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<li id="fn:135">"80-G-1017252 USS Rigel (AF-58)". Naval History and Heritage Command. Retrieved 14 June 2020. <a href="https://www.history.navy.mil/content/history/nhhc/our-collections/photography/numerical-list-of-images/nara-series/80-g/80-G-1010000/80-g-1017252-uss-rigel--af-58-.html" target="_blank">https://www.history.navy.mil/content/history/nhhc/our-collections/photography/numerical-list-of-images/nara-series/80-g/80-G-1010000/80-g-1017252-uss-rigel--af-58-.html</a> <a href="#fnref:135" class="footnote-back-ref">↩</a></li>
<li id="fn:136">Yenne, Bill (2018). The Complete History of U.S. Cruise Missiles. Forest Lake, Minnesota: Specialty Press. p. 69. ISBN 978-1-58007-256-4. <a href="978-1-58007-256-4" target="_blank">978-1-58007-256-4</a> <a href="#fnref:136" class="footnote-back-ref">↩</a></li>
<li id="fn:137">"Antarctica Detail: ID 12640". U.S. Geological Survey. U.S. Department of the Interior. Archived from the original on 2 February 2019. Retrieved 2 February 2019. <a href="https://geonames.usgs.gov/apex/f?p=gnispq:5:0::NO::P5_ANTAR_ID:12640" target="_blank">https://geonames.usgs.gov/apex/f?p=gnispq:5:0::NO::P5_ANTAR_ID:12640</a> <a href="#fnref:137" class="footnote-back-ref">↩</a></li>
<li id="fn:138">"Antarctica Detail: ID 12639". U.S. Geological Survey. U.S. Department of the Interior. Retrieved 2 February 2019. <a href="https://geonames.usgs.gov/apex/f?p=gnispq:5:0::NO::P5_ANTAR_ID:12639" target="_blank">https://geonames.usgs.gov/apex/f?p=gnispq:5:0::NO::P5_ANTAR_ID:12639</a> <a href="#fnref:138" class="footnote-back-ref">↩</a></li>
</ol>

Rigel open-in-new

Rigel