K-type main-sequence star

<p>A K-type main-sequence star, also referred to as a K-type dwarf, or orange dwarf, is a <a href="/facts/Main_sequence/DJ3Wq8kd">main-sequence</a> (<a href="/facts/Hydrogen/BoYHjl0J">hydrogen</a>-burning) <a href="/facts/Star/PFbd6ICx">star</a> of <a href="/facts/Spectral_classification/dYrIuK9H">spectral type</a> K and <a href="/facts/Luminosity_class/dYrIuK9H">luminosity class</a> V. These stars are intermediate in size between red <a href="/facts/Red_dwarf/56CMQcF0">M-type main-sequence stars</a> ("red dwarfs") and yellow/white <a href="/facts/G-type_main-sequence_star/8zjE512K">G-type main-sequence stars</a>. They have masses between 0.6 and 0.9 times the <a href="/facts/Solar_mass/j6Auhku8">mass</a> of the <a href="/facts/Sun/CadPCVHh">Sun</a> and <a href="/facts/Effective_temperature/RY30DaSY">surface temperatures</a> between 3,900 and 5,300 <a href="/facts/Kelvin/E3trzC4C">K</a>. These stars are of particular interest in the search for <a href="/facts/Extraterrestrial_life/arxCPFTQ">extraterrestrial life</a> due to their stability and long lifespan. These stars stay on the main sequence for up to 70 billion years, a length of time much larger than the time the <a href="/facts/Universe/XbfpnDmM">universe</a> has existed (13.8 billion years), as such none have had sufficient time to leave the main sequence. Well-known examples include <a href="/facts/Alpha_Centauri/6BlySfIj">Alpha Centauri</a> B (K1 V), <a href="/facts/Epsilon_Indi/4Hjwnlh0">Epsilon Indi</a> (K5 V) and <a href="/facts/Epsilon_Eridani/5LMmzaXl">Epsilon Eridani</a> (K2 V).
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K-type main-sequence star open-in-new

K-type main-sequence star