Editing Meissa (section)

==Properties==
Meissa is a [[giant star]] with a [[stellar classification]] of O8&nbsp;III and an [[apparent magnitude|apparent visible magnitude]] 3.54. It is an enormous star with about 34<ref name=voss/> times the mass of the Sun and 10 times the Sun's radius. The [[stellar atmosphere|outer atmosphere]] has an [[effective temperature]] of around 35,000&nbsp;K,<ref name=Gordon2018/> giving it the characteristic blue glow of a hot [[O-type star]].<ref name=csiro/> Meissa is a soft X-ray source with a luminosity of 10<sup>32</sup> erg s<sup>−1</sup> and peak emission in the energy range of 0.2–0.3 keV, which suggests the X-rays are probably being generated by the [[stellar wind]].<ref name=aaa530_A150/> The stellar wind of Meissa is well characterized by a mass-loss rate of {{val|2.5|e=−8}} solar masses per year and a terminal velocity of {{val|2000|u=km/s|fmt=commas}}.<ref name=aaa628_A36/>

Meissa is actually a [[double star]] with a companion at an [[angular separation]] of 4.41&nbsp;[[arcsecond]]s along a [[position angle]] of 43.12° (as of 1937).<ref name=aass53_433/> This fainter component is of magnitude 5.61 and it has a stellar classification of B0.5&nbsp;V, making it a [[B-type main sequence star]].<ref>{{cite journal|doi=10.1086/300234 |title=ICCD Speckle Observations of Binary Stars. XIX. An Astrometric/Spectroscopic Survey of O Stars |date=1998 |last1=Mason |first1=Brian D. |last2=Gies |first2=Douglas R. |last3=Hartkopf |first3=William I. |last4=Bagnuolo, Jr. |first4=William G. |last5=Ten Brummelaar |first5=Theo |last6=McAlister |first6=Harold A. |journal=The Astronomical Journal |volume=115 |issue=2 |pages=821–847 |bibcode=1998AJ....115..821M }}</ref> There is an outlying component, Meissa C, which is an [[F-type main sequence star]] with a classification of F8&nbsp;V. This star in turn may have a very low mass companion that is probably a [[brown dwarf]].<ref name=aaa530_A150/>

In 2018, a companion was detected around Meissa A, with a project separation of 10.13 mas. However, it was not detected again.<ref name=Lanthermann>{{cite journal| bibcode=2023A&A...672A...6L|arxiv=2302.03168 |doi=10.1051/0004-6361/202245364 |title=Multiplicity of northern bright O-type stars with optical long baseline interferometry |date=2023 |last1=Lanthermann |first1=C. |last2=Le Bouquin |first2=J.-B. |last3=Sana |first3=H. |last4=Mérand |first4=A. |last5=Monnier |first5=J. D. |last6=Perraut |first6=K. |last7=Frost |first7=A. J. |last8=Mahy |first8=L. |last9=Gosset |first9=E. |last10=De Becker |first10=M. |last11=Kraus |first11=S. |last12=Anugu |first12=N. |last13=Davies |first13=C. L. |last14=Ennis |first14=J. |last15=Gardner |first15=T. |last16=Labdon |first16=A. |last17=Setterholm |first17=B. |last18=Ten Brummelaar |first18=T. |last19=Schaefer |first19=G. H. |journal=Astronomy & Astrophysics |volume=672 |pages=A6 |pmid=36974081 }}</ref>