Meissa

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Meissa
λ (circled) in the constellation Orion.
Observation data
Epoch J2000      Equinox J2000
Constellation Orion
A
Right ascension 05h 35m 08.27608s[1]
Declination +09° 56′ 02.9913″[1]
Apparent magnitude (V) 3.7[2]
B
Right ascension 05h 35m 08.48130s[3]
Declination +09° 56′ 06.0995″[3]
Apparent magnitude (V) 5.6[2]
Characteristics
A
Spectral type O8 III((f))[4]
U−B color index −1.01[5]
B−V color index −0.21[5]
B
Spectral type B0 V[5]
U−B color index −0.77[5]
B−V color index +0.04[5]
Astrometry
Radial velocity (Rv)+30.10[6] km/s
A
Distance
1,320 ± 80 ly
(410 ± 30 pc)
Absolute magnitude (MV)−1.94
Details
A
Myr
HR
 1879
B: HD 36862, HR 1880
Database references
SIMBADλ Ori
A
B

Meissa

luminous and only slightly further away than Rigel, it appears 3 magnitudes dimmer at visual wavelengths, with much of its radiation emitted in the ultraviolet
due to its high temperature.

Nomenclature

φ2 Orionis

Lambda Orionis is the star's

Arabic Al-Maisan which means 'The Shining One'. Al-Maisan was originally used for Gamma Geminorum, but was mistakenly applied to Lambda Orionis and the name stuck.[13] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[14] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[15] included a table of the first two batches of names approved by the WGSN; which included Meissa for this star. It is now so entered in the IAU Catalog of Star Names.[16]

The original Arabic name for this star, Al Hakah (the source for another name for it, Heka) refers to the Arabic lunar mansion that includes this star and the two of

Chinese name for Meissa itself is 觜宿一 (Zī Sù yī, English: the First Star of Turtle Beak.)[18]

Properties

Meissa is a giant star with a stellar classification of O8 III and an apparent visible magnitude 3.54. It is an enormous star with about 34[7] times the mass of the Sun and 10 times the Sun's radius. The outer atmosphere has an effective temperature of around 35,000 K,[8] giving it the characteristic blue glow of a hot O-type star.[19] Meissa is a soft X-ray source with a luminosity of 1032 erg s−1 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.[20] The stellar wind of Meissa is well characterized by a mass-loss rate of 2.5×10−8 solar masses per year and a terminal velocity of 2,000 km/s.[9]

Meissa is actually a

F-type main sequence star with a classification of F8 V. This star in turn may have a very low mass companion that is probably a brown dwarf.[20]

In 2018, a companion was detected around Meissa A, with a project separation of 10.13 mas. However, it was not detected again.[23]

Ring

WISE infrared view of the ring around Meissa, which is the faint "white" star north of the small bright red nebula.
(NASA/JPL-Caltech/UCLA)

Meissa is surrounded by a ring of nebulosity about 12 degrees across. It is thought to be the remains of a supernova explosion, now ionized by the ultraviolet radiation from Meissa itself and some of the surrounding hot stars.[24]

Cluster

This star is the dominant member of a 5-million-year-old star-forming region known as the λ Orionis cluster,

Sh2-264[26] H II region in the neighboring volume of space, which in turn is surrounded by an expanding ring of cool gas that has an age of about 2–6 million years. The expansion of this gaseous ring may be explained by a former binary companion of Meissa that became a Type II supernova. Such an event would also explain the star's peculiar velocity with respect to the center of the expanding ring, as the explosion and resulting mass loss could have kicked Meissa out of the system. A potential candidate for the supernova remnant is the neutron star Geminga.[27] However, the last is unlikely given the distance between Geminga and the cluster.[28]

  • Lambda Orionis A, B and C. Background image was taken with Spitzer and insert showing the AB components is from Gemini
    Lambda Orionis A, B and C. Background image was taken with Spitzer and insert showing the AB components is from Gemini
  • This image taken by the Spitzer Space Telescope shows two low-mass stars in the rectangles that show tails in the 24 Micron filter image. This is seen as signs that Meissa is photoevaporating the disks of these low-mass stars.[19]
    This image taken by the Spitzer Space Telescope shows two low-mass stars in the rectangles that show tails in the 24 Micron filter image. This is seen as signs that Meissa is photoevaporating the disks of these low-mass stars.[29]

References

  1. ^
    S2CID 244398875
    . Gaia DR3 record for this source at VizieR.
  2. ^
    doi:10.1093/mnras/staa454
    .
  3. ^
    S2CID 244398875
    . Gaia DR3 record for this source at VizieR.
  4. S2CID 119248206
    .
  5. ^
    doi:10.1093/mnras/181.4.657
    .
  6. S2CID 119231169
    .
  7. ^
    ISSN 0004-6361
    .
  8. ^
    ISSN 0004-637X
    .
  9. ^
    S2CID 118958583
    .
  10. ^
    S2CID 53480665
    .
  11. ^
    doi:10.1046/j.1365-8711.2002.05341.x
    .
  12. Bibcode:2002yCat.2237....0D
    .
  13. ^
    ISBN 0486210790. Retrieved 2011-07-16. {{cite book}}: ISBN / Date incompatibility (help
    )
  14. ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  15. ^ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  16. ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
  17. ISBN 9789867332257
    .
  18. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 24 日 Archived 2011-07-16 at the Wayback Machine
  19. Commonwealth Scientific and Industrial Research Organisation. December 21, 2004. Archived from the original
    on March 18, 2012. Retrieved 2012-01-16.
  20. ^
    S2CID 118633609
    .
  21. Bibcode:1983A&AS...53..433S
    .
  22. doi:10.1086/300234
    .
  23. PMID 36974081
    .
  24. S2CID 20902398
    .
  25. S2CID 1595852
    .
  26. Bibcode:2005RMxAC..24..217B
    .
  27. Bibcode:1996A&A...309..892C
    .
  28. S2CID 15223974
    .
  29. S2CID 199137075
    .
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