Gamma Muscae

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γ Muscae
Musca IAU.svg
Red circle.svg
Location of γ Muscae (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Musca
Right ascension 12h 32m 28.01343s[1]
Declination −72° 07′ 58.7597″[1]
Apparent magnitude (V) 3.87[2]
Characteristics
Spectral type B5 V[3]
U−B color index −0.61[2]
B−V color index −0.15[2]
Variable type SPB
Astrometry
Radial velocity (Rv)2.5±7.4[4] km/s
Proper motion (μ) RA: −51.34[1] mas/yr
Dec.: −5.40[1] mas/yr
Parallax (π)10.04 ± 0.13[1] mas
Distance325 ± 4 ly
(100 ± 1 pc)
Absolute magnitude (MV)–1.1[5]
Details
Mass5.09[6] M☉
Radius4.17[6] R☉
Luminosity790[5] L☉
Surface gravity (log g)3.87[6] cgs
Temperature15,490[6] K
Rotational velocity (v sin i)205[3] km/s
Age67.7[6] Myr
Other designations
β Vol, CD−70° 997, FK5 487, GC 17672, HD 109026, HIP 61199, HR 4773, SAO 257000
Database references
SIMBADdata

γ Muscae, Latinised as Gamma Muscae, is a blue-white hued star in the southern circumpolar constellation of Musca, the Fly. It can be seen with the naked eye, having an apparent visual magnitude of 3.87.[2] Based upon an annual parallax shift of 10.04 mas as seen from Earth, it is located about 325 light years from the Sun.

This is a B-type main-sequence star with a stellar classification of B5 V.[3] It is a variable star that ranges between magnitudes 3.84 and 3.86 over a period of 2.7 days, and is classed as a slowly pulsating B star.[7] It is around five times as massive as the Sun.[8] The star is spinning rapidly with a projected rotational velocity of 205 km/s. This is giving it an oblate shape with an equatorial bulge that is 7% larger than the polar radius.[3]

Gamma Muscae is a proper motion member of the Lower-Centaurus Crux sub-group in the Scorpius-Centaurus OB association, the nearest such association of co-moving massive stars to the Sun.[5]

References[]

  1. ^ a b c d e van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  2. ^ a b c d Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  3. ^ a b c d van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.
  4. ^ Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
  5. ^ a b c de Geus, E. J.; et al. (June 1989), "Physical parameters of stars in the Scorpio-Centaurus OB association", Astronomy and Astrophysics, 216 (1–2): 44–61, Bibcode:1989A&A...216...44D.
  6. ^ a b c d e Glagolevskij, Yu. V. (January 2019), "On Properties of Main Sequence Magnetic Stars", Astrophysical Bulletin, 74 (1): 66–79, Bibcode:2019AstBu..74...66G, doi:10.1134/S1990341319010073. Vizier-4
  7. ^ BSJ (5 March 2012). "Gamma Muscae". AAVSO Website. American Association of Variable Star Observers. Retrieved 21 December 2013.
  8. ^ Molenda-Zakowicz, J.; Połubek, G. (2004). "Empirical absolute magnitudes, luminosities and effective temperatures of SPB variables and the problem of variability classification of monoperiodic stars" (PDF). Acta Astronomica. 54: 281–97 [283]. Bibcode:2004AcA....54..281M.
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