64 Serpentis

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64 Serpentis
Observation data
Epoch J2000      Equinox J2000
Constellation Serpens
Right ascension 18h 57m 16.58980s[1]
Declination +02° 32′ 07.2512″[1]
Apparent magnitude (V) 5.56[2]
Characteristics
Spectral type B8 IIIe[3] or B8/9 II[4]
B−V color index 0.004±0.004[2]
Astrometry
Radial velocity (Rv)−9.7±3.0[2] km/s
Proper motion (μ) RA: −6.04[1] mas/yr
Dec.: −12.00[1] mas/yr
Parallax (π)2.87 ± 0.26[1] mas
Distance1,100 ± 100 ly
(350 ± 30 pc)
Absolute magnitude (MV)−2.13[2]
Details[3]
Mass4.4±1.3 M☉
Luminosity724[5] L☉
Surface gravity (log g)3.47±0.12 cgs
Temperature11,995+623
−593 K
Rotational velocity (v sin i)171±10 km/s
Age170[5] Myr
Other designations
64 Ser, BD+02° 3738, HD 175869, HIP 93051, HR 7158, SAO 124089[6]
Database references
SIMBADdata

64 Serpentis is a single,[3] blue-white hued star in Serpens Cauda, the eastern segment of the equatorial constellation of Serpens. With an apparent visual magnitude of 5.56,[2] it is a dim star but visible to the naked eye in good seeing conditions. Based upon an annual parallax shift of 2.87±0.26 mas,[1] it is located roughly 1,100 light years away. It is moving closer to the Sun with a heliocentric radial velocity of about −10 km/s.[2] It is one of the brightest stars in front of the Great Rift.

Over time this star has received a range of stellar classifications, which varied considerably in the determined luminosity class. Houk and Swift (1999) have it classified as B8/9 II,[4] Slettebak (1982) listed a class of B8 IV,[7] Cowley (1972) has B9 III(p)? (Hg),[8] while Frémat et al. (2006) gave it a classification of B8 III.[5] Despite these assignments, it is still considered to be in the main sequence phase. An overshoot of the convective core due to internal waves and rotational effects are believed to be mixing in fresh hydrogen and removing helium ashes, which is extending the duration of its stay on the main sequence.[3] It may be chemically peculiar,[8] displaying an overabundance of mercury (Hg) in its outer atmosphere.[9]

64 Serpentis was observed extensively during the CoRoT mission, which allowed highly accurate monitoring of its brightness. This revealed that the star displays low-amplitude variations with the main frequency being 1.56 days long, while it has smaller variations with other frequencies. These variations may be due to rotational modulation of spots or clouds in the photosphere, or possibly from non-radial pulsations.[10] It does not exhibit the signature of a significant magnetic field.[3]

This is a classical Be star – a rapidly rotating B-type main sequence star that has formed an orbiting gaseous disk through a mass ejection process. The circling gas is heated by the star, creating the Balmer line emission that overlays the stellar spectrum. The rapid rotation gives the star an oblate shape with a prominent equatorial bulge.[11] 64 Serpentis is about 170 million years old with roughly 4.4 times the mass of the Sun and is radiating 724 times the Sun's luminosity from its photosphere at an effective temperature of around 12,000 K.[5][3]

References[]

  1. ^ a b c d e f van Leeuwen, F. (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 e f Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  3. ^ a b c d e f Neiner, C.; et al. (March 2012), "Seismic modelling of the late Be stars HD 181231 and HD 175869 observed with CoRoT: a laboratory for mixing processes", Astronomy & Astrophysics, 539: 12, Bibcode:2012A&A...539A..90N, doi:10.1051/0004-6361/201118151, A90.
  4. ^ a b Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H.
  5. ^ a b c d Frémat, Y.; et al. (June 2006), "Fundamental parameters of Be stars located in the seismology fields of COROT", Astronomy and Astrophysics, 451 (3): 1053–1063, arXiv:astro-ph/0509336, Bibcode:2006A&A...451.1053F, doi:10.1051/0004-6361:20053305, S2CID 2652232
  6. ^ "64 Ser". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-03-22.
  7. ^ Slettebak, A. (September 1982), "Spectral types and rotational velocities of the brighter Be stars and A-F type shell stars", Astrophysical Journal Supplement Series, 50: 55–83, Bibcode:1982ApJS...50...55S, doi:10.1086/190820.
  8. ^ a b Cowley, A. (November 1972), "Spectral classification of the bright B8 stars", Astronomical Journal, 77: 750–755, Bibcode:1972AJ.....77..750C, doi:10.1086/111348.
  9. ^ Renson, P.; Manfroid, J. (May 2009), "Catalogue of Ap, HgMn and Am stars", Astronomy and Astrophysics, 498 (3): 961–966, Bibcode:2009A&A...498..961R, doi:10.1051/0004-6361/200810788
  10. ^ Gutiérrez-Soto, J.; et al. (October 2009), "Low-amplitude variations detected by CoRoT in the B8IIIe star HD 175869" (PDF), Astronomy and Astrophysics, 506 (1): 133–141, arXiv:astro-ph/0509336, Bibcode:2009A&A...506..133G, doi:10.1051/0004-6361/200911915.
  11. ^ Rivinius, Thomas; Carciofi, Alex C.; Martayan, Christophe (October 2013), "Classical Be stars. Rapidly rotating B stars with viscous Keplerian decretion disks", The Astronomy and Astrophysics Review, 21: 69, arXiv:1310.3962, Bibcode:2013A&ARv..21...69R, doi:10.1007/s00159-013-0069-0, S2CID 118652497, 69.
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