| 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 mas[1] |
| Distance | 1,100 ± 100 ly (350 ± 30 pc) |
| Absolute magnitude (MV) | −2.13[2] |
| Details[3] | |
| Mass | 4.4±1.3 M☉ |
| Luminosity | 724[5] L☉ |
| Surface gravity (log g) | 3.47±0.12 cgs |
| Temperature | 11,995+623 −593 K |
| Rotational velocity (v sin i) | 171±10 km/s |
| Age | 170[5] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
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]
vanLeeuwen2007 was invoked but never defined (see the help page).Anderson2012 was invoked but never defined (see the help page).Neiner2012 was invoked but never defined (see the help page).Houk1999 was invoked but never defined (see the help page).Fremat2006 was invoked but never defined (see the help page).SIMBAD was invoked but never defined (see the help page).Slettebak1982 was invoked but never defined (see the help page).Cowley1972 was invoked but never defined (see the help page).Renson2009 was invoked but never defined (see the help page).Soto2009 was invoked but never defined (see the help page).Rivinius2013 was invoked but never defined (see the help page).