BPM 37093

BPM 37093

A light curve for V886 Centauri, adapted from Kanaan et al. (1992)[1]
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Centaurus
Right ascension 12h 38m 49.78112s[2]
Declination −49° 48′ 00.2195″[2]
Apparent magnitude (V) 14.0[3]
Characteristics
Spectral type DAV4.4[4]
Variable type DAV (ZZ Ceti)[4]
Astrometry
Radial velocity (Rv)−12[4] km/s
Proper motion (μ) RA: -557.111 mas/yr[2]
Dec.: -74.036 mas/yr[2]
Parallax (π)67.4058 ± 0.0186 mas[2]
Distance48.39 ± 0.01 ly
(14.836 ± 0.004 pc)
Details
Mass1.10[5] M☉
Radius0.0057 R☉
Luminosity0.001[6] L☉
Surface gravity (log g)8.81 ± 0.05[7] cgs
Temperature11730 ± 350[7] K
Other designations
V886 Cen, BPM 37093, GJ 2095, LFT 931, LHS 2594, LTT 4816, WD 1236-495[3]
Database references
SIMBADdata
ARICNSdata

BPM 37093 (V886 Centauri) is a variable white dwarf star of the DAV, or ZZ Ceti, type, with a hydrogen atmosphere and an unusually high mass of approximately 1.1 times the Sun's. It is 48 light-years (15 parsecs) from Earth in the constellation Centaurus and vibrates; these pulsations cause its luminosity to vary.[3][5] Like other white dwarfs, BPM 37093 is thought to be composed primarily of carbon and oxygen, which are created by thermonuclear fusion of helium nuclei in the triple-alpha process.[8]

  1. ^ Cite error: The named reference Kanaan was invoked but never defined (see the help page).
  2. ^ a b c d Cite error: The named reference GaiaDR3 was invoked but never defined (see the help page).
  3. ^ a b c Cite error: The named reference simbad was invoked but never defined (see the help page).
  4. ^ a b c A Catalog of Spectroscopically Identified White Dwarfs Archived 2018-08-08 at the Wayback Machine, George P. McCook and Edward M. Sion, Astrophysical Journal Supplement 121, #1 (March 1999), pp. 1–130. CDS ID III/210 Archived 2013-10-22 at the Wayback Machine.
  5. ^ a b Cite error: The named reference arxiv04 was invoked but never defined (see the help page).
  6. ^ Cite error: The named reference bergeron was invoked but never defined (see the help page).
  7. ^ a b Cite error: The named reference Brassard was invoked but never defined (see the help page).
  8. ^ Late stages of evolution for low-mass stars Archived 2020-06-11 at the Wayback Machine, Michael Richmond, lecture notes, Physics 230, Rochester Institute of Technology, accessed online May 3, 2007.