H Centauri

A light curve for V945 Centauri, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Centaurus
Right ascension 12h 57m 04.35244s[2]
Declination −51° 11′ 55.5058″[2]
Apparent magnitude (V) 5.163[2]
Characteristics
Spectral type B7V + B8.5V + B[3]
Apparent magnitude (B) 5.102
Apparent magnitude (V) 5.163
Variable type ellipsoidal variable[3]
Astrometry
Radial velocity (Rv)14.55 ± 1.6[3] km/s
Proper motion (μ) RA: −30.15 mas/yr
Dec.: −14.61 mas/yr
Parallax (π)8.85 ± 0.27 mas
Distance370 ± 10 ly
(113 ± 3 pc)
Details[3]
Primary
Mass3.32 ± 0.51 M☉
Radius2.09 ± 0.12 R☉
Luminosity111 ± 21 L☉
Surface gravity (log g)4.3 ± 0.1 cgs
Temperature13000 K
Secondary
Mass2.37 ± 0.48 M☉
Radius1.67 ± 0.09 R☉
Luminosity37 ± 7 L☉
Surface gravity (log g)4.4 ± 0.1 cgs
Temperature10687 ± 52 K
Other designations
H Centauri, V945 Centauri, CD−50 7394, CPD−50 5596, CPC 0 10830, GC 17569, GCRV 7736, GSC 08258-01469, HD 112409, HIC 63210, HIP 63210, HR 4913, PPM 341451, SAO 240407
Database references
SIMBADdata

H Centauri (H Cen), also known as V945 Centauri, is probable triple star system[3] located in the constellation Centaurus. From parallax measurements, it is located 113 parsecs (370 light years) from the Sun. It is a member of the Lower Centaurus–Crux (LCC) subgroup of the Scorpius–Centaurus association.[4]

This system is a double-lined spectroscopic binary formed by two B-type main-sequence star with spectral types B7V and B8.5V. They are in a close (but detached) circular orbit with a period of 0.6496 days and a separation of 5.63 solar radii. Observed at an inclination of 24°, the system is an ellipsoidal variable whose apparent visual magnitude varies from 5.14 to 5.17 over the course of an orbit as the star's visible surface area changes. The system's spectrum contains a third set of spectral lines that are probably from a third star, also of type B.[3]

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. 1 2 3
  3. 1 2 3 4 5 6 Harmanec, P.; Aerts, C.; Prša, A.; Verhoelst, T.; Kolenberg, K. (September 2010). "V945 Centauri = HD 112409: a bright hot short-period binary in a triple system?" (PDF). Astronomy and Astrophysics. 520: A73, 11 pp. Bibcode:2010A&A...520A..73H. doi:10.1051/0004-6361/201014096.
  4. ↑ Chen, Christine H.; Pecaut, Mark; Mamajek, Eric E.; Su, Kate Y. L.; Bitner, Martin (September 2012). "A Spitzer MIPS Study of 2.5-2.0 M ⊙ Stars in Scorpius–Centaurus". The Astrophysical Journal. 756 (2): article 133, 24 pp. arXiv:1207.3415. Bibcode:2012ApJ...756..133C. doi:10.1088/0004-637X/756/2/133. S2CID 119278056.
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