HD 36960
 
| |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Orion |
| Right ascension | 5h 35m 02.68074s[1] |
| Declination | −06° 00′ 07.3036″[1] |
| Apparent magnitude (V) | 4.72[2] |
| Characteristics | |
| Spectral type | B0.5 V[3] |
| U−B color index | −0.98[2] |
| B−V color index | −0.22[2] |
| Astrometry | |
| Radial velocity (Rv) | +27.7 km/s |
| Proper motion (μ) | RA: −0.66[1] mas/yr Dec.: +0.01[1] mas/yr |
| Parallax (π) | 2.02 ± 0.31[1] mas |
| Distance | approx. 1,600 ly (approx. 500 pc) |
| Absolute magnitude (MV) | −3.18[4] |
| Details | |
| Mass | 15.66[3] M☉ |
| Radius | 5.6[4] R☉ |
| Luminosity | 19,952[4] L☉ |
| Surface gravity (log g) | 4.10[4] cgs |
| Temperature | 29,000[4] K |
| Metallicity [Fe/H] | −0.20[5] dex |
| Rotational velocity (v sin i) | 28[4] km/s |
| Age | 6[4] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 36960 (HR 1887) is a B-type main-sequence star in the constellation Orion. At an apparent magnitude of +4.78 it is easily visible to the naked eye in many areas, though in most urban areas it cannot be seen due to light pollution. Although it does not have a Bayer or Flamsteed designation, it is brighter than over 30 Flamsteed stars in Orion]], as well as being brighter than any of the stars in the nearby Orion Nebula such as θ1 Orionis C and θ2 Orionis.
HD 36960 forms a close pair with the slightly fainter HD 36959 36" away. Multiple star catalogues also list the 9th magnitude BD-06°1233 as part of the system. HD 36959 is itself a very close binary with a 9th magnitude companion.[6] All these stars are likely members of open cluster NGC 1980 which includes ι Orionis 7' away.
At over 15 solar masses, it shines with around 20,000 times the Sun's luminosity due to its high surface temperature of 29,000 K and radius over five times that of the sun. It is calculated to be around six million years old, consistent with other stars thought to be members of NGC 1980.
References
- 1 2 3 4 5 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
- 1 2 3 Reed, B. Cameron (2003). "Catalog of Galactic OB Stars". The Astronomical Journal. 125 (5): 2531. Bibcode:2003AJ....125.2531R. doi:10.1086/374771.
- 1 2 Hohle, M. M.; Neuhäuser, R.; Schutz, B. F. (2010). "Masses and luminosities of O- and B-type stars and red supergiants". Astronomische Nachrichten. 331 (4): 349. Bibcode:2010AN....331..349H. arXiv:1003.2335
. doi:10.1002/asna.200911355. - 1 2 3 4 5 6 7 Nieva, María-Fernanda; Przybilla, Norbert (2014). "Fundamental properties of nearby single early B-type stars". Astronomy & Astrophysics. 566: A7. Bibcode:2014A&A...566A...7N. arXiv:1412.1418 . doi:10.1051/0004-6361/201423373.
- ↑ Nieva, M.-F.; Przybilla, N. (2012). "Present-day cosmic abundances. A comprehensive study of nearby early B-type stars and implications for stellar and Galactic evolution and interstellar dust models". Astronomy & Astrophysics. 539: A143. Bibcode:2012A&A...539A.143N. doi:10.1051/0004-6361/201118158.
- ↑ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.