| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Columba |
| Right ascension | 05h 57m 32.20958s[1] |
| Declination | −35° 16′ 59.8153″[1] |
| Apparent magnitude (V) | 4.366 + 12.664[2] |
| Characteristics | |
| Spectral type | B2.5 IV[3] + G8 V[4] |
| U−B color index | −0.66[5] |
| B−V color index | −0.18[5] |
| Variable type | Candidate SPB[6] |
| Astrometry | |
| Radial velocity (Rv) | +24.2[7] km/s |
| Proper motion (μ) | RA: −3.24[1] mas/yr Dec.: +10.21[1] mas/yr |
| Parallax (π) | 3.75 ± 0.18 mas[1] |
| Distance | 870 ± 40 ly (270 ± 10 pc) |
| Absolute magnitude (MV) | −2.76[8] |
| Details[6] | |
| γ Col A | |
| Mass | 5.7±0.3 M☉ |
| Radius | 4.8±0.4 R☉ |
| Luminosity | 2,070[9] L☉ |
| Surface gravity (log g) | 3.328±0.100[10] cgs |
| Temperature | 15570±320[10] K |
| Rotational velocity (v sin i) | 96±16 km/s |
| Age | 23.6±2.0[11] Myr |
| γ Col B | |
| Mass | 0.94[2] M☉ |
| Temperature | 5,367[2] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
Gamma Columbae, Latinized from γ Columbae, is a possible wide binary star system[2] in the southern constellation of Columba. It is visible to the naked eye with an apparent visual magnitude of 4.36.[5] Based upon an annual parallax shift of 3.75 mas,[1] it is located roughly 870 light years from the Sun.
The primary component is an evolved[6] B-type subgiant star with a stellar classification of B2.5 IV.[3] It is a candidate slowly pulsating B-type star with a mean longitudinal magnetic field strength of 94±28 G.[6] The star has nearly six times the mass of the Sun and close to five times the Sun's girth.[6] It is radiating over 2,000 times the solar luminosity from its outer atmosphere at an effective temperature of 12,904 K.[9] The estimated age of this star is around 24 million years.[11] At this age, it is thought to be the remnant of a once more massive star that just finished hydrogen fusion, and is undergoing structural readjustment. This process is extremely short, on the order of ten thousand years, making it a rare object.[10]
The visual magnitude 12.664[2] companion is a G-type main sequence star with a classification of G8 V.[4] It lies at an angular separation of 33.8 arc seconds from the primary, which corresponds to a projected physical separation of 8,844 AU.[2] Despite the young age of these stars, there has been no X-ray emission detected.[2]
References
- ^ 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.
- ^ a b c d e f g Gerbaldi, M.; et al. (November 2001), "Binary systems with post-T Tauri secondaries", Astronomy and Astrophysics, 379: 162–184, Bibcode:2001A&A...379..162G, doi:10.1051/0004-6361:20011298.
- ^ a b Hiltner, W. A.; et al. (July 1969), "MK Spectral Types for Bright Southern OB Stars", Astrophysical Journal, 157: 313–326, Bibcode:1969ApJ...157..313H, doi:10.1086/150069.
- ^ a b Huélamo, N.; et al. (July 2000), "X-ray emission from Lindroos binary systems", Astronomy and Astrophysics, 359: 227–241, arXiv:astro-ph/0005348, Bibcode:2000A&A...359..227H.
- ^ a b c Johnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1999), "UBVRIJKL photometry of the bright stars", Commission Lunar and Planetary Laboratory, 4: 99, Bibcode:1966CoLPL...4...99J.
- ^ a b c d e Hubrig, S.; et al. (April 2009), "New magnetic field measurements of β Cephei stars and slowly pulsating B stars", Astronomische Nachrichten, 330 (4): 317, arXiv:0902.1314, Bibcode:2009AN....330..317H, doi:10.1002/asna.200811187, S2CID 17497112.
- ^ Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Carnegie Institution for Science, Bibcode:1953GCRV..C......0W, LCCN 54001336.
- ^ 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.
- ^ a b McDonald, I.; et al. (2012). "Fundamental Parameters and Infrared Excesses of Hipparcos Stars". Monthly Notices of the Royal Astronomical Society. 427 (1): 343–57. arXiv:1208.2037. Bibcode:2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x. S2CID 118665352.
- ^ a b c Irrgang, Andreas; Przybilla, Norbert; Meynet, Georges (2022). "γ Columbae as a recently stripped pulsating core of a massive star". Nature Astronomy. 6 (12): 1414–1420. arXiv:2211.00358. Bibcode:2022NatAs...6.1414I. doi:10.1038/s41550-022-01809-6. S2CID 253244604.
- ^ a b Tetzlaff, N.; et al. (2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
- ^ "gam Col -- Variable Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2016-12-19.
External links
- Kaler, James B. (January 29, 2016), "Gamma Columbae", STARS, University of Illinois, retrieved 2016-12-21.
This page was last edited on 15 August 2023, at 05:54