Astronomy:HD 113703
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h 06m 16.70s[1] |
| Declination | −48° 27′ 47.8″[1] |
| Apparent magnitude (V) | +4.71[2] |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | B4V[3] + K0Ve[4] |
| U−B color index | −0.562[2] |
| B−V color index | −0.148±0.006[2] |
| Astrometry | |
| Radial velocity (Rv) | +6.0±4.2[5] km/s |
| Proper motion (μ) | RA: −29.558[1] mas/yr Dec.: −15.692[1] mas/yr |
| Parallax (π) | 8.1592 ± 0.1559[1] mas |
| Distance | 400 ± 8 ly (123 ± 2 pc) |
| Absolute magnitude (MV) | −0.68[2] |
| Details | |
| f Cen Aa | |
| Mass | 4.39[6] M☉ |
| Surface gravity (log g) | 3.99[6] cgs |
| Temperature | 14,769[6] K |
| Rotational velocity (v sin i) | 140±7[7] km/s |
| Age | 92[6] Myr |
| f Cen C | |
| Mass | 0.9[8] M☉ |
| Luminosity | 0.49[8] L☉ |
| Temperature | 5,020[8] K |
| Age | 50[8] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 113703, also known by the Bayer designation f Centauri, is a multiple star[9] system in the southern constellation of Centaurus. The combined apparent visual magnitude of this system is +4.71,[2] which is sufficient to make it faintly visible to the naked eye. The distance to this system is approximately 400 light years based on parallax measurements. It is a member of the Lower Centaurus Crux subgroup of the Scorpius–Centaurus association.[6]
The primary of f Centauri is a blue-white hued B-type main-sequence star with a stellar classification of B4V.[3] It is a young star with an age estimated at around 92 million years,[6] and is spinning rapidly with a projected rotational velocity of 140 km/s.[7] A close companion with a K magnitude of 9.16, designated component C, was detected in 2002 at an angular separation of 1.55″.[10] In 2013, a spectroscopic companion to the primary was observed using long baseline interferometry, with the two being designated components Aa and Ab.[11]
A faint, magnitude 10.8 companion, component B, was first reported by J. F. W. Herschel in 1836. As of 2015, it was located at a separation of 11.6″ along a position angle of 78°.[12] This is a K-type star with a class of K0Ve, showing emission in the Calcium H and K lines. It is a known BY Draconis variable star with the designation V1155 Centauri.[13] It shares a common space motion with the primary, indicating a probable physical relationship, and its Gaia Data Release 3 parallax of 7.965″±0.018″ suggests a distance of 409 light years.[14] The star shows a strong overabundance in lithium, which demonstrates its young age.[4] It is about 0.8 magnitudes above zero age main sequence and thus is still contracting as a post-T Tauri star.[15] X-ray emission has been detected from this star.[8]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 Houk, Nancy (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. 2. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode: 1978mcts.book.....H.
- ↑ 4.0 4.1 Catchpole, R. M. (1971). "A lithium rich star in Sco-Cen". Monthly Notices of the Royal Astronomical Society 154: 15. doi:10.1093/mnras/154.1.15P. Bibcode: 1971MNRAS.154P..15C.
- ↑ Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Goldman, Bertrand et al. (November 2018). "A Large Moving Group within the Lower Centaurus Crux Association". The Astrophysical Journal 868 (1): 15. doi:10.3847/1538-4357/aae64c. 32. Bibcode: 2018ApJ...868...32G.
- ↑ 7.0 7.1 Brown, A. G. A.; Verschueren, W. (March 1997). "High S/N Echelle spectroscopy in young stellar groups. II. Rotational velocities of early-type stars in SCO OB2". Astronomy and Astrophysics 319: 811–838. Bibcode: 1997A&A...319..811B.
- ↑ 8.0 8.1 8.2 8.3 8.4 Stelzer, B. et al. (September 2003). "Late B-type stars and their candidate companions resolved with Chandra". Astronomy and Astrophysics 407 (3): 1067–1078. doi:10.1051/0004-6361:20030934. Bibcode: 2003A&A...407.1067S.
- ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869–879. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E.
- ↑ Shatsky, N.; Tokovinin, A. (January 2002). "The mass ratio distribution of B-type visual binaries in the Sco OB2 association". Astronomy and Astrophysics 382: 92–103. doi:10.1051/0004-6361:20011542. Bibcode: 2002A&A...382...92S.
- ↑ Rizzuto, A. C. et al. (December 2013). "Long-baseline interferometric multiplicity survey of the Sco-Cen OB association". Monthly Notices of the Royal Astronomical Society 436 (2): 1694–1707. doi:10.1093/mnras/stt1690. Bibcode: 2013MNRAS.436.1694R.
- ↑ Mason, B. D. et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal 122 (6): 3466. doi:10.1086/323920. Bibcode: 2001AJ....122.3466M.
- ↑ Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1: B/gcvs. Bibcode: 2009yCat....102025S.
- ↑ Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ Andrews, P. J.; Thackeray, A. D. (1973). "Absolute magnitudes of B-type primaries in visual binaries.". Monthly Notices of the Royal Astronomical Society 165: 1–9. doi:10.1093/mnras/165.1.1. Bibcode: 1973MNRAS.165....1A.
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