Tau Librae
Tau Librae, Latinized from τ Librae, is the Bayer designation for a binary star system at the southern edge of the zodiac constellation of Libra. It can be seen with the naked eye, having an apparent visual magnitude of 3.68.[2] The distance to this system is around 367 light years, as determined from an annual parallax shift of 8.89 mas.[1]
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Libra |
| Right ascension | 15h 38m 39.36950s[1] |
| Declination | −29° 46′ 39.8956″[1] |
| Apparent magnitude (V) | 3.68[2] |
| Characteristics | |
| Spectral type | B2.5 V[3] |
| U−B color index | −0.717[2] |
| B−V color index | −0.179[2] |
| Astrometry | |
| Radial velocity (Rv) | +33.3±2.3[4] km/s |
| Proper motion (μ) | RA: −22.08[1] mas/yr Dec.: −24.46[1] mas/yr |
| Parallax (π) | 8.89 ± 0.20 mas[1] |
| Distance | 367 ± 8 ly (112 ± 3 pc) |
| Absolute magnitude (MV) | −1.59[5] |
| Orbit[6] | |
| Period (P) | 3.2907 d |
| Eccentricity (e) | 0.28 |
| Longitude of the node (Ω) | 114° |
| Periastron epoch (T) | 2439272.312 JD |
| Semi-amplitude (K1) (primary) | 75 km/s |
| Semi-amplitude (K2) (secondary) | 167 km/s |
| Details | |
| τ Lib A | |
| Mass | 7.25±0.49[7] M☉ |
| Radius | 3.2[8] R☉ |
| Luminosity (bolometric) | 2,705[7] L☉ |
| Surface gravity (log g) | 4.33[9] cgs |
| Temperature | 17,990[9] K |
| Metallicity [Fe/H] | +0.17[9] dex |
| Rotational velocity (v sin i) | 134[4] km/s |
| Age | 31.5±5.6[10] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Judging by its motion through space and physical properties, this system is a member of the Upper Centaurus–Lupus group of the Scorpius–Centaurus association.[4] It is double-lined[12] spectroscopic binary with an orbital period of just 3.3 days and an eccentricity of 0.28.[6] The primary, component A, is a B-type main sequence star with a stellar classification of B2.5 V.[3] It is estimated to hold more than seven[7] times the mass of the Sun and have over three[8] times the Sun's radius. It is only 31.5[10] million years old and is spinning relatively rapidly with a projected rotational velocity of 134 km/s.[4] It is a heartbeat star system, with pulsations caused by tidal forces.[13]
The system is emitting an infrared excess, suggesting the presence of a circumstellar disk of material.[9]
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 Gutierrez-Moreno, Adelina; Moreno, Hugo (June 1968), "A photometric investigation of the Scorpio-Centaurus association", Astrophysical Journal Supplement, 15: 459, Bibcode:1968ApJS...15..459G, doi:10.1086/190168.
- ^ a b Hiltner, W. A.; Garrison, R. F.; Schild, R. E. (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 c d Jilinski, E.; et al. (March 2006), "Radial velocity measurements of B stars in the Scorpius–Centaurus association", Astronomy and Astrophysics, 448 (3): 1001–1006, arXiv:astro-ph/0601643, Bibcode:2006A&A...448.1001J, doi:10.1051/0004-6361:20041614, S2CID 17818058.
- ^ 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 Pourbaix, D.; et al. (2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics, 424 (2): 727–732, arXiv:astro-ph/0406573, Bibcode:2004A&A...424..727P, doi:10.1051/0004-6361:20041213, S2CID 119387088.
- ^ a b c Hohle, M. M.; et al. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483.
- ^ a b Pasinetti-Fracassini, L. E.; et al. (February 2001), "Catalog of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics (3rd ed.), 367: 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
- ^ a b c d Saffe, C.; Gómez, M.; Pintado, O.; González, E. (October 2008), "Spectroscopic metallicities of Vega-like stars", Astronomy and Astrophysics, 490 (1): 297–305, arXiv:0805.3936, Bibcode:2008A&A...490..297S, doi:10.1051/0004-6361:200810260, S2CID 15059920.
- ^ a b Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 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.
- ^ "tau Lib". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-01-30.
{{cite web}}: CS1 maint: postscript (link) - ^ Strom, Stephen E.; et al. (February 2005), "B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?", The Astronomical Journal, 129 (2): 809–828, arXiv:astro-ph/0410337, Bibcode:2005AJ....129..809S, doi:10.1086/426748, S2CID 15059129.
- ^ Sharma, Awshesh N.; Bedding, Timothy R.; Saio, Hideyuki; White, Timothy R. (2022). "Pulsating B stars in the Scorpius–Centaurus Association with TESS". Monthly Notices of the Royal Astronomical Society. 515 (1): 828–840. arXiv:2203.02582. Bibcode:2022MNRAS.515..828S. doi:10.1093/mnras/stac1816.
External links
- Kaler, James B. (May 17, 2013), "Tau Librae", Stars, University of Illinois, retrieved 2017-02-02.