57 Tauri, also known as h Tauri and V483 Tauri, is a star 148 light years from the Earth, in the constellation Taurus.[2] It is a 5th magnitude star, so it will be visible to the naked eye of an observer located far from city lights.[3] 57 Tauri is a member of the Hyades star cluster.[11] It is a Delta Scuti variable star, whose brightness changes slightly, ranging from magnitude 5.55 to 5.59.[3]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 04h 19m 57.70457s[2] |
| Declination | +14° 02′ 06.7322″[2] |
| Apparent magnitude (V) | 5.55 - 5.59[3] |
| Characteristics | |
| Spectral type | F0 IV[4] |
| B−V color index | 0.283[5] |
| Variable type | δ Scuti[3] |
| Astrometry | |
| Proper motion (μ) | RA: 115.369±0.078[2] mas/yr Dec.: −18.825±0.052[2] mas/yr |
| Parallax (π) | 21.9777 ± 0.0621 mas[2] |
| Distance | 148.4 ± 0.4 ly (45.5 ± 0.1 pc) |
| Absolute magnitude (MV) | 5.56[6] |
| Orbit[7] | |
| Primary | δ Scuti star |
| Period (P) | 2.4860±0.0017 d |
| Eccentricity (e) | 0.028±0.010 |
| Longitude of the node (Ω) | 140.5±20.4° |
| Periastron epoch (T) | 2451164.968±0.144 |
| Semi-amplitude (K1) (primary) | 29.906±0.316 km/s |
| Details | |
| Mass | 1.6[2] M☉ |
| Radius | 2.0[2] R☉ |
| Luminosity | 9.8[2] L☉ |
| Surface gravity (log g) | 4.00[2] cgs |
| Temperature | 7,258[2] K |
| Metallicity [Fe/H] | 0.051[8] dex |
| Rotation | 0.905 d[9] |
| Rotational velocity (v sin i) | 97.6[9] km/s |
| Age | 1.2[2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
In 1908, Lewis Boss listed 57 Tauri as a member of the Hyades cluster based upon its proper motion agreeing with the motions of other cluster members.[12] Its membership in the cluster was firmly established forty-four years later by Hendrik van Bueren, using both proper motion and radial velocity.[13] 57 Tauri is located 10.8 light years from the core of the Hyades cluster.[14]
Robert Millis discovered that 57 Tauri is a variable star, in 1967. He reported that the amplitude varied by 0.02 magnitudes with a period of 1.5 hours.[15] In 1972, it was given the variable star designation V483 Tauri.[16] A year 2000 study of 57 Tauri, based on 54 nights of photometric data, identified twelve pulsation frequencies ranging in period from 58.6 minutes to 6.17 days.[11]
In 1999, Anthony Kaye discovered that 57 Tauri is a spectroscopic binary by examining 139 high signal-to-noise spectra obtained at Kitt Peak.[7]
References
edit- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 3 February 2023.
- ^ a b c d e f g h i j k l Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
- ^ Gray, R. O.; Napier, M. G.; Winkler, L. I. (April 2001). "The Physical Basis of Luminosity Classification in the Late A-, F-, and Early G-Type Stars. I. Precise Spectral Types for 372 Stars". The Astronomical Journal. 121 (4): 2148–2158. Bibcode:2001AJ....121.2148G. doi:10.1086/319956.
- ^ Böhm-Vitense, Erika; Robinson, Richard; Carpenter, Kenneth; Mena-Werth, Jose (April 2002). "What Is Happening at Spectral Type F5 in Hyades F Stars?". The Astrophysical Journal. 569 (2): 941–963. Bibcode:2002ApJ...569..941B. doi:10.1086/339395.
- ^ Cesetti, M.; Pizzella, A.; Ivanov, V. D.; Morelli, L.; Corsini, E. M.; Dalla Bontà, E. (2013). "The Infrared Telescope Facility (IRTF) spectral library:. Spectral diagnostics for cool stars". Astronomy and Astrophysics. 549. arXiv:1211.5572. Bibcode:2013A&A...549A.129C. doi:10.1051/0004-6361/201219078. S2CID 118828206.
- ^ a b Kaye, A. B. (April 1999). "57 Tau = HD 27397 - A Spectroscopic Binary" (PDF). Information Bulletin on Variable Stars. 4697: 1. Bibcode:1999IBVS.4697....1K. Retrieved 4 February 2023.
- ^ Huber, Daniel; Bryson, Stephen T.; Haas, Michael R.; Barclay, Thomas; Barentsen, Geert; Howell, Steve B.; Sharma, Sanjib; Stello, Dennis; Thompson, Susan E. (2016). "The K2 Ecliptic Plane Input Catalog (Epic) and Stellar Classifications of 138,600 Targets in Campaigns 1–8". The Astrophysical Journal Supplement Series. 224 (1): 2. arXiv:1512.02643. Bibcode:2016ApJS..224....2H. doi:10.3847/0067-0049/224/1/2. S2CID 118621218.
- ^ a b van Saders, Jennifer L.; Pinsonneault, Marc H. (October 2013). "Fast Star, Slow Star; Old Star, Young Star: Subgiant Rotation as a Population and Stellar Physics Diagnostic". The Astrophysical Journal. 776 (2): 20. arXiv:1306.3701. Bibcode:2013ApJ...776...67V. doi:10.1088/0004-637X/776/2/67. S2CID 119097746. 67.
- ^ "h Tau -- delta Sct Variable". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2023-02-03.
- ^ a b Paparó, M.; Rodriguez, E.; McNamara, B. J.; Kolláth, Z.; Rolland, A.; Gonzalez-Bedolla, S. F.; Jiang, Shi-yang; Li, Zhi-ping (February 2000). "A comprehensive study of the delta Scuti star, 57 Tauri (= HR 1351) in the Hyades cluster". Astronomy and Astrophysics Supplement. 142: 1–11. Bibcode:2000A&AS..142....1P. doi:10.1051/aas:2000131.
- ^ Boss, Lewis J. (September 1908). "Convergent of a moving cluster in Taurus". Astronomical Journal. 26: 31–36. Bibcode:1908AJ.....26...31B. doi:10.1086/103802.
- ^ van Bueren, H. G. (May 1952). "On the structure of the Hyades cluster". Bulletin of the Astronomical Institutes of the Netherlands. 11 (432): 385–402. Bibcode:1952BAN....11..385V.
- ^ Freund, S.; Robrade, J.; Schneider, P. C.; Schmitt, J. H. M. M. (August 2020). "Updated X-ray view of the Hyades cluster". Astronomy and Astrophysics. 640: A66. arXiv:2006.05135. Bibcode:2020A&A...640A..66F. doi:10.1051/0004-6361/201937304.
- ^ Millis, Robert L. (1967). An investigation of the Delta Scuti stars (Ph.D. Thesis). University of Wisconsin.
- ^ Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P.; Perova, N. B. (September 1972). "58th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 717 (1): 1. Bibcode:1972IBVS..717....1K. Retrieved 3 February 2023.