Y Tauri is a carbon star located in the constellation Taurus. Parallax measurements by Gaia put it at a distance of approximately 2,170 light-years (670 parsecs).[1]
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| Right ascension | 05h 45m 39.4101s[1] |
| Declination | +20° 41′ 42.149″[1] |
| Apparent magnitude (V) | 6.5 - 9.2[2] |
| Characteristics | |
| Evolutionary stage | AGB[3][4] |
| Spectral type | C6.5,4e(N3)[2] |
| Variable type | SRb[2] |
| Astrometry | |
| Radial velocity (Rv) | 17.00[5] km/s |
| Proper motion (μ) | RA: 0.039[1] mas/yr Dec.: −4.532[1] mas/yr |
| Parallax (π) | 1.5006 ± 0.0592 mas[1] |
| Distance | 2,170 ± 90 ly (670 ± 30 pc) |
| Absolute magnitude (MV) | −1.1 (near max.)[6] |
| Details | |
| Mass | 4.3[7] M☉ |
| Radius | 219[8] R☉ |
| Luminosity | 6,025[4] L☉ |
| Surface gravity (log g) | 0.228[7] cgs |
| Temperature | 3,217[9] K |
| Metallicity [Fe/H] | −0.106[7] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
Y Tauri is a semiregular variable star. Its class is SRb, and its primary pulsation cycle lasts 241.5 days.[2] No long secondary period has been identified.[11] It has a radius of 219 R☉, an effective surface temperature of 3,217 K, and a bolometric luminosity of 4,489 L☉. Its mass is calculated to be 4.3 M☉.
Y Tauri is losing mass at 4×10−7 M☉/yr, and is surrounded by dust at a temperature of 1,900 K.[3]
References
edit- ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
- ^ a b c d Samus, N. N.; Durlevich, O. V.; 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. Bibcode:2009yCat....102025S.
- ^ a b Van De Sande, M.; Walsh, C.; Millar, T. J. (2021). "Chemical modelling of dust-gas chemistry within AGB outflows - III. Photoprocessing of the ice and return to the ISM". Monthly Notices of the Royal Astronomical Society. 501 (1): 491. arXiv:2011.11563. Bibcode:2021MNRAS.501..491V. doi:10.1093/mnras/staa3689.
- ^ a b Guandalini, R; Cristallo, S (2013). "Luminosities of carbon-rich asymptotic giant branch stars in the Milky Way". Astronomy & Astrophysics. 555: A120. arXiv:1305.4203. Bibcode:2013A&A...555A.120G. doi:10.1051/0004-6361/201321225. S2CID 54918450.
- ^ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
- ^ Gontcharov, G. A. (October 2011). "The red giant branch in the Tycho-2 catalogue". Astronomy Letters. 37 (10): 707–717. arXiv:1607.00557. Bibcode:2011AstL...37..707G. doi:10.1134/S1063773711090040. ISSN 1063-7737. S2CID 119272127.
- ^ a b c Anders, F.; et al. (1 August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy and Astrophysics. 628: A94. arXiv:1904.11302. Bibcode:2019A&A...628A..94A. doi:10.1051/0004-6361/201935765. ISSN 0004-6361. S2CID 131780028.
- ^ Stassun, Keivan G.; et al. (2019-10-01). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. hdl:1721.1/124721. ISSN 0004-6256. S2CID 166227927.
- ^ Chandler, Colin Orion; McDonald, Iain; Kane, Stephen R. (2016). "The Catalog of Earth-Like Exoplanet Survey Targets (CELESTA): A Database of Habitable Zones Around Nearby Stars". The Astronomical Journal. 151 (3): 59. arXiv:1510.05666. Bibcode:2016AJ....151...59C. doi:10.3847/0004-6256/151/3/59. S2CID 119246448.
- ^ "ASAS All Star Catalogue". The All Sky Automated Survey. Retrieved 8 December 2021.
- ^ Olivier, E. A.; Wood, P. R. (2003). "On the Origin of Long Secondary Periods in Semiregular Variables". The Astrophysical Journal. 584 (2): 1035–1041. Bibcode:2003ApJ...584.1035O. doi:10.1086/345715. S2CID 40373007.