Astronomy:19 Lyrae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Lyra |
| Right ascension | 19h 11m 46.008s[2] |
| Declination | +31° 17′ 00.44″[2] |
| Apparent magnitude (V) | 5.93[3] |
| Characteristics | |
| Spectral type | B8 IIIp Si Sr[4] |
| B−V color index | −0.062±0.004[3] |
| Variable type | α2 CVn[5] |
| Astrometry | |
| Radial velocity (Rv) | −30.1±2.9[3] km/s |
| Proper motion (μ) | RA: −4.143[2] mas/yr Dec.: −2.763[2] mas/yr |
| Parallax (π) | 3.4213 ± 0.0417[2] mas |
| Distance | 950 ± 10 ly (292 ± 4 pc) |
| Absolute magnitude (MV) | −1.24[3] |
| Details | |
| Mass | 3.76±0.22[6] M☉ |
| Radius | 6.40[7] R☉ |
| Luminosity | 397.48[3] L☉ |
| Temperature | 11,194+501 −479[6] K |
| Rotational velocity (v sin i) | 35[8] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
19 Lyrae is a single[10] variable star located approximately 950[2] light years away from the Sun in the northern constellation of Lyra.[9] It has the variable star designation V471 Lyr, while 19 Lyrae is the Flamsteed designation. This object is just bright enough to be visible to the naked eye, appearing as a dim, blue-white star with a baseline apparent visual magnitude of 5.93.[3] It is moving closer to the Earth with a heliocentric radial velocity of −30 km/s, and may come as close as 167 light-years around 8.5 million years from now.[3]
This is a magnetic chemically-peculiar star[11] with a stellar classification of B8 IIIp Si Sr,[4] showing abundance anomalies in silicon and strontium. The light variations of this star were discovered by J. E. Winzer in 1974.[12] It is an Alpha2 Canum Venaticorum-type variable with a period of 1.160898 days (or 7.0980 days[12]), ranging in magnitude from a high of 5.91 down to 5.98.[5] The surface magnetic field has a strength of (111.3±56.9)×10−4 T[13]
19 Lyrae has a moderate rotation rate, showing a projected rotational velocity of 35 km/s.[8] Stellar models give it an estimated 3.8[6] times the mass of the Sun and its girth is measured at 6.4[7] times the Sun's radius. It is radiating 397[3] times the luminosity of the Sun from its photosphere at an effective temperature of around 11,194 K.[6] The star has an absolute magnitude of −1.24,[3] which shows how bright the star would appear if it were located at a distance of 10 parsecs (33 ly) from the Sun.
References
- ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html, retrieved 8 December 2021.
- ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 3.8 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 4.0 4.1 Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement 99: 135, doi:10.1086/192182, Bibcode: 1995ApJS...99..135A
- ↑ 5.0 5.1 Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1 61 (1): 80–88, doi:10.1134/s1063772917010085, Bibcode: 2017ARep...61...80S.
- ↑ 6.0 6.1 6.2 6.3 Netopil, Martin et al. (July 2017), "An Investigation of the Rotational Properties of Magnetic Chemically Peculiar Stars", Monthly Notices of the Royal Astronomical Society 468 (3): 2745–2756, doi:10.1093/mnras/stx674, Bibcode: 2017MNRAS.468.2745N.
- ↑ 7.0 7.1 Shulyak, D. et al. (2014), "Interferometry of chemically peculiar stars: Theoretical predictions versus modern observing facilities", Monthly Notices of the Royal Astronomical Society 443 (2): 1629, doi:10.1093/mnras/stu1259, Bibcode: 2014MNRAS.443.1629S.
- ↑ 8.0 8.1 Abt, Helmut A. et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal 573 (1): 359–365, doi:10.1086/340590, Bibcode: 2002ApJ...573..359A
- ↑ 9.0 9.1 "19 Lyr". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=19+Lyr.
- ↑ Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ Kochukhov, O.; Bagnulo, S. (2006), "Evolutionary state of magnetic chemically peculiar stars", Astronomy and Astrophysics 450 (2): 763, doi:10.1051/0004-6361:20054596, Bibcode: 2006A&A...450..763K
- ↑ 12.0 12.1 Adelman, S. J.; Rice, R. H. (April 1999), "UVBY photometry of the mCP stars HD 35298, 19 Lyrae, HD 192678, and HR 8216", Astronomy and Astrophysics Supplement 136: 111–115, doi:10.1051/aas:1999202, Bibcode: 1999A&AS..136..111A.
- ↑ Bychkov, V. D. et al. (2009), "Catalogue of averaged stellar effective magnetic fields - II. Re-discussion of chemically peculiar A and B stars", Monthly Notices of the Royal Astronomical Society 394 (3): 1338, doi:10.1111/j.1365-2966.2008.14227.x, Bibcode: 2009MNRAS.394.1338B.
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