Gamma Arietis
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Aries |
Right ascension | 01h 53m 31.81479s[1] |
Declination | +19° 17′ 37.8790″[1] |
Apparent magnitude (V) | 3.86 (4.58/4.64)[2] |
Characteristics | |
Gamma1 Ari (B) | |
Spectral type | A0Vnp |
B−V color index | −0.14[4] |
Gamma2 Ari (A) | |
Spectral type | A2IVpSiSrCr[5] |
B−V color index | −0.03[4] |
Variable type | |
Astrometry | |
Radial velocity (Rv) | +3.7[7] km/s |
Proper motion ( | RA: +79.20[1] mas/yr Dec.: −97.63[1] mas/yr |
Parallax ( | 19.88 ± 0.96 mas[1] |
Distance | 164 ± 8 ly (50 ± 2 pc) |
Details | |
Gamma1 Ari (Ba) | |
Mass | 2.67[8] M☉ |
Radius | 2.014 R☉ |
Luminosity | 42.0 L☉ |
Surface gravity (log g) | 4.26[8] cgs |
Temperature | 10,356[8] K |
Rotational velocity (v sin i) | 54[9] km/s |
Age | 34[10] Myr |
Gamma2 Ari (A) | |
Mass | 2.72[8] M☉ |
Radius | 1.941[8] R☉ |
Luminosity | 41.5 L☉ |
Surface gravity (log g) | 4.30[8] cgs |
Temperature | 10,512[8] K |
Metallicity [Fe/H] | 0.43±0.14[11] dex |
Rotational velocity (v sin i) | 201[9] km/s |
Gamma1 Ari (Bb) | |
Mass | 0.7[10] M☉ |
Temperature | 4,312[10] K |
Metallicity [Fe/H] | −0.5[10] dex |
Rotational velocity (v sin i) | 5[10] km/s |
Other designations | |
Gamma1 Ari (B): HD 11502, HR 545, SAO 92680, WDS J01535+1918B. | |
Gamma2 Ari (A): HD 11503, HR 546, SAO 92681, WDS J01535+1918A | |
Database references | |
SIMBAD | |
Gamma Arietis (
The combined apparent visual magnitude of the stars is 3.86,[2] which is readily visible to the naked eye and makes this the fourth-brightest member of Aries. Based upon parallax measurements obtained during the Hipparcos mission,[1] the distance to Gamma Arietis from the Sun is approximately 164 light-years (50 parsecs).
Properties[edit]
The double star nature of this system was discovered by Robert Hooke in 1664.[13] The two components have an angular separation of 7.606 arcseconds,[2] which can be resolved with a small telescope. The orbital period of the pair is greater than 5000 years.[14]
The brighter component,
The marginally fainter of the two visible stars,
Both of the visible stars have mass of about 2.7 M☉, luminosities of about 40 L☉, effective temperatures of about 10,000 K, and radii of about 2 R☉. Their age is about 34 million years.
Nomenclature[edit]
Gamma Arietis has been called "the First Star in Aries" as having been at one time the nearest visible star to the equinoctial point.
It bore the traditional name Mesarthim. Originally it had shared the name Sheratan with Beta Arietis. However, this got corrupted to "Sartai" in medieval manuscripts, which Bayer erroneously explained as being the Hebrew grammatical term מְשָׁרְתִים mᵉshārᵉthīm "servants", and later scholars picked up on this term.[21]
In 2016, the I
In Chinese, 婁宿 (Lóusù), meaning Bond (asterism), refers to an asterism consisting of Gamma, Beta and Alpha Arietis.[25] Consequently, the Chinese name for Gamma Arietis itself is 婁宿
In Hindu astrology, Gamma Arietis and Beta Arietis (Sheratan) are Ashvins, the twin Rigvedic deities who act as doctors of the divine of the world.(Richard H Allen)
References[edit]
- ^ a b c d e f van Leeuwen, F. (November 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 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ a b Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", The Astrophysical Journal Supplement Series, 99: 135–172, Bibcode:1995ApJS...99..135A, doi:10.1086/192182.
- ^ a b c d Murphy, Simon J.; et al. (October 2015), "An Evaluation of the Membership Probability of 212
λ Boo Stars. I. A Catalogue", Publications of the Astronomical Society of Australia, 32: 43, arXiv:1508.03633, Bibcode:2015PASA...32...36M, doi:10.1017/pasa.2015.34, S2CID 59405545, e036. - ^ Abt, H. A.; Cardona, O. (January 1, 1984), "The nature of the visual companions of Ap and Am stars", Astrophysical Journal, Part 1, 276: 266–269, Bibcode:1984ApJ...276..266A, doi:10.1086/161610.
- ^ a b Samus', N. N; et al. (2017), "General catalogue of variable stars", Astronomy Reports, GCVS 5.1, 61 (1): 80, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
- ^ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
- ^ a b c d e f g 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.
- ^ a b Royer, F.; et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics, 393: 897–911, arXiv:astro-ph/0205255, Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943, S2CID 14070763.
- ^ a b c d e f Gullikson, Kevin; et al. (August 2016), "The Close Companion Mass-ratio Distribution of Intermediate-mass Stars", The Astronomical Journal, 152 (2): 13, arXiv:1604.06456, Bibcode:2016AJ....152...40G, doi:10.3847/0004-6256/152/2/40, S2CID 119179065, 40.
- ^ Wu, Yue; et al. (January 2011), "Coudé-feed stellar spectral library - atmospheric parameters", Astronomy and Astrophysics, 525: A71, arXiv:1009.1491, Bibcode:2011A&A...525A..71W, doi:10.1051/0004-6361/201015014, S2CID 53480665.
- ^ "gam Ari", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2012-08-04.
- ^ Aitken, Robert G. (1935), The Binary Stars, New York: McGraw-Hill, p. 1.
- ^ Kaler, James B., "Mesarthim", Stars, University of Illinois, retrieved 2012-08-04.
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ "gam Ari". The International Variable Star Index. AAVSO. Retrieved 3 July 2022.
- ^ Renson, P.; Manfroid, J. (May 2009), "Catalogue of Ap, HgMn and Am stars", Astronomy and Astrophysics, 498 (3): 961–966, Bibcode:2009A&A...498..961R, doi:10.1051/0004-6361/200810788.
- ^ a b Skiff, B. A. (2014), "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)", VizieR On-line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014), 1, Bibcode:2014yCat....1.2023S.
- ^ Gerbaldi, M.; Faraggiana, R.; Lai, O. (December 2003), "The heterogeneous class of lambda Bootis stars", Astronomy and Astrophysics, 412 (2): 447–464, Bibcode:2003A&A...412..447G, doi:10.1051/0004-6361:20031472.
- ^ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010), On the naming convention used for multiple star systems and extrasolar planets, arXiv:1012.0707.
- ^ Kunitzsch, Paul; Smart, Tim (2006), A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.), Cambridge, Massachusetts: Sky Pub, ISBN 978-1-931559-44-7.
- ^ IAU Working Group on Star Names (WGSN), International Astronomical Union, retrieved 22 May 2016.
- ^ WG Triennial Report (2015-2018) - Star Names (PDF), p. 5, retrieved 2018-07-14.
- ^ IAU Catalog of Star Names, retrieved 28 July 2016.
- ^ (in Chinese)
中國 星座 神話 , written by陳 久金 . Published by台灣 書房 出版 有限 公司 , 2005, ISBN 978-986-7332-25-7. - ^ (in Chinese)
香港 太 空 館 -研究 資源 -亮 星 中 英 對照 表 Archived January 30, 2011, at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.