Beta Canis Majoris
| |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Canis Major |
| Right ascension | 06h 22m 41.98535s[1] |
| Declination | −17° 57′ 21.3073″[1] |
| Apparent magnitude (V) | 1.985[2] (1.97 - 2.01[3]) |
| Characteristics | |
| Spectral type | B1 II-III[4] |
| U−B color index | −0.99[2] |
| B−V color index | −0.235[2] |
| Variable type | β Cep[5] |
| Astrometry | |
| Radial velocity (Rv) | +33.7[6] km/s |
| Proper motion (μ) | RA: −3.23[1] mas/yr Dec.: −0.78[1] mas/yr |
| Parallax (π) | 6.62 ± 0.22[1] mas |
| Distance | 490 ± 20 ly (151 ± 5 pc) |
| Absolute magnitude (MV) | −4.1[7] |
| Details | |
| Mass | 13.5 ± 0.5[8] M☉ |
| Radius | 9.7 ± 1.3[9] R☉ |
| Luminosity | 26600[9] L☉ |
| Surface gravity (log g) | 3.79 ± 0.20[9] cgs |
| Temperature | 23,150[10] K |
| Metallicity [Fe/H] | 0.04 ± 0.10[8] dex |
| Rotational velocity (v sin i) | 31 ± 5[8] km/s |
| Age | 12.4 ± 0.7[8] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Beta Canis Majoris (β Canis Majoris, abbreviated Beta CMa, β CMa), also named Mirzam,[13] is a star in the southern constellation of Canis Major (Latin for 'greater dog'), and is located at a distance of about 500 light-years (150 parsecs) from the Sun.[1] In the modern constellation it lies at the position of the dog's front leg.
Nomenclature
Beta Canis Majoris is the star's Bayer designation. The traditional names Mirzam, Al-Murzim or Murzim,[11] derive from the Arabic (مرزم) for 'The Herald', and probably refers to its position, heralding (i.e., rising before) Sirius in the night sky. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[14] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[15] included a table of the first two batches of names approved by the WGSN; which included Mirzam for this star.
In Chinese, 軍市 (Jūn Shì), meaning 'Market for Soldiers', refers to an asterism consisting of β Canis Majoris, Nu3 Canis Majoris, 15 Canis Majoris, Pi Canis Majoris, Omicron1 Canis Majoris and Xi1 Canis Majoris.[16] Consequently, β Canis Majoris itself is known as 軍市一 (Jūn Shì yī, English: the First Star of Market for Soldiers).[17] From this Chinese name arose the name Kuen She.[11]
The Dunhuang Star Chart noted β Canis Majoris as Yeji "Pheasant Cock", though was located about 10 degrees too far north of its correct position.[18]
Beta Canis Majoris was called Oupo by the people of the Tuamotus.[19]
Properties
| Frequency (day−1) |
Amplitude (km s−1) |
|---|---|
| 3.9793 | 2.7 |
| 3.9995 | 2.6 |
| 4.1832 | 0.7 |
Mirzam is a Beta Cephei variable that varies in apparent magnitude between +1.97 and +2.01 over a six-hour period, a change in brightness that is too small to be discerned with the naked eye. It exhibits this variation in luminosity because of periodic pulsations in its outer envelope, which follow a complex pattern with three different cycles; all about six hours in length. The two dominant pulsation frequencies have a combined beat period of roughly 50 days. The strongest pulsation mode is a radial first overtone, while the second is non-radial.[8]
This star has a mass of about 13–14 times the mass of the Sun[8] with 8–11 times the Sun's radius.[9] The effective temperature of the star's outer envelope is about 23,150 K, which is much higher than the Sun's at 5,778 K. The energy emitted at the high temperature of the former is what gives this star a blue-white hue characteristic of a B-type star.[10][20] The estimated age of Mirzam is 12–13 million years, which is long enough for a star of this mass to have evolved into a giant star. The stellar classification of B1 II-III[4] indicates that the spectrum matches a star part way between a giant star and a bright giant.
Beta Canis Majoris is located near the far end of the Local Bubble, a cavity in the local interstellar medium through which the Sun is traveling.
In culture
Mirzam appears on the flag of Brazil, symbolising the state of Amapá.[21]
USS Murzim (AK-95) was a United States Navy Crater class cargo ship named after one of the star's alternative traditional names.
A small Dutch lamp company used the star in one of their commercials.
References
- 1 2 3 4 5 6 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 - 1 2 3 Cousins, A. W. J. (1972), "UBV Photometry of Some Very Bright Stars", Monthly Notes of the Astronomical Society of Southern Africa, 31: 69, Bibcode:1972MNSSA..31...69C
- ↑ Balona, L. A.; Bregman, L.; Letsapa, B. A.; Magoro, B. T.; Walsh, S. E. (1996). "The Pulsation Frequencies of beta CMa". Information Bulletin on Variable Stars. 4313: 1. Bibcode:1996IBVS.4313....1B.
- 1 2 Abt, Helmut A.; et al. (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode:2002ApJ...573..359A, doi:10.1086/340590
- ↑ 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: 02025. Bibcode:2009yCat....102025S.
- ↑ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Washington, Washington: Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W
- ↑ Shobbrook, R. R.; Handler, G.; Lorenz, D.; Mogorosi, D. (2006). "Photometric studies of three multiperiodic β Cephei stars: β CMa, 15 CMa and KZ Mus". Monthly Notices of the Royal Astronomical Society. 369: 171. arXiv:astro-ph/0603754. Bibcode:2006MNRAS.369..171S. doi:10.1111/j.1365-2966.2006.10289.x.
- 1 2 3 4 5 6 7 Mazumdar, A.; et al. (November 2006), "An asteroseismic study of the β Cephei star β Canis Majoris", Astronomy and Astrophysics, 459 (2): 589–596, arXiv:astro-ph/0607261, Bibcode:2006A&A...459..589M, doi:10.1051/0004-6361:20064980
- 1 2 3 4 Hubrig, S.; et al. (June 2006), "Discovery of magnetic fields in the βCephei star ξ1 CMa and in several slowly pulsating B stars*", Monthly Notices of the Royal Astronomical Society: Letters, 369 (1): L61–L65, arXiv:astro-ph/0604283, Bibcode:2006MNRAS.369L..61H, doi:10.1111/j.1745-3933.2006.00175.x
- 1 2 Zorec, J.; et al. (July 2009), "Fundamental parameters of B supergiants from the BCD system. I. Calibration of the (λ_1, D) parameters into Teff", Astronomy and Astrophysics, 501 (1): 297–320, arXiv:0903.5134, Bibcode:2009A&A...501..297Z, doi:10.1051/0004-6361/200811147
- 1 2 3 Allen, Richard Hinckley (1899), "Star-names and their meanings", New York, G. E. Stechert: 129–130, Bibcode:1899sntm.book.....A
- ↑ "V* bet CMa -- Variable Star of beta Cep type", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-02
- ↑ "IAU Catalog of Star Names". Retrieved 28 July 2016.
- ↑ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
- ↑ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
- ↑ (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.
- ↑ (Chinese) 香港太空館 - 研究資源 - 亮星中英對照表, Hong Kong Space Museum. Accessed on line November 23, 2010.
- ↑ Jean-Marc Bonnet-Bidaud; Dr Françoise Praderie & Dr Susan Whitfield (16 June 2009). "The Dunhuang Chinese Sky: A Comprehensive Study Of The Oldest Known Star Atlas".
- ↑ Makemson 1941, p. 239.
- ↑ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2012-03-10, retrieved 2012-01-16
- ↑ "Astronomy of the Brazilian Flag". FOTW Flags Of The World website.
Cited text
- Makemson, Maud Worcester (1941), The Morning Star Rises: An Account of Polynesian Astronomy, Yale University Press