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词条 Beta Canis Minoris
释义

  1. Nomenclature

  2. Properties

  3. Variability

  4. Possible companion

  5. References

{{Starbox begin
| name=Beta Canis Minoris
}}{{Starbox image
| image =
| caption = Position of Beta Canis Minoris.
}}{{Starbox observe
| epoch = J2000
| ra = {{RA|07|27|09.04174}}[1]
| dec = {{DEC|+08|17|21.5368}}[1]
| appmag_v = 2.84 - 2.92[3]
| constell = Canis Minor
}}{{Starbox character
| class = B8 Ve[4]
| b-v = –0.09[5]
| u-b = –0.28[5]
| variable = γ Cas[3] + SPBe[4]
}}{{Starbox astrometry
| radial_v = +22[9]
| prop_mo_ra = -59.375 ± 1.708[10]
| prop_mo_dec = -35.010 ± 1.368[10]
| parallax = 20.3535
| p_error =1.2220
| parallax_footnote = [1]
| absmag_v = −0.59[13]
}}{{Starbox detail
| mass = 3.5[4]
| radius = 3.5[15]
| luminosity = 195[4]
| temperature = 11,772[15]
| metal_fe =
| gravity = 3.51[15]
| rotational_velocity = 210[19]
| age_myr = {{val|160|+20|-60}}[20]
}}{{Starbox catalog
| names=Gomeisa, Algomeyla, Gomelza, 3 Canis Minoris, BD+08°1774, FK5 285, HD 58715, HIP 36188, HR 2845, IRAS 07244+0823, SAO 115456.[21]
}}{{Starbox reference
|Simbad=bet+CMi
}}{{Starbox end}}

Beta Canis Minoris (β Canis Minoris, abbreviated Beta CMi, β CMi), also named Gomeisa,[2] is a star in the constellation of Canis Minor. In the night sky it is notable for its proximity to the prominent star Procyon.

Nomenclature

β Canis Minoris (Latinised to Beta Canis Minoris) is the star's Bayer designation.

The traditional name Gomeisa comes from the Arabic al-ghumaisa’ 'the bleary-eyed (woman)',[23] short for مرزم الغميصاء mirzam al-ghumaisa’ 'girdle of the bleary-eyed one'. In Arabic, the short form would be identical with the name of Procyon. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[3] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[4] included a table of the first two batches of names approved by the WGSN; which included Gomeisa for this star.

In Chinese, {{lang|zh|南河}} ({{lang|zh-Latn|Nán Hé}}), meaning South River, refers to an asterism consisting of β Canis Minoris, Procyon and Epsilon Canis Minoris.[5] Consequently, β Canis Minoris itself is known as {{lang|zh|南河二}} ({{lang|zh-Latn|Nán Hé èr}}, {{lang-en|the Second Star of South River}}.)[6]

Properties

From parallax measurements, the distance to this star is about {{Convert|160 ± 10|ly|pc|abbr=off|lk=on}}. It has an apparent visual magnitude of 2.89,[5] making it easily visible to the naked eye. Beta Canis Minoris has about 3.5 times the Sun's mass and is rotating rapidly with a projected rotational velocity of {{nowrap|210 km s−1}},[19] which gives a lower bound on the azimuthal rotational velocity along the star's equator. The actual rotation rate may be about once per day.[23]

The stellar classification of this star is B8 Ve.[4] A luminosity class V star belongs on the main sequence, which means it is generating energy through the thermonuclear fusion of hydrogen at its core. The star is radiating this energy from its outer envelope at an effective temperature of 12,050 K,[4] giving it a blue-white hue typical of B-type stars.[33] An 'e' classification indicates that the spectrum contains emission lines, which means this is a Be star that is surrounded by a thin, circumstellar disk made of gaseous material ejected from the star. This hot, gaseous disk is about three times the radius of the star.[4]

Variability

β Canis Minoris has long been suspected of variability, and in 1977 it was classified as a γ Cassiopeiae variable in the General Catalogue of Variable Stars. A number of studies have found no variation at all.[36] While it shows little variation in brightness, it does display changes in the hydrogen emission coming from the gaseous disk but even those are less pronounced than in many other Be stars.[37]

Examination with the Canadian MOST space telescope reveals changes in the brightness of β Canis Minoris at the milli-magnitude level. This variation has a cyclic pattern formed from multiple overlapping frequencies, with the dominant frequencies being 3.257 and 3.282 cycles per day. As such, it belongs to a class called slowly pulsating B-type (SPB) stars. Be stars that show these types of pulsation have been dubbed SPBe stars.[4]

Possible companion

It is likely that Beta Canis Minoris is a close binary with a 170-day, eccentric orbit. The companion would have about 42% of the Sun's Mass. The nature of the companion is unknown, but it is speculated that it could be a subdwarf O star remaining after binary interactions that spun up the Be primary. If confirmed, this would make it a member of the very rare Phi Persei Be+sdO type systems.[37]

References

1. ^1 2 {{cite DR2|3143264535611161088}}
2. ^{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt | title=IAU Catalog of Star Names |accessdate=28 July 2016}}
3. ^{{cite web | url=https://www.iau.org/science/scientific_bodies/working_groups/280/ | title=IAU Working Group on Star Names (WGSN)|accessdate=22 May 2016}}
4. ^{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf | title=Bulletin of the IAU Working Group on Star Names, No. 1 |accessdate=28 July 2016}}
5. ^{{zh icon}} 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}}.
6. ^{{zh icon}} 香港太空館 - 研究資源 - 亮星中英對照表 {{webarchive|url=https://web.archive.org/web/20110130063007/http://www.lcsd.gov.hk/CE/Museum/Space/Research/StarName/c_research_chinengstars_e_g.htm |date=2011-01-30 }}, Hong Kong Space Museum. Accessed on line November 23, 2010.
7. ^1 {{cite journal|bibcode=1982IBVS.2123....1B|title=No Rapid Variability Observed for the Be Stars HD 58050 and β CMi|journal=Information Bulletin on Variable Stars|volume=2123|pages=1|author1=Bozic|first1=H.|last2=Muminovic|first2=M.|last3=Pavlovski|first3=K.|last4=Stupar|first4=M.|last5=Harmanec|first5=P.|last6=Horn|first6=J.|last7=Koubsky|first7=P.|year=1982}}
8. ^1 {{citation | title=XHIP: An extended hipparcos compilation | last1=Anderson | first1=E. | last2=Francis | first2=Ch. | journal=Astronomy Letters | volume=38 | issue=5 | pages=331 | year=2012 | bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015 | arxiv=1108.4971 | postscript=. }}
9. ^1 2 {{cite journal | first=F. | last=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 |arxiv = 0708.1752 }}
10. ^1 {{cite book | last=Wilson | first=Ralph Elmer | year=1953 | title=General Catalogue of Stellar Radial Velocities | publisher=Carnegie Institution of Washington | location=Washington | bibcode=1953GCRV..C......0W }}
11. ^1 2 {{citation | last1=Abt | first1=Helmut A. | last2=Levato | first2=Hugo | last3=Grosso | first3=Monica | title=Rotational Velocities of B Stars | journal=The Astrophysical Journal | volume=573 | issue=1 | pages=359–365 |date=July 2002 | doi=10.1086/340590 | bibcode=2002ApJ...573..359A }}
12. ^1 2 3 {{citation | last1=Johnson | display-authors=1 | first1=H. L. | last2=Iriarte | first2=B. | last3=Mitchell | first3=R. I. | last4=Wisniewskj | first4=W. Z. | title=UBVRIJKL photometry of the bright stars | journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | pages=99 | year=1966 | bibcode=1966CoLPL...4...99J }}
13. ^1 2 3 4 5 6 7 8 {{citation | display-authors=1 | last1=Saio | first1=H. | last2=Cameron | first2=C. | last3=Kuschnig | first3=R. | last4=Walker | first4=G. A. H. | last5=Matthews | first5=J. M. | last6=Rowe | first6=J. F. | last7=Lee | first7=U. | last8=Huber | first8=D. | last9=Weiss | first9=W. W. | title=MOST Detects g-Modes in the Late-Type Be Star β Canis Minoris (B8 Ve) | journal=The Astrophysical Journal | volume=654 | issue=1 | pages=544–550 |date=January 2007 | doi=10.1086/509315 | bibcode=2007ApJ...654..544S |arxiv = astro-ph/0609460 }}
14. ^1 2 3 {{citation | last1=Meilland | first1=A. | last2=Stee | first2=Ph. | last3=Chesneau | first3=O. | last4=Jones | first4=C. | title=VLTI/MIDI observations of 7 classical Be stars | journal=Astronomy and Astrophysics | volume=505 | issue=2 | pages=687–693 |date=October 2009 | doi=10.1051/0004-6361/200911960 | bibcode=2009A&A...505..687M |arxiv = 0908.1239 }}
15. ^1 {{citation | title=bet CMi -- Be Star | work=SIMBAD | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Beta+Canis+Minoris | accessdate=2012-01-09 }}
16. ^1 2 {{citation | first1=James B. | last1=Kaler | work=Stars | title=GOMEISA (Beta Canis Minoris) | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/gomeisa.html | accessdate=2012-01-09 }}
17. ^1 {{citation |title=The Colour of Stars |date=December 21, 2004 |work=Australia Telescope, Outreach and Education |publisher=Commonwealth Scientific and Industrial Research Organisation |url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |accessdate=2012-01-16 |deadurl=yes |archiveurl=https://www.webcitation.org/6630AbtJZ?url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |archivedate=2012-03-10 |df= }}
18. ^1 {{citation | display-authors=1 | last1=Janson | first1=Markus | last2=Bonavita | first2=Mariangela | last3=Klahr | first3=Hubert | last4=Lafrenière | first4=David | last5=Jayawardhana | first5=Ray | last6=Zinnecker | first6=Hans | title=High-contrast Imaging Search for Planets and Brown Dwarfs around the Most Massive Stars in the Solar Neighborhood | journal=The Astrophysical Journal | volume=736 | issue=2 | page=89 |date=August 2011 | doi=10.1088/0004-637X/736/2/89 | bibcode=2011ApJ...736...89J |arxiv = 1105.2577 }}
19. ^1 2 {{cite journal|bibcode=2017ApJ...836..112D|arxiv=1701.05201|title=A Spectroscopic Orbit for the Late-type Be Star β CMi|journal=The Astrophysical Journal|volume=836|pages=112|author1=Dulaney|first1=Nicholas A.|last2=Richardson|first2=Noel D.|last3=Gerhartz|first3=Cody J.|last4=Bjorkman|first4=J. E.|last5=Bjorkman|first5=K. S.|last6=Carciofi|first6=Alex C.|last7=Klement|first7=Robert|last8=Wang|first8=Luqian|last9=Morrison|first9=Nancy D.|last10=Bratcher|first10=Allison D.|last11=Greco|first11=Jennifer J.|last12=Hardegree-Ullman|first12=Kevin K.|last13=Lembryk|first13=Ludwik|last14=Oswald|first14=Wayne L.|last15=Trucks|first15=Jesica L.|year=2017|doi=10.3847/1538-4357/836/1/112}}
20. ^1 2 {{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)|journal=VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S|volume=1|display-authors=etal|author1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009}}
[7][8][9][10][11][12][13][14][15][16][17][18][19][20]
}}{{Stars of Canis Minor}}

12 : Bayer objects|B-type main-sequence stars|Canis Minor|Gamma Cassiopeiae variable stars|Stars with proper names|Flamsteed objects|Hipparcos objects|HR objects|Henry Draper Catalogue objects|Durchmusterung objects|Slowly pulsating B stars|Spectroscopic binaries
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