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Alpha Coronae Borealis

Coordinates: Sky map 15h 34m 41.268s, +26° 42′ 52.89″
From Wikipedia, the free encyclopedia
Alpha Coronae Borealis
Location of α Coronae Borealis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Corona Borealis
Right ascension 15h 34m 41.268s[1]
Declination +26° 42′ 52.89″[1]
Apparent magnitude (V) 2.24[2]
Characteristics
Spectral type A0V + G5V[3]
U−B color index −0.03[4]
B−V color index −0.02[4]
Variable type Eclipsing binary[5]
Astrometry
Radial velocity (Rv)+1.7[6] km/s
Proper motion (μ) RA: 120.27[1] mas/yr
Dec.: −89.58[1] mas/yr
Parallax (π)43.46 ± 0.28 mas[1]
Distance75.0 ± 0.5 ly
(23.0 ± 0.1 pc)
Absolute magnitude (MV)+0.16/+5.05[3]
Orbit
Period (P)17.3599 d[7]
Semi-major axis (a)0.19379(50) AU[8]
Eccentricity (e)0.3794(19)[8]
Inclination (i)88.2 ± 0.1[7]°
Periastron epoch (T)56,646±0 (JD)[8]
Argument of periastron (ω)
(secondary)		312.32±0.43[8]°
Semi-amplitude (K1)
(primary)		36.22±0.13[8] km/s
Semi-amplitude (K2)
(secondary)		98.02±0.33[8] km/s
Details
α CrB A
Mass2.58[3] M☉
Radius2.89–3.04[3][7] R☉
Luminosity74[3] L☉
Surface gravity (log g)3.89[3] cgs
Temperature9,700[3] K
Rotational velocity (v sin i)139[9] km/s
Age0.314 Gyr
α CrB B
Mass0.92[3] M☉
Radius0.90[3][7] R☉
Luminosity0.81[3] L☉
Surface gravity (log g)4.50[3] cgs
Temperature5,800[3] K
Rotational velocity (v sin i)< 14[7] km/s
Other designations
Gemma, Alphecca, Ashtaroth, Gnosia Stella Coronae, 5 CrB, BD +27°2512, GCTP 3519.00, FK5 578, HD 139006, HIP 76267, HR 5793, SAO 83893.
Database references
SIMBADdata

Alpha Coronae Borealis (α Coronae Borealis, abbreviated Alpha CrB, α CrB), officially named Alphecca /ælˈfɛkə/,[10] is an eclipsing binary star in the constellation of Corona Borealis. It is located about 75 light years from the Sun and contains two main sequence stars, one class A and one class G.

Properties

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A light curve for Alpha Coronae Borealis, plotted from TESS data[11]
α Coronae Borealis in optical light

Alpha Coronae Borealis is a binary system, its stars orbiting each other in an eccentric orbit every 17.36 days. Because the plane of this orbit is inclined at an angle of 88.2° to the line of sight to the Earth,[7] the pair form a detached eclipsing binary system similar to Algol (β Per). The periodic eclipses result in a magnitude variation of +2.21 to +2.32, which is hardly noticeable to the unaided eye.

The primary component is a white main sequence star that has a stellar classification of A0V and 2.6 times the mass of the Sun. Estimates of the star's radius range from 2.89 to 3.04 times the radius of the Sun.[3][7] An excess of infrared radiation at 24 μm and 70 μm has been detected about the primary star by the IRAS.[12] This suggests the presence of a large disc of dust and material around the star, prompting speculation of a planetary or proto-planetary system similar to that currently assumed around Vega. The disk extends out to a radius of around 60 astronomical units (AU).[13]

The secondary component is a yellow main sequence star with an estimated stellar class of G5, 0.92 times the Sun's mass and 0.90 times the Sun's radius. The X-ray luminosity of this star is 6 × 1028 erg s−1, which is 30 times greater than the peak activity level of the Sun. This higher activity level is expected for a young star of this class. The corona has a temperature of about 5 MK, which is much hotter than the Sun's corona. The upper limit of 14 km/s for the equatorial rotation velocity is equivalent to a rotation period of 3 days. More likely, the rotation period is 7–9 days.[3][7]

The space velocity components of this star system are U = +14.257, V = +0.915 and W = +3.147 km/s. α CrB is believed to be a member of the Ursa Major Moving Group of stars that have a common motion through space.[14]

Nomenclature

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α CrB, the brightest star in Corona Borealis

α Coronae Borealis (Latinised to Alpha Coronae Borealis) is the star's Bayer designation.

It bore the traditional names Alphecca, Gemma, and Gnosia Stella Coronae. Alphecca is Arabic, short for نير الفكّة nayyir al-fakka "the bright (star) of the broken (ring of stars)". Gemma is Latin for "jewel". Also Latin in origin is Gnosia Stella Coronae "Cretan star of the Crown" (specifically from Vergil's Georgics),[15] from Gnōsus or Gnōsos ("Knossos"), referencing the birthplace of Ariadne, whose wedding diadem became in some myths the constellation of Corona Borealis, following her marriage to Bacchus.[16] As the brightest star in Corona Borealis, it lent its name to Alphekka Meridiana, the brightest in the constellation of Corona Australis.[citation needed] The International Astronomical Union Working Group on Star Names (WGSN) has chosen Alphecca as the formal name for this star.[17]

The term nayyir al-fakka or Nir al Feccah appeared in the Al Achsasi Al Mouakket catalogue.[18]

In Chinese, 貫索 (Guàn Suǒ), meaning Coiled Thong, refers to an asterism consisting of Alpha Coronae Borealis, Pi Coronae Borealis, Theta Coronae Borealis, Beta Coronae Borealis, Gamma Coronae Borealis, Delta Coronae Borealis, Epsilon Coronae Borealis, Iota Coronae Borealis and Rho Coronae Borealis.[19] Consequently, the Chinese name for Alpha Coronae Borealis itself is 貫索四 (Guàn Suǒ sì, English: the Fourth Star of Coiled Thong.).[20]

In culture

[edit]

Under the name Alphecca, this is one of the medieval Behenian fixed stars.

References

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  1. ^ a b c d e van Leeuwen, F. (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. Vizier catalog entry
  2. ^ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". VizieR Online Data Catalog. 2237. Bibcode:2002yCat.2237....0D.
  3. ^ a b c d e f g h i j k l m n Tomkin, J.; Popper, D. M. (June 1986). "Rediscussion of eclipsing binaries. XV - Alpha Coronae Borealis, a main-sequence system with components of types A and G". Astronomical Journal. 91: 1428. Bibcode:1986AJ.....91.1428T. doi:10.1086/114121.
  4. ^ a b Johnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4 (99): 99. Bibcode:1966CoLPL...4...99J.
  5. ^ 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.
  6. ^ Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication: 0. Bibcode:1953GCRV..C......0W.
  7. ^ a b c d e f g h Güdel, M.; Arzner, K.; Audard, M.; Mewe, R. (May 2003). "Tomography of a stellar X-ray corona: alpha Coronae Borealis". Astronomy and Astrophysics. 403: 155–171. Bibcode:2003A&A...403..155G. doi:10.1051/0004-6361:20030257.
  8. ^ a b c d e f Schmitt, J. H. M. M.; Schröder, K.-P.; Rauw, G.; Hempelmann, A.; Mittag, M.; González-Pérez, J. N.; Czesla, S.; Wolter, U.; Jack, D. (2016-02-01). "The α CrB binary system: A new radial velocity curve, apsidal motion, and the alignment of rotation and orbit axes". Astronomy & Astrophysics. 586: A104. doi:10.1051/0004-6361/201526662. ISSN 0004-6361.
  9. ^ Royer, F.; Grenier, S.; Baylac, M.-O.; Gómez, A. E.; Zorec, J. (October 2002). "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i". Astronomy and Astrophysics. 393 (3): 897–911. arXiv:astro-ph/0205255. Bibcode:2002A&A...393..897R. doi:10.1051/0004-6361:20020943. S2CID 14070763. Table 8.
  10. ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
  11. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  12. ^ Su, K. Y. L.; et al. (December 2006). "Debris Disk Evolution around A Stars". The Astrophysical Journal. 653 (1): 675–689. arXiv:astro-ph/0608563. Bibcode:2006ApJ...653..675S. doi:10.1086/508649. S2CID 14116473.
  13. ^ Pawellek, Nicole; Krivov, Alexander V.; Marshall, Jonathan P.; Montesinos, Benjamin; Ábrahám, Péter; Moór, Attila; et al. (2014). "Disk Radii and Grain Sizes in Herschel-resolved Debris Disks". The Astrophysical Journal. 792 (1): 19. arXiv:1407.4579. Bibcode:2014ApJ...792...65P. doi:10.1088/0004-637X/792/1/65. S2CID 119282523. 65.
  14. ^ King, Jeremy R.; Villarreal, Adam R.; Soderblom, David R.; Gulliver, Austin F.; Adelman, Saul J. (April 2003). "Stellar Kinematic Groups. II. A Reexamination of the Membership, Activity, and Age of the Ursa Major Group". The Astronomical Journal. 125 (4): 1980–2017. Bibcode:2003AJ....125.1980K. doi:10.1086/368241.
  15. ^ Allen, Richard Hinckley. "Corona Borealis, the Northern Crown, Star Names — Their Lore and Meaning".
  16. ^ Ridpath, Ian; Tirion, Wil (2001). Stars and Planets Guide. Princeton, New Jersey: Princeton University Press. pp. 126–128. ISBN 978-0-691-08913-3.
  17. ^ "Naming Stars". International Astronomical Union. Retrieved 2018-11-02.
  18. ^ Knobel, E. B. (June 1895). "Al Achsasi Al Mouakket, on a catalogue of stars in the Calendarium of Mohammad Al Achsasi Al Mouakket". Monthly Notices of the Royal Astronomical Society. 55 (8): 429. Bibcode:1895MNRAS..55..429K. doi:10.1093/mnras/55.8.429.
  19. ^ (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.
  20. ^ (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 Archived 2008-10-25 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
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