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Denebola

Summary

Denebola is the second-brightest individual star in the zodiac constellation of Leo.[13] It is the easternmost of the bright stars of Leo. It has the Bayer designation Beta Leonis or β Leonis, which are abbreviated Beta Leo or β Leo. Denebola is an A-type main sequence star with 75% more mass than the Sun and 15 times the Sun's luminosity. Based on parallax measurements from the Hipparcos astrometry satellite, the star is at a distance of 36 light-years (11 parsecs) from the Sun. Its apparent visual magnitude is 2.14, making it readily visible to the naked eye. Denebola is a Delta Scuti type variable star, meaning its luminosity varies very slightly over a period of a few hours.

Denebola
Location of β Leonis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Leo
Pronunciation /dəˈnɛbələ/,[1]
Right ascension 11h 49m 03.57834s[2]
Declination +14° 34′ 19.4090″[2]
Apparent magnitude (V) 2.14[3]
Characteristics
Spectral type A3Va[4]
U−B color index +0.07[5]
B−V color index +0.09[5]
Variable type δ Sct[3]
Astrometry
Radial velocity (Rv)−0.2[6] km/s
Proper motion (μ) RA: −497.68[2] mas/yr
Dec.: −114.67[2] mas/yr
Parallax (π)90.91 ± 0.52 mas[2]
Distance35.9 ± 0.2 ly
(11.00 ± 0.06 pc)
Absolute magnitude (MV)+1.93[7]
Details
Mass1.78[8] M☉
Radius1.728[8] R☉
Luminosity15[8] L☉
Surface gravity (log g)4.0[9] cgs
Temperature8,500[9] K
Metallicity [Fe/H]+0.00[8] dex
Rotational velocity (v sin i)128[10] km/s
Age100–380[8] Myr
Other designations
Deneb Aleet, β Leonis, 94 Leo, BD+15°2383, FK5 444, GJ 448, HD 102647, HIP 57632, HR 4534, SAO 99809, LHS 2462, LTT 13249[11][12]
Database references
SIMBADdata

Nomenclature edit

 
Denebola is the most eastward (left) bright star in this stick-figure diagram overlaid on a constellation photograph of Leo

β Leonis (Latinised to Beta Leonis) is the star's Bayer designation. In Johann Bayer's Uranometria (1603), it was designated β (Beta) as the second-brightest star in the constellation. It also bears the Flamsteed designation of 94 Leonis (assigned on the basis of increasing right ascension rather than luminosity) and additional designations followed as the star was recorded in subsequent star catalogues.

The traditional name Denebola is shortened from Deneb Alased, from the Arabic phrase ذنب الاسد ðanab al-asad 'tail of the lion', as it represents the lion's tail, the star's position in the Leo constellation.[14] (Deneb in Cygnus has a similar name origin.) In the Alphonsine Tables it was recorded as Denebalezeth.[15] On R. A. Proctor's 1871 star chart of the Northern Hemisphere it was designated Deneb Aleet. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[16] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[17] included a table of the first two batches of names approved by the WGSN, which included Denebola for this star. It is now so entered in the IAU Catalog of Star Names.[18]

15th century astronomer Ulugh Beg, gives the name Al Ṣarfah, the Changer (i.e. of the weather), as the star's individual title.[19] Al-Biruni, a Muslim scholar and polymath of the 11th century, wrote of it: "The heat turns away when it rises, and the cold turns away when it disappears."[19]

Ancient Chinese astronomers designated it the first star of the five-star asterism "Seat of the Five Emperors", hence its Chinese name 五帝座一 (Wǔdìzuò-yī).

In Hindu astronomy, Denebola corresponds to the Nakshatra (a sector along the ecliptic) named Uttara Phalgunī (second reddish one).

Denebola, along with Spica and Arcturus, is part of the Spring Triangle asterism, and by extension, also of the Great Diamond together with the star Cor Caroli.[20]

Properties edit

Denebola is a relatively young star with an age estimated at less than 400 million years. Interferometric observations give a radius that is about 173% that of the Sun. Its high rate of rotation results in an oblate shape with an equatorial bulge. It has 75% more mass than the Sun, which results in a much higher overall luminosity and a shorter life span on the main sequence.[8]

 
Illustration of an A-type dwarf star

Based upon the star's spectrum, it has a stellar classification of A3 Va,[4] with the luminosity class 'Va' indicating this is a particularly luminous dwarf, a main sequence star that is generating energy through the nuclear fusion of hydrogen at its core. The effective temperature of Denebola's outer envelope is about 8,500 K, which results in the white hue typical of A-type stars. Denebola has a high projected rotational velocity of 128 km/s, which is of the same order of magnitude as for the very rapidly rotating star Achernar. The Sun, in comparison, has an equatorial rotation velocity of 2 km/s.[9] This star is believed to be a Delta Scuti variable star that exhibits fluctuations in luminosity of 0.025 magnitudes roughly ten times per day.[21]

Denebola shows a strong infrared excess, indicating there is a circumstellar debris disk of cool dust in orbit around it.[22] This dust has a temperature of about 120 K (−153 °C). Observations with the Herschel Space Observatory have provided resolved images, which show the disk to be located at a mean radius of 39 astronomical units from the star.[23] As the Solar System is believed to have formed out of such a disk, Denebola and similar stars such as Vega and Beta Pictoris may be candidate locations for extrasolar planets.

Kinematic studies have shown that Denebola is part of a stellar association dubbed the IC 2391 supercluster. All the stars of this group share a roughly common motion through space, although they are not gravitationally bound. This suggests that they were born in the same location, and perhaps initially formed an open cluster. Other stars in this association include Alpha Pictoris, Beta Canis Minoris and the open cluster IC 2391. In total more than sixty probable members of the group have been identified.[24]

In culture edit

In astrology, Denebola was believed to portend misfortune and disgrace.[25]

See also edit

References edit

  1. ^ "Denebola". Merriam-Webster.com Dictionary.
  2. ^ a b c d e 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.
  3. ^ a b Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
  4. ^ a b Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Robinson, P. E. (2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I". The Astronomical Journal. 126 (4): 2048. arXiv:astro-ph/0308182. Bibcode:2003AJ....126.2048G. doi:10.1086/378365. S2CID 119417105.
  5. ^ a b Hoffleit, D.; Jaschek, C., eds. (1991). The Bright Star Catalogue. New Haven: Yale University Observatory. Bibcode:1991bsc..book.....H.
  6. ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. Vol. 30. University of Toronto: International Astronomical Union. p. 57. Bibcode:1967IAUS...30...57E.
  7. ^ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  8. ^ a b c d e f Di Folco, E.; et al. (2004). "VLTI near-IR interferometric observations of Vega-like stars". Astronomy and Astrophysics. 426 (2): 601–617. Bibcode:2004A&A...426..601D. doi:10.1051/0004-6361:20047189.
  9. ^ a b c Acke, B.; Waelkens, C. (2004). "Chemical analysis of 24 dusty (pre-)main sequence stars". Astronomy and Astrophysics. 427 (3): 1009–1017. arXiv:astro-ph/0408221. Bibcode:2004A&A...427.1009A. doi:10.1051/0004-6361:20041460. S2CID 16615394.
  10. ^ Royer, F.; Zorec, J.; Gómez, A. E. (February 2007). "Rotational velocities of A-type stars. III. Velocity distributions". Astronomy and Astrophysics. 463 (2): 671–682. arXiv:astro-ph/0610785. Bibcode:2007A&A...463..671R. doi:10.1051/0004-6361:20065224. S2CID 18475298.
  11. ^ "* bet Leo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2007-06-18.
  12. ^ "Denebola". Alcyone. Retrieved 2006-08-10.
  13. ^ The two components of the γ Leonis double star, which are unresolved to the naked eye, have a combined magnitude brighter than it.
  14. ^ Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York, NY: Dover Publications Inc. p. 258. ISBN 0-486-21079-0. Retrieved 2010-12-12.
  15. ^ Kunitzsch, Paul (1986). "The Star Catalogue Commonly Appended to the Alfonsine Tables". Journal for the History of Astronomy. 17 (49): 89–98. Bibcode:1986JHA....17...89K. doi:10.1177/002182868601700202. S2CID 118597258.
  16. ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  17. ^ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  18. ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
  19. ^ a b LacusCurtius • Allen's Star Names — Leo
  20. ^ Rao, Joe (June 11, 2012). "How to See Mars and Saturn in Night Sky's Spring Triangle". Space.com. Archived from the original on 2023-05-29. Retrieved 2024-01-29.
  21. ^ Mkrtichian, D. E.; Yurkov, A. (5–7 November 1997). "β Leo - Back to Delta Scuti Stars?". Proceedings of the 20th Stellar Conference of the Czech and Slovak Astronomical Institutes. Brno, Czech Republic: Dordrecht, D. Reidel Publishing Co. p. 172. Bibcode:1998vsr..conf..143M. ISBN 80-85882-08-6.
  22. ^ Cote, J. (1987). "B and A type stars with unexpectedly large colour excesses at IRAS wavelengths". Astronomy and Astrophysics. 181 (1): 77–84. Bibcode:1987A&A...181...77C.
  23. ^ Matthews, B. C.; et al. (2010). "Resolving debris discs in the far-infrared: Early highlights from the DEBRIS survey". Astronomy and Astrophysics. 518: L135. arXiv:1005.5147. Bibcode:2010A&A...518L.135M. doi:10.1051/0004-6361/201014667. S2CID 54013449.
  24. ^ Eggen, O. J. (1991). "The IC 2391 supercluster". Astronomical Journal. 102: 2028–2040. Bibcode:1991AJ....102.2028E. doi:10.1086/116025.
  25. ^ Allen, Richard Hinckley (1899). Star Names and their Meanings. New York, Leipzig: G. E. Stechert.

Further reading edit

  • Defrère, D.; et al. (April 2021). "The HOSTS Survey: Evidence for an Extended Dust Disk and Constraints on the Presence of Giant Planets in the Habitable Zone of β Leo". The Astronomical Journal. 161 (4): 186. arXiv:2103.03268. Bibcode:2021AJ....161..186D. doi:10.3847/1538-3881/abe3ff. S2CID 232135141. 186.
  • Churcher, L. J.; et al. (November 2011). "Multiwavelength modelling of the β Leo debris disc: one, two or three planetesimal populations?". Monthly Notices of the Royal Astronomical Society. 417 (3): 1715–1734. arXiv:1107.0316. Bibcode:2011MNRAS.417.1715C. doi:10.1111/j.1365-2966.2011.19341.x. S2CID 73557018.
  • Stock, Nathan D.; et al. (December 2010). "The Structure of the β Leonis Debris Disk". The Astrophysical Journal. 724 (2): 1238–1255. arXiv:1010.0003. Bibcode:2010ApJ...724.1238S. doi:10.1088/0004-637X/724/2/1238. S2CID 28349642.
  • Bartolini, C.; et al. (August 1981). "The delta Scuti Star beta Leonis". Information Bulletin on Variable Stars. 2010: 1. Bibcode:1981IBVS.2010....1B.

External links edit

  • Kaler, Jim. "Denebola". Stars. University of Illinois. Retrieved 2012-01-14.

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