The traditional name Denebola is shortened from Deneb Alased, from the Arabic phrase ذنب الاسدðanab al-asad 'tail of the lion', as it represents the lion's tail, the star's position in the Leo constellation.[15] (DenebinCygnus has a similar name origin.) In the Alphonsine Tables it was recorded as Denebalezeth.[16]OnR. 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)[17] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[18] 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.[19]
15th century astronomer Ulugh Beg, gives the name Al Ṣarfah, the Changer (i.e. of the weather), as the star's individual title.[20]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."[20]
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).
InHinduastronomy, Denebola corresponds to the Nakshatra (a sector along the ecliptic) named Uttara Phalgunī (second reddish one).
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]
Denebola shows a strong infrared excess, indicating there is a circumstellar debris disk of cool dust in orbit around it.[23] 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.[24] 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.[25]
^ abGray, 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. S2CID119417105.
^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.
^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. ISBN80-85882-08-6.
^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.
