Regulus

This article is about the star. For the Roman general and consul, see Marcus Atilius Regulus. For other uses, see Regulus (disambiguation).
Regulus

Location of Regulus in Leo
Observation data
Epoch J2000      Equinox J2000
Constellation Leo
Right ascension A: 10h 08m 22.311s[1]
BC: 10h 08m 12.8/14s[2]
Declination A: +11° 58′ 01.95″[1]
BC: +11° 59′ 48″[2]
Apparent magnitude (V) 1.40[3]/8.13[4]/13.50[4]
Characteristics
Evolutionary stage Main sequence
Spectral type B8 IVn[3] + K2 V[5] + M4 V[5]
U−B color index –0.36/+0.51[6]
B−V color index –0.11/+0.86[6]
Variable type Suspected[7]
Astrometry
Radial velocity (Rv)+5.9/+6.3[8] km/s
Proper motion (μ) RA: -248.73 ± 0.35[1] mas/yr
Dec.: 5.59 ± 0.21[1] mas/yr
Parallax (π)41.13 ± 0.35[1] mas
Distance79.3 ± 0.7 ly
(24.3 ± 0.2 pc)
Absolute magnitude (MV)–0.52/6.3/11.6
Details
α Leo A
Mass3.8[9] M☉
Radius3.092 ± 0.147[3] R☉
Luminosity288[9] L☉
Surface gravity (log g)3.54 ± 0.09[10] cgs
Temperature12,460 ± 200[9] K
Rotational velocity (v sin i)347[11] km/s
Age≳1[12] Gyr
α Leo B/C
Mass0.8[13]/0.3[4] M☉
Radius0.5/? R☉
Luminosity0.50[13]/? L☉
Surface gravity (log g)4.4[13]/? cgs
Temperature4885[13]/? K
Other designations
Alpha Leonis, 32 Leo, Cor Leonis, Aminous Basilicus, Lion’s Heart, Rex, Kalb al Asad, Kabeleced, FK5 380, GCTP 2384.00, GJ 9316, HIP 49669, HR 3982.
α Leo A: BD+12 2149, HD 87901, LTT 12716, SAO 98967.
α Leo B/C: BD+12 2147, HD 87884, LTT 12714, SAO 98966.
Database references
SIMBADdata

Regulus (α Leo, α Leonis, Alpha Leonis) is the brightest star in the constellation Leo and one of the brightest stars in the night sky, lying approximately 79 light years from Earth.[1] Regulus is a multiple star system composed of four stars that are organized into two pairs. The spectroscopic binary Regulus A consists of a blue-white main-sequence star and its companion, which has not yet been directly observed, but is probably a white dwarf.[5] Located farther away is the pair Regulus B and Regulus C and D, which are dim main-sequence stars.

Observations

Regulus is 0.46 degree from the ecliptic, the closest of the bright stars, and is regularly occulted by the Moon. Occultations by the planets Mercury and Venus are possible but rare, as are occultations by asteroids.

The last occultation of Regulus by a planet was on July 7, 1959, by Venus.[14] The next will occur on October 1, 2044, also by Venus. Other planets will not occult Regulus over the next few millennia because of their node positions. An occultation of Regulus by the asteroid 166 Rhodope was observed by 12 researchers from Portugal, Spain, Italy, and Greece on October 19, 2005. Differential bending of light was measured to be consistent with general relativity.[15] Regulus was occulted by the asteroid 163 Erigone in the early morning of March 20, 2014.[16] The center of the shadow path passed through New York and eastern Ontario, but no one is known to have seen it, due to cloud cover. The International Occultation Timing Association recorded no observations at all.[17]

Although best seen in the evening in northern hemisphere in late winter and spring, Regulus appears at some time of night throughout the year except for about a month on either side of August 22, when the Sun is too near. Regulus passes through SOHO's LASCO C3 every August.[18] For most Earth observers, the heliacal rising of Regulus occurs in the first week of September. Every 8 years, Venus passes Regulus around the time of the star's heliacal rising, as on 5 September 2014.

The primary of Regulus A has about 3.5 times the Sun’s mass. It is spinning extremely rapidly, with a rotation period of only 15.9 hours, which causes it to have a highly oblate shape.[19] This results in so-called gravity darkening: the photosphere at Regulus' poles is considerably hotter, and five times brighter per unit surface area, than its equatorial region. If it were rotating only 15% faster, the star's gravity would be insufficient to hold it together, and it would spin itself apart.[12]

System

Regulus is a multiple star system consisting of at least four stars. Regulus A is the dominant star, with a binary companion 177" distant that is thought to be physically related. Regulus D is a 12th magnitude companion at 212", which shares a common motion with the other stars.[20]

Regulus A is a binary star consisting of a blue-white main sequence star of spectral type B7V, which is orbited by a star of at least 0.3 solar masses, which is probably a white dwarf. The two stars take approximately 40 days to complete an orbit around their common centre of mass. Given the extremely distorted shape of the primary, the relative orbital motion may be notably altered with respect to the two-body purely Keplerian scenario because of non-negligible long-term orbital perturbations affecting, for example, its orbital period. In other words, Kepler's third law, which holds exactly only for two point-like masses, would be no longer valid because of the highly distorted shape of the primary. Regulus A was long thought to be fairly young, only 50 - 100 million years old, calculated by comparing its temperature, luminosity, and mass. The existence of a white dwarf companion would mean that the system is at least a 1,000 million years old, just to account for the formation of the white dwarf. The discrepancy can be accounted for by a history of mass transfer onto a once-smaller Regulus A.[12]

Regulus BC is 5,000 AU[21] from Regulus A. They share a common proper motion and are thought to orbit each other taking several million years.[4] Designated Regulus B and Regulus C, the pair has Henry Draper Catalogue number HD 87884. The first is a K2V star, while the companion is approximately M4V.[19] The companion pair has an orbital period of about 600 years[4] with a separation of 2.5" in 1942.[19]

Visibility

The Regulus system as a whole is the twenty-first brightest star in the night sky with an apparent magnitude of +1.35. The light output is dominated by Regulus A. Regulus B, if seen in isolation, would be a binocular object of magnitude +8.1, and its companion, Regulus C, the faintest of the three stars that has been directly observed, would require a substantial telescope to be seen, at magnitude +13.5. Regulus A is itself a spectroscopic binary: the secondary star has not yet been directly observed as it is much fainter than the primary. The BC pair lies at an angular distance of 177 arc-seconds from Regulus A, making them visible in amateur telescopes.[22]

Etymology and cultural associations

Rēgulus is Latin for 'prince' or 'little king'. The Greek variant Basiliscus is also used. It is known as Qalb al-Asad, from the Arabic قلب الأسد, meaning 'the heart of the lion'. This phrase is sometimes approximated as Kabelaced and translates into Latin as Cor Leōnis. It is known in Chinese as 轩辕十四, the Fourteenth Star of Xuanyuan, the Yellow Emperor. In Hindu astronomy, Regulus corresponds to the Nakshatra Magha ("the bountiful").

Babylonians called it Sharru ("the King"), and it marked the 15th ecliptic constellation. In India it was known as Maghā ("the Mighty"), in Sogdiana Magh ("the Great"), in Persia Miyan ("the Centre") and also as Venant, one of the four 'royal stars' of the Persian monarchy.[23] It was one of the fifteen Behenian stars known to medieval astrologers, associated with granite, mugwort, and the kabbalistic symbol .

In MUL.APIN, Regulus is listed as LUGAL, meaning "the star that stands in the breast of the Lion:the King.".[24]

Regulus through Celestron CGEM DX 1100 @ F6.3, Canon T3i, Televue 4X Powermate, ISO 800, 30 sec exposure

See also

References

  1. 1 2 3 4 5 6 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. Vizier catalog entry
  2. 1 2 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27. Bibcode:2000A&A...355L..27H.
  3. 1 2 3 van Belle, Gerard T.; von Braun, Kaspar (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". The Astrophysical Journal 694 (2): 1085–1098. arXiv:0901.1206. Bibcode:2009ApJ...694.1085V. doi:10.1088/0004-637X/694/2/1085.
  4. 1 2 3 4 5 Tokovinin, A. A. (1997). "MSC - a catalogue of physical multiple stars". Astronomy and Astrophysics Supplement Series 124: 75–84. Bibcode:1997A&AS..124...75T. doi:10.1051/aas:1997181.
  5. 1 2 3 Gies, D.R.; Dieterich, S.; Richardson, N. D.; Riedel, A. R.; Team, B. L.; McAlister, H. A.; Bagnuolo, Jr., W. G.; Grundstrom, E. D.; Štefl, S.; Rivinius, Th.; Baade, D.; et al. (2008). "A Spectroscopic Orbit for Regulus". The Astrophysical Journal 682 (2): L117–L120. arXiv:0806.3473. Bibcode:2008ApJ...682L.117G. doi:10.1086/591148.
  6. 1 2 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues 2237: 0. Bibcode:2002yCat.2237....0D.
  7. ↑ 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.
  8. ↑ Evans, D. S. (1967). "The Revision of the General Catalogue of Radial Velocities". Determination of Radial Velocities and their Applications 30: 57. Bibcode:1967IAUS...30...57E.
  9. 1 2 3 Malagnini, M. L.; Morossi, C. (November 1990), "Accurate absolute luminosities, effective temperatures, radii, masses and surface gravities for a selected sample of field stars", Astronomy and Astrophysics Supplement Series 85 (3): 1015–1019, Bibcode:1990A&AS...85.1015M.
  10. ↑ Fitzpatrick, E. L.; Massa, D. (March 2005), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", The Astronomical Journal 129 (3): 1642–1662, arXiv:astro-ph/0412542, Bibcode:2005AJ....129.1642F, doi:10.1086/427855.
  11. ↑ Zorec, J.; Royer, F. (January 2012), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", Astronomy & Astrophysics 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691.
  12. 1 2 3 Rappaport, S.; Podsiadlowski, Ph.; Horev, I. (2009). "The Past and Future History of Regulus". The Astrophysical Journal 698 (1): 666–675. arXiv:0904.0395. Bibcode:2009ApJ...698..666R. doi:10.1088/0004-637X/698/1/666.
  13. 1 2 3 4 Martin, E. L.; Magazzu, A.; Rebolo, R. (1992). "On the post-T-Tauri nature of late-type visual companions to B-type stars". Astronomy and Astrophysics 257: 186. Bibcode:1992A&A...257..186M.
  14. ↑ "Occultations of bright stars by planets between 0 and 4000". Retrieved 2007-10-16.
  15. ↑ Sigismondi, Costantino; Troise, Davide (2008). "Asteroidal Occultation of Regulus:. Differential Effect of Light Bending". "THE ELEVENTH MARCEL GROSSMANN MEETING on Recent Developments in Theoretical and Experimental General Relativity: 2594. Bibcode:2008mgm..conf.2594S. doi:10.1142/9789812834300_0469. ISBN 9789812834263.
  16. ↑ Sigismondi, C.; Flatres, T.; George, T.; Braga-Ribas, F. (2014). "Stellar limb darkening scan during 163 Erigone asteroidal occultation of Regulus on March 20, 2014 at 6:06 UT". The Astronomer's Telegram 5987: 1. Bibcode:2014ATel.5987....1S.
  17. ↑ Regulus 2014 International Occultation Timing Association
  18. ↑ Battams, Karl. "Notable objects in LASCO C3". Sungrazing Comets. Navy.mil. Retrieved 2012-09-05.
  19. 1 2 3 McAlister, H. A.; ten Brummelaar, T. A.; Gies; Huang; Bagnuolo, Jr.; Shure; Sturmann; Sturmann; Turner; Taylor; Berger; Baines; Grundstrom; Ogden; Ridgway; Van Belle; et al. (2005). "First Results from the CHARA Array. I. An Interferometric and Spectroscopic Study of the Fast Rotator Alpha Leonis (Regulus)". The Astrophysical Journal 628: 439–452. arXiv:astro-ph/0501261. Bibcode:2005ApJ...628..439M. doi:10.1086/430730.
  20. ↑ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
  21. ↑ Lindroos, K. P. (1985). "A study of visual double stars with early type primaries. IV Astrophysical data". Astronomy and Astrophysics Supplement Series 60: 183. Bibcode:1985A&AS...60..183L.
  22. ↑ Pugh, Philip (2009). "Simple Deep Sky Viewing". The Science and Art of Using Telescopes. Patrick Moore's Practical Astronomy Series. p. 157. doi:10.1007/978-0-387-76470-2_6. ISBN 978-0-387-76469-6.
  23. ↑ Allen, Richard Hinckley (1963). Star Names: Their Lore and Meaning. Dover. pp. 255–6. ISBN 0-486-21079-0.
  24. ↑ Rogers, J. H. (February 1998). "Origins of the ancient constellations: I. The Mesopotamian traditions". Journal of the British Astronomical Association, no.1 108: 9–28. Bibcode:1998JBAA..108....9R.

External links

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Coordinates: 10h 08m 22.3s, +11° 58′ 02″

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