Mu Leporis

From Wikipedia, the free encyclopedia
Jump to: navigation, search
Mu Leporis
Diagram showing star positions and boundaries of the Lepus constellation and its surroundings
Cercle rouge 100%.svg

Location of μ Lepus (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Lepus
Right ascension 05h 12m 55.90168s[1]
Declination −16° 12′ 19.6885″[1]
Apparent magnitude (V) 3.259[2]
Spectral type B9 IV:HgMn[3]
U−B color index –0.357[2]
B−V color index –0.096[2]
Variable type Suspected α2 CVn[4]
Radial velocity (Rv) +27.7[5] km/s
Proper motion (μ) RA: +47.09[1] mas/yr
Dec.: –16.39[1] mas/yr
Parallax (π) 17.54 ± 0.55[1] mas
Distance 186 ± 6 ly
(57 ± 2 pc)
Absolute magnitude (MV) −0.49[6]
Mass 3.45[7] M
Radius 3.39±0.16[4] R
Luminosity 251[6] L
Surface gravity (log g) 3.85[8] cgs
Temperature 12,820±436[7] K
Metallicity [Fe/H] –0.05[8] dex
Rotational velocity (v sin i) 16±0.5[4] km/s
Age 125[7] Myr
Other designations
μ Lep, 5 Lep, BD−16° 1072, FK5 1144, HD 33904, HIP 24305, HR 1702, SAO 150237[9]
Database references

Mu Leporis, Latinized from μ Leporis, is a star in the southern constellation of Lepus. The apparent visual magnitude is 3.259,[2] making the star visible to the naked eye at night from the southern hemisphere. Parallax measurements yield an estimated distance of 186 light-years (57 parsecs) from the Earth.[1] It is moving further from the Sun with a radial velocity of +27.7 km/s.[5]

The stellar classification of this star is B9 IV:HgMn,[3] although the ':' indicates an uncertain spectral value. The luminosity class of IV indicates that this is a subgiant that has exhausted the hydrogen at its core and it is in the process of evolving into a giant star. At present it has about 3.4 times the Sun's radius,[4] 3.45[7] times the mass of the Sun, and is radiating 251[6] times the Sun's luminosity from its photosphere at an effective temperature of 12,800 K.[8]

Mu Leporis is a suspected Alpha² Canum Venaticorum variable with a period of about two days, although this has not been confirmed. The spectrum of this star shows overabundances of mercury and manganese, as indicated by the HgMn in the stellar class.[4] X-ray emission has been detected coming from a location at an angular separation of 0.93 arcseconds from this star. At the estimated distance of Mu Leporis, this equals a projected distance of 52 Astronomical Units. The source may be a stellar companion: either a star that has not yet reached the main sequence or a small, low-temperature star. The X-ray luminosity of this object is (4.4 ± 0.1) × 10 29 erg s−1.[10]


  1. ^ a b c d e f van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357 
  2. ^ a b c d Gutierrez-Moreno, Adelina; et al. (1966). "A System of photometric standards". 1. Publicaciones Universidad de Chile, Department de Astronomy: 1–17. Bibcode:1966PDAUC...1....1G. 
  3. ^ a b Houk, N.; Smith-Moore, M. (1988), Michigan Catalogue of Two-dimensional Spectral Types for the HD Stars, Volume 4, Declinations -26°.0 to -12°.0, Ann Arbor, MI: Department of Astronomy, University of Michigan, 
  4. ^ a b c d e Kochukhov, O.; et al. (October 2011), "No magnetic field in the spotted HgMn star μ Leporis", Astronomy & Astrophysics, 534: L13, arXiv:1110.0829Freely accessible, Bibcode:2011A&A...534L..13K, doi:10.1051/0004-6361/201117970 
  5. ^ a b Wilson, Ralph Elmer (1953). General Catalogue of Stellar Radial Velocities. Washington: Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W. 
  6. ^ a b c Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971Freely accessible, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015. 
  7. ^ a b c d David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154Freely accessible, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146. 
  8. ^ a b c Smith, K. C.; Dworetsky, M. M. (July 1993), "Elemental Abundances in Normal Late B-Stars and Hgmn-Stars from Co-Added IUE Spectra - Part One - Iron Peak Elements", Astronomy and Astrophysics, 274 (2): 335, Bibcode:1993A&A...274..335S 
  9. ^ "mu. Lep -- Variable Star of alpha2 CVn type", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-09 
  10. ^ Behar, Ehud; et al. (September 2004), "Resolving X-Ray Sources from B Stars Spectroscopically: The Example of μ Leporis", The Astrophysical Journal, 612 (1): L65–L68, arXiv:astro-ph/0407338Freely accessible, Bibcode:2004ApJ...612L..65B, doi:10.1086/424485 

External links[edit]