Mu Leporis, Latinized from μ Leporis, is a star in the southern constellation of Lepus. The apparent visual magnitude is 3.259, making the star visible to the naked eye at night from the southern hemisphere. Parallax measurements yield an estimated distance of 170 light-years (52 parsecs) from the Earth. It is moving further from the Sun with a radial velocity of +27.7km/s.
The stellar classification of this star is B9IV: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 12,800K.[8]
Mu Leporis is a suspected Alpha² Canum Venaticorum variable with a period of 2.933 days.[11] The stellar 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 0.93arcseconds from this star. At the estimated distance of Mu Leporis, this equals a projected distance of 52Astronomical 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.[12]
Gutierrez-Moreno, Adelina; etal. (1966). "A System of photometric standards". Publications of the Department of Astronomy University of Chile. Publicaciones Universidad de Chile, Department de Astronomy. 1: 1–17. Bibcode:1966PDAUC...1....1G.
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. Bibcode:1988mcts.book.....H.
Wilson, Ralph Elmer (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Washington: Carnegie Institution of Washington. Bibcode:1953GCRV..C......0W.
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:1501.03154. Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146. S2CID33401607.
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.
Kochukhov, O.; Khalack, V.; Kobzar, O.; Neiner, C.; Paunzen, E.; Labadie-Bartz, J.; David-Uraz, A. (October 2021). "TESS survey of rotational and pulsational variability of mercury–manganese stars". Monthly Notices of the Royal Astronomical Society. 506 (4): 5328–5344.
Behar, Ehud; etal. (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/0407338. Bibcode:2004ApJ...612L..65B. doi:10.1086/424485. S2CID18006589.
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