Mu Lupi
(Redirected from Μ Lupi)
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Lupus |
| Right ascension | 15h 18m 32.02296s[1] |
| Declination | −47° 52′ 30.9957″[1] |
| Apparent magnitude (V) | 4.29[2] |
| Characteristics | |
| Spectral type | B8 Ve[3] |
| U−B color index | −0.41[2] |
| B−V color index | −0.03[2] |
| Astrometry | |
| Radial velocity (Rv) | +14.90±1.78[4] km/s |
| Proper motion (μ) | RA: −29.59[1] mas/yr Dec.: −35.07[1] mas/yr |
| Parallax (π) | 9.72 ± 0.71 mas[1] |
| Distance | 340 ± 20 ly (103 ± 8 pc) |
| Absolute magnitude (MV) | −0.57[5] |
| Details[3] | |
| Mass | 4.42±0.20 M☉ |
| Luminosity | 603 L☉ |
| Surface gravity (log g) | 3.80±0.10 cgs |
| Temperature | 13,470±500 K |
| Rotational velocity (v sin i) | 280±20 km/s |
| Age | 112 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Mu Lupi (μ Lup) is a system of three or four[7] stars in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 4.29[2] and lies roughly 340 light-years from the Sun.
Two of the components of this system, A and B, form a pair with an angular separation of 1.1 arcseconds. As of 2014, no orbit has been published. Component C lies at an angular separation of 22.6 arcseconds from the AB pair, and may be a common proper motion companion. It is an A-type main-sequence star with a classification of A2 V. A fourth component at an angular separation of 6.15 arcseconds from component A, may be a brown dwarf.[7]
References
[edit]- ^ a b c d e 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, S2CID 18759600.
- ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
- ^ a b Levenhagen, R. S.; Leister, N. V. (2006), "Spectroscopic analysis of southern B and Be stars", Monthly Notices of the Royal Astronomical Society, 371 (1): 252–262, arXiv:astro-ph/0606149, Bibcode:2006MNRAS.371..252L, doi:10.1111/j.1365-2966.2006.10655.x, S2CID 16492030.
- ^ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
- ^ Hubrig, S.; et al. (June 2001), "Search for low-mass PMS companions around X-ray selected late B stars", Astronomy and Astrophysics, 372: 152–164, arXiv:astro-ph/0103201, Bibcode:2001A&A...372..152H, doi:10.1051/0004-6361:20010452, S2CID 17507782.
- ^ "* mu. Lup -- Be Star". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-03-08.
{{cite web}}: CS1 maint: postscript (link) - ^ a b Veramendi, M. E.; González, J. F. (July 2014), "Spectroscopic study of early-type multiple stellar systems. II. New binary subsystems", Astronomy & Astrophysics, 567: 10, arXiv:1405.1084, Bibcode:2014A&A...567A..35V, doi:10.1051/0004-6361/201423736, S2CID 21711755, A35.
