Nu1 Lupi
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Lupus |
| Right ascension | 15h 22m 08.27124s[1] |
| Declination | −47° 55′ 40.0543″[1] |
| Apparent magnitude (V) | 5.01[2] |
| Characteristics | |
| Spectral type | F6 III-IV[3] |
| U−B color index | +0.04[2] |
| B−V color index | +0.50[2] |
| Astrometry | |
| Proper motion (μ) | RA: −141.19[1] mas/yr Dec.: −132.92[1] mas/yr |
| Parallax (π) | 27.89 ± 0.33[1] mas |
| Distance | 117 ± 1 ly (35.9 ± 0.4 pc) |
| Absolute magnitude (MV) | +2.32[4] |
| Details | |
| Mass | 1.67[5] M☉ |
| Surface gravity (log g) | 3.87±0.10[5] cgs |
| Temperature | 6,447±80[5] K |
| Metallicity [Fe/H] | 0.17±0.05[5] dex |
| Rotational velocity (v sin i) | 2.8±0.2[4] km/s |
| Age | 2.0[5] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Nu1 Lupi (ν1 Lup) is a solitary[7] star in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 5.01.[2] It is a high proper motion star[8] with an annual parallax shift of 27.89[1] mas as seen from Earth, yielding a distance estimate of 117 light years from the Sun.
This is a two[5] billion year old evolved star with a stellar classification of F6 III-IV,[3] indicating that the spectrum has characteristics intermediate between a subgiant and giant star. It is most likely the source of X-ray emission[8] detected at these coordinates with a luminosity of 1.09×1029 erg s−1.[9] The star has an estimated 1.67[5] times the mass of the Sun and is spinning slowly with a projected rotational velocity of 2.8 km/s.[4]
References
- 1 2 3 4 5 6 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, Bibcode:2007A&A...474..653V, arXiv:0708.1752
, doi:10.1051/0004-6361:20078357. - 1 2 3 4 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data, SIMBAD, Bibcode:1986EgUBV........0M.
- 1 2 Gray, R. O.; et al. (2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–70, Bibcode:2006AJ....132..161G, arXiv:astro-ph/0603770 , doi:10.1086/504637.
- 1 2 3 Ammler-von Eiff, M.; Reiners, A. (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: 31, Bibcode:2012A&A...542A.116A, arXiv:1204.2459 , doi:10.1051/0004-6361/201118724, A116.
- 1 2 3 4 5 6 7 Bensby, T.; et al. (2014), "Exploring the Milky Way stellar disk. A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood", Astronomy & Astrophysics, 562 (A71): 28, Bibcode:2014A&A...562A..71B, arXiv:1309.2631 , doi:10.1051/0004-6361/201322631.
- ↑ "nu.01 Lup -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-03-08.
- ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, Bibcode:2008MNRAS.389..869E, arXiv:0806.2878 , doi:10.1111/j.1365-2966.2008.13596.x.
- 1 2 Haakonsen, Christian Bernt; Rutledge, Robert E. (September 2009), "XID II: Statistical Cross-Association of ROSAT Bright Source Catalog X-ray Sources with 2MASS Point Source Catalog Near-Infrared Sources", The Astrophysical Journal Supplement, 184 (1): 138–151, Bibcode:2009ApJS..184..138H, arXiv:0910.3229 , doi:10.1088/0067-0049/184/1/138.
- ↑ Pizzolato, N.; et al. (September 2000), "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases", Astronomy and Astrophysics, 361: 614–628, Bibcode:2000A&A...361..614P.