Categories
Omicron Lupi
Topic: Astronomy
From HandWiki - Reading time: 3 min
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Lupus |
| Right ascension | 14h 51m 38.30289s[1] |
| Declination | −43° 34′ 31.2965″[1] |
| Apparent magnitude (V) | 4.323[2] (4.84 + 5.27)[3] |
| Characteristics | |
| Spectral type | B5 IV[3] |
| U−B color index | −0.620[2] |
| B−V color index | −0.159[2] |
| Astrometry | |
| Radial velocity (Rv) | +7.30±0.74[4] km/s |
| Proper motion (μ) | RA: −25.20[1] mas/yr Dec.: −27.13[1] mas/yr |
| Parallax (π) | 8.07 ± 0.59[1] mas |
| Distance | 400 ± 30 ly (124 ± 9 pc) |
| Absolute magnitude (MV) | −1.2±0.3[5] |
| Details | |
| Mass | 5.7±0.2[5] M☉ |
| Radius | 3.5[5] R☉ |
| Luminosity | 1,260[5] L☉ |
| Surface gravity (log g) | 4.1±0.1[5] cgs |
| Temperature | 18,000[6] K |
| Rotational velocity (v sin i) | 25[6] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Omicron Lupi (ο Lup) is a binary star[3] in the southern constellation of Lupus. It is a visible to the naked eye with a combined apparent visual magnitude of 4.323.[2] Based upon an annual parallax shift of 8.07 mas as seen from Earth,[1] it is located around 400 light-years from the Sun, give or take 30 light-years. At that distance, the visual magnitude of the system is diminished by an extinction factor of 0.13±0.01 due to interstellar dust.[5] It is a member of the Upper Centaurus–Lupus[8] subgroup of the nearby Scorpius–Centaurus association.[6]
This is a visual binary star system with the components having an angular separation of 0.1 arcsecond.[8] The primary, component A, is a magnitude 4.84 B-type subgiant star with a stellar classification of B5 V.[3] It displays radial velocity variations indicating it has an unseen second companion orbiting at a separation of at least 17 AU with a period of 27 years or more.[6] The spectrum of the primary displays a Zeeman effect indicating a magnetic field with a strength ranging from −94 to 677 G.[6] The visible companion, component B, has a visual magnitude of 5.27.[3]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 Cousins, A. W. J. (1973), "Revised zero points and UBV photometry of stars in the Harvard E and F regions", Memoirs of the Royal Astronomical Society 77: 223–236, Bibcode: 1973MmRAS..77..223C.
- ↑ 3.0 3.1 3.2 3.3 3.4 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 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, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Petit, V. et al. (February 2013), "A magnetic confinement versus rotation classification of massive-star magnetospheres", Monthly Notices of the Royal Astronomical Society 429 (1): 398–422, doi:10.1093/mnras/sts344, Bibcode: 2013MNRAS.429..398P, https://pure.uva.nl/ws/files/1746728/147519_A_magnetic_confinement.pdf.
- ↑ 6.0 6.1 6.2 6.3 6.4 Alecian, E. et al. (December 2011), "First HARPSpol discoveries of magnetic fields in massive stars", Astronomy & Astrophysics 536: 4, doi:10.1051/0004-6361/201118354, L6, Bibcode: 2011A&A...536L...6A.
- ↑ "omi Lup". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=omi+Lup.
- ↑ 8.0 8.1 Chen, Christine H. et al. (September 2012), "A Spitzer MIPS Study of 2.5-2.0 M⊙ Stars in Scorpius–Centaurus", The Astrophysical Journal 756 (2): 24, doi:10.1088/0004-637X/756/2/133, 133, Bibcode: 2012ApJ...756..133C.
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