ι Lupi, Latinised as Iota Lupi, is a solitary[11] star in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 3.54.[2] Based upon an annual parallax shift of 9.65 mas as seen from Earth, it is located around 338 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.23 due to interstellar dust.[5] Relative to its neighbors, this star has a peculiar velocity of 27.4±4.9 km/s.[6] It appears to be a member of the Scorpio-Centaurus OB association.[12]
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Lupus |
| Right ascension | 14h 19m 24.22219s[1] |
| Declination | −46° 03′ 29.1437″[1] |
| Apparent magnitude (V) | 3.54[2] |
| Characteristics | |
| Spectral type | B2.5 IV[3] |
| U−B color index | −0.742[2] |
| B−V color index | −0.180[2] |
| Astrometry | |
| Radial velocity (Rv) | 21.6±4.1[4] km/s |
| Proper motion (μ) | RA: −12.56[1] mas/yr Dec.: −4.76[1] mas/yr |
| Parallax (π) | 9.65 ± 0.20 mas[1] |
| Distance | 338 ± 7 ly (104 ± 2 pc) |
| Absolute magnitude (MV) | −1.48[5] |
| Details | |
| Mass | 6.9±0.1[6] M☉ |
| Radius | 4.05±0.33[7] R☉ |
| Luminosity (bolometric) | 2,082[8] L☉ |
| Surface gravity (log g) | 3.94±0.07[7] cgs |
| Temperature | 18,605±221[7] K |
| Metallicity [Fe/H] | +0.19±0.15[7] dex |
| Rotational velocity (v sin i) | 370[9] km/s |
| Age | 20.3±4.8[6] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
This star has the spectrum of a B-type subgiant star with a stellar classification of B2.5 IV,[3] which may indicate that it has used up its core supply of hydrogen and has begun to expand off the main-sequence. It is rotating rapidly with a projected rotational velocity of 370 km/s.[9] This is giving the star an oblate shape with an equatorial bulge that is an estimated 12% larger than the polar radius.[13] It is about 20[6] million years old with 6.9[6] times the mass of the Sun and 4[7] times the Sun's radius. The star radiates 2,082[8] times the solar luminosity from its outer atmosphere at an effective temperature of 18,605[7] K.
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 Gutierrez-Moreno, Adelina; Moreno, Hugo (June 1968), "A photometric investigation of the Scorpio-Centaurus association", Astrophysical Journal Supplement, 15: 459, Bibcode:1968ApJS...15..459G, doi:10.1086/190168.
- ^ a b Hiltner, W. A.; et al. (July 1969), "MK Spectral Types for Bright Southern OB Stars", Astrophysical Journal, 157: 313–326, Bibcode:1969ApJ...157..313H, doi:10.1086/150069.
- ^ 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.
- ^ a b Gontcharov, G. A. (November 2012), "Spatial distribution and kinematics of OB stars", Astronomy Letters, 38 (11): 694–706, arXiv:1606.09028, Bibcode:2012AstL...38..694G, doi:10.1134/S1063773712110035, S2CID 119108982.
- ^ a b c d e Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
- ^ a b c d e f Fitzpatrick, E. L.; Massa, D. (March 2005), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", The Astronomical Journal, 129 (3): 1642–1662, arXiv:astro-ph/0412542, Bibcode:2005AJ....129.1642F, doi:10.1086/427855, S2CID 119512018.
- ^ a b Hohle, M. M.; et al. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483.
- ^ a b Uesugi, Akira; Fukuda, Ichiro (1970), "Catalogue of rotational velocities of the stars", Contributions from the Institute of Astrophysics and Kwasan Observatory, University of Kyoto, Bibcode:1970crvs.book.....U.
- ^ "iot Lup -- Variable Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-03-05.
- ^ 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ de Geus, E. J.; et al. (June 1989), "Physical parameters of stars in the Scorpio-Centaurus OB association", Astronomy and Astrophysics, 216 (1–2): 44–61, Bibcode:1989A&A...216...44D.
- ^ Belle, G. T. (2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.
External links
edit- Kaler, James B. (August 9, 2013), "Iota Lupi", Stars, University of Illinois, retrieved 2017-03-06.