Astronomy:Iota Canis Majoris
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Canis Major |
| Right ascension | 06h 56m 08.22413s[1] |
| Declination | −17° 03′ 15.2675″[1] |
| Apparent magnitude (V) | 4.40[2] (4.36 - 4.40[3]) |
| Characteristics | |
| Spectral type | B3 Ib[4] or B3 Ib/II[5] |
| U−B color index | −0.74[6] |
| B−V color index | −0.07[6] |
| Variable type | Beta Cephei?[2] |
| Astrometry | |
| Radial velocity (Rv) | +41.20[7] km/s |
| Proper motion (μ) | RA: −3.56 ± 0.17[1] mas/yr Dec.: +2.42 ±0.20[1] mas/yr |
| Parallax (π) | 1.04 ± 0.20[1] mas |
| Distance | approx. 3,100 ly (approx. 1,000 pc) |
| Absolute magnitude (MV) | −5.51[8] |
| Details | |
| Mass | 12.5[9] M☉ |
| Radius | 25.9[8] R☉ |
| Luminosity | 47,000[8] L☉ |
| Surface gravity (log g) | 2.60[10] cgs |
| Temperature | 17,000[10] K |
| Metallicity [Fe/H] | −0.17[11] dex |
| Rotational velocity (v sin i) | 27±4[10] km/s |
| Age | 14.8[9] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Iota Canis Majoris, Latinized from ι Canis Majoris, is a solitary[12] variable supergiant star in the southern constellation of Canis Major. It is visible to the naked eye with an apparent visual magnitude that varies between +4.36 and +4.40.[3] The distance to this star is approximately 3,100 light years based on parallax measurements. It is drifting further away with a radial velocity of +41.2 km/s.[7]
Iota Canis Majoris is a massive blue-white B-type supergiant with a stellar classification of B3 Ib.[4] It has been classified as a Beta Cephei type variable star,[3] but the supergiant spectral type and a period of over a month mean it is no longer considered to be of that type.[2] This star is 14.8[9] million years old and is spinning with a projected rotational velocity of 27 km/s.[10] It has 12.5[9] times the mass and 25.9 times the radius of the Sun.[8] Iota Canis Majoris is radiating 47,000[8] times the luminosity of the Sun from its photosphere at an effective temperature of 17,000 K.[10]
The star displays a bow shock feature from its interaction with the interstellar medium, but this nebulosity is not aligned with the star's motion through the galaxy.[13]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (November 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 Stankov, Anamarija; Handler, Gerald (2005). "Catalog of Galactic β Cephei Stars". The Astrophysical Journal Supplement Series 158 (2): 193–216. doi:10.1086/429408. ISSN 0067-0049. Bibcode: 2005ApJS..158..193S.
- ↑ 3.0 3.1 3.2 Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1: 02025. Bibcode: 2009yCat....102025S.
- ↑ 4.0 4.1 Prinja, R. K.; Massa, D. L. (2010). "Signature of wide-spread clumping in B supergiant winds". Astronomy and Astrophysics 521: L55. doi:10.1051/0004-6361/201015252. ISSN 0004-6361. Bibcode: 2010A&A...521L..55P.
- ↑ Houk, Nancy; Smith-Moore, M. (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. 4. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode: 1988mcts.book.....H.
- ↑ 6.0 6.1 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode: 1986EgUBV........0M.
- ↑ 7.0 7.1 Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. ISSN 1063-7737. Bibcode: 2006AstL...32..759G.
- ↑ 8.0 8.1 8.2 8.3 8.4 Balona, L. A.; Engelbrecht, C. A. (1985). "Photometry and frequency analysis of line profile variables". Monthly Notices of the Royal Astronomical Society 214 (4): 559. doi:10.1093/mnras/214.4.559. Bibcode: 1985MNRAS.214..559B.
- ↑ 9.0 9.1 9.2 9.3 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (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. doi:10.1111/j.1365-2966.2010.17434.x. Bibcode: 2011MNRAS.410..190T.
- ↑ 10.0 10.1 10.2 10.3 10.4 Lefever, K.; Puls, J.; Morel, T.; Aerts, C.; Decin, L.; Briquet, M. (2010). "Spectroscopic determination of the fundamental parameters of 66 B-type stars in the field-of-view of the CoRoT satellite". Astronomy and Astrophysics 515: A74. doi:10.1051/0004-6361/200911956. Bibcode: 2010A&A...515A..74L.
- ↑ Gies, Douglas R.; Lambert, David L. (1992). "Carbon, nitrogen, and oxygen abundances in early B-type stars". Astrophysical Journal 387: 673. doi:10.1086/171116. Bibcode: 1992ApJ...387..673G.
- ↑ 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.
- ↑ Bodensteiner, J.; Baade, D.; Greiner, J.; Langer, N. (October 2018). "Infrared nebulae around bright massive stars as indicators for binary interactions". Astronomy & Astrophysics 618: 13. doi:10.1051/0004-6361/201832722. A110. Bibcode: 2018A&A...618A.110B.
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