Astronomy:Iota Canis Majoris
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Canis Major |
| Right ascension | 06h 56m 08.2246s[1] |
| Declination | −17° 03′ 15.259″[1] |
| Apparent magnitude (V) | 4.40[2] (4.36 to 4.40)[3] |
| Characteristics | |
| Evolutionary stage | Supergiant |
| Spectral type | B3 Ib[4] or B3 Ib/II[5] |
| U−B color index | −0.74[6] |
| B−V color index | −0.07[6] |
| Astrometry | |
| Radial velocity (Rv) | 41.75±0.43[1] km/s |
| Proper motion (μ) | RA: −3.547[1] mas/yr Dec.: 3.190[1] mas/yr |
| Parallax (π) | 0.9453 ± 0.1857[1] mas |
| Distance | 3,100±130 ly (950±40 pc) |
| Absolute magnitude (MV) | −5.51[7] |
| Details[8] | |
| Mass | 13.7±0.5 M☉ |
| Radius | 32±4 R☉ |
| Luminosity | 52,480 L☉ |
| Surface gravity (log g) | 2.59±0.05 cgs |
| Temperature | 15,600±400 K |
| Metallicity [Fe/H] | −0.17[9] dex |
| Rotational velocity (v sin i) | 30±6 km/s |
| Age | 14.79+1.43 −1.30 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Iota Canis Majoris is a solitary[11] supergiant star in the southern constellation of Canis Major. Its name is a Bayer designation that is Latinized from ι Canis Majoris, and abbreviated Iota CMa or ι CMa. This is a variable star that ranges in apparent visual magnitude from +4.36 to +4.40, which is faintly visible to the naked eye.[3] The distance to this star is approximately 3,100 light years based on spectroscopic measurements.[8] It is drifting further away from the Sun with a radial velocity of +42 km/s.[1]
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 day mean it is no longer considered to be of that type.[2] This star is 15 million years old and is spinning with a projected rotational velocity of 30 km/s. It has 14 times the mass and 32 times the radius of the Sun. Iota Canis Majoris is radiating 52,000 times the luminosity of the Sun from its photosphere at an effective temperature of 15,600 K.[8]
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 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 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.
- ↑ 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.
- ↑ 8.0 8.1 8.2 Weßmayer, D. et al. (December 2022). "Quantitative spectroscopy of B-type supergiants" (in en). Astronomy & Astrophysics 668: A92. doi:10.1051/0004-6361/202243973. ISSN 0004-6361. Bibcode: 2022A&A...668A..92W.
- ↑ 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.
- ↑ "iot CMa". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=iot+CMa.
- ↑ 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.
- ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html.
- ↑ Bodensteiner, J. et al. (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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