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HR 4102

Coordinates: Sky map 10h 24m 23.7s, −74° 01′ 54″
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This article is about I Carinae. For i Carinae, see HD 79447. For l Carinae, see HD 84810. For ι Carinae, see Iota Carinae.
HR 4102
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Carina
Right ascension 10h 24m 23.70597s[1]
Declination −74° 01′ 53.8036″[1]
Apparent magnitude (V) 3.99[2]
Characteristics
Spectral type F3 V[3]
U−B color index −0.01[2]
B−V color index +0.36[2]
Astrometry
Radial velocity (Rv)−4.7±0.6[4] km/s
Proper motion (μ) RA: −16.29[1] mas/yr
Dec.: −27.67[1] mas/yr
Parallax (π)61.64 ± 0.12 mas[1]
Distance52.9 ± 0.1 ly
(16.22 ± 0.03 pc)
Absolute magnitude (MV)2.94[5]
Details
Mass1.42[6] M☉
Radius1.592[7] R☉
Luminosity5.015[7] L☉
Surface gravity (log g)4.34[6] cgs
Temperature7,017±239[6] K
Metallicity [Fe/H]+0.02[3] dex
Rotational velocity (v sin i)51.6[8] km/s
Age977[6] Myr
Other designations
I Car, CD−73° 576, GJ 391, HD 90589, HIP 50954, HR 4102, SAO 256710[9]
Database references
SIMBADdata

I Carinae is a single,[10] yellow-white hued star in the southern constellation Carina. It is a fourth[2] magnitude star that is visible to the naked eye. An annual parallax shift of 61.64 mas provides a distance estimate of 62 light years. It is moving closer with a radial velocity of −5 km/s,[4] and in an estimated 2.7 million years will pass within 24.3 ly (7.46 pc) of the Sun.[11] In the next 7500 years, the south Celestial pole will pass close to this star and Omega Carinae (5800 CE).[12]

Gray et al. (2006) gave this star a stellar classification of F3 V,[3] indicating it is an F-type main-sequence star that is generating energy through hydrogen fusion at its core. It is younger than the Sun with an estimated age of 977[6] million years, and is spinning with a projected rotational velocity of 51.6 km/s.[8] The star has 1.4[6] times the mass of the Sun, 1.6[7] times its radius, and is radiating 5.56[5] times the Sun's luminosity from its photosphere at an effective temperature of around 7,017 K.[6] It is a variable star and most likely (99.2% chance) the source of detected X-ray emission coming from these coordinates.[13]

References

[edit]
  1. ^ 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.
  2. ^ a b c d Cousins, A. W. J.; Stoy, R. H. (1962), "Photoelectric magnitudes and colours of Southern stars.", Royal Observatory Bulletin, 64: 103, Bibcode:1962RGOB...64..103C.
  3. ^ a b c Gray, R. O.; et al. (July 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): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
  4. ^ a b Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
  5. ^ a b Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  6. ^ a b c d e f g David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  7. ^ a b c Schofield, Mathew; Chaplin, William J.; Huber, Daniel; Campante, Tiago L.; Davies, Guy R.; Miglio, Andrea; Ball, Warrick H.; Appourchaux, Thierry; Basu, Sarbani; Bedding, Timothy R.; Christensen-Dalsgaard, Jørgen; Creevey, Orlagh; García, Rafael A.; Handberg, Rasmus; Kawaler, Steven D. (2019-03-01), "The Asteroseismic Target List for Solar-like Oscillators Observed in 2 minute Cadence with the Transiting Exoplanet Survey Satellite", The Astrophysical Journal Supplement Series, 241 (1): 12, arXiv:1901.10148, Bibcode:2019ApJS..241...12S, doi:10.3847/1538-4365/ab04f5, ISSN 0067-0049 I Carinae's database entry at VizieR.
  8. ^ a b Schröder, C.; Reiners, Ansgar; Schmitt, Jürgen H. M. M. (January 2009), "Ca II HK emission in rapidly rotating stars. Evidence for an onset of the solar-type dynamo" (PDF), Astronomy and Astrophysics, 493 (3): 1099–1107, Bibcode:2009A&A...493.1099S, doi:10.1051/0004-6361:200810377[permanent dead link]
  9. ^ "I Car". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-01-15.
  10. ^ 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.
  11. ^ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv:1412.3648, Bibcode:2015A&A...575A..35B, doi:10.1051/0004-6361/201425221, S2CID 59039482, A35.
  12. ^ "Precession".
  13. ^ 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, arXiv:0910.3229, Bibcode:2009ApJS..184..138H, doi:10.1088/0067-0049/184/1/138, S2CID 119267456.
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