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HD 95109

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This article is about the variable star: U carinae. For u Carinae, seeHD 94510.
HD 95109
Location of U Carinae (circled)
Observation data
EpochJ2000EquinoxJ2000
Constellation Carina
Right ascension 10h57m48.18690s[1]
Declination −59° 43′ 55.8872″[1]
Apparent magnitude(V) 5.72 - 6.90[2]
Characteristics
Evolutionary stage Yellow supergiant
Spectral type F6-G7 Iab[2]
Variable type δ Cep[2]
Astrometry
Proper motion(μ)RA:−5.963mas/yr[3]
Dec.:+2.397mas/yr[3]
Parallax(π)0.553 ± 0.0226mas[3]
Distance6,187±218ly
(1898±67pc)[4]
Absolute magnitude(MV)−5.27[5]
Details
Mass7.5 - 11.7[6]M☉
Radius187±5[4]R☉
Luminosity26,642±1,584[4]L☉
Surface gravity(logg)1.2[7]cgs
Temperature5,397[4]– 5,980[7]K
Metallicity+0.01[8]
Age29[8]Myr
Other designations
UCar,CD−59°3448,HD95109,HR4276,HIP52589
Database references
SIMBADdata

HD 95109(U Carinae) is aClassical Cepheid variable,a type ofvariablestar,in the constellationCarina.Its apparent magnitude is 6.86.

A near-infrared (J band)light curvefor U Carinae, adpated from Laney and Stobie (1992)[9]

U Car is aδ Cepheid variablewith a period of 38.7681 days. It was one of the earliest Cepheids to be discovered. It has also one of the longest periods, and hence is one of the most luminous in the class.[10]There are still only a few Cepheids with longer periods, includingRS Puppis,SV Vulpeculae,and the unusualS Vulpeculae.[2]

The brightness variation in U Car is caused byfundamental modepulsations. The radius and temperature both vary, with the radius changing by 42R☉during each cycle.[11]The temperature variation causes the spectral type to vary between F6 and G7.

References

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  1. ^abVan 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.S2CID18759600.
  2. ^abcdSamus, N. N.; Durlevich, O. V.; 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.Bibcode:2009yCat....102025S.
  3. ^abVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData Release 3. Summary of the content and survey properties ".Astronomy and Astrophysics.674:A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
  4. ^abcdGallenne, A.; Mérand, A.; Kervella, P.; Pietrzyński, G.; Gieren, W.; Hocdé, V.; Breuval, L.; Nardetto, N.; Lagadec, E. (May 25, 2021). "Extended envelopes around Galactic Cepheids. V. Multi-wavelength and time-dependent analysis of IR excess".Astronomy & Astrophysics.651:A113.arXiv:2105.12197.Bibcode:2021A&A...651A.113G.doi:10.1051/0004-6361/202140350.ISSN0004-6361.
  5. ^Groenewegen, M. A. T. (2013). "Baade-Wesselink distances to Galactic and Magellanic Cloud Cepheids and the effect of metallicity".Astronomy & Astrophysics.550:A70.arXiv:1212.5478.Bibcode:2013A&A...550A..70G.doi:10.1051/0004-6361/201220446.S2CID118665355.
  6. ^Caputo, F.; Bono, G.; Fiorentino, G.; Marconi, M.; Musella, I. (2005). "Pulsation and Evolutionary Masses of Classical Cepheids. I. Milky Way Variables".The Astrophysical Journal.629(2): 1021–1033.arXiv:astro-ph/0505149.Bibcode:2005ApJ...629.1021C.doi:10.1086/431641.S2CID17359646.
  7. ^abRomaniello, M.;Primas, F.;Mottini, M.; Pedicelli, S.; Lemasle, B.; Bono, G.; François, P.; Groenewegen, M. A. T.; Laney, C. D. (2008). "The influence of chemical composition on the properties of Cepheid stars. II. The iron content".Astronomy and Astrophysics.488(2): 731.arXiv:0807.1196.Bibcode:2008A&A...488..731R.doi:10.1051/0004-6361:20065661.S2CID16955805.
  8. ^abMarsakov, V. A.; Koval', V. V.; Kovtyukh, V. V.; Mishenina, T. V. (2013). "Properties of the population of classical Cepheids in the Galaxy".Astronomy Letters.39(12): 851.Bibcode:2013AstL...39..851M.doi:10.1134/S1063773713120050.S2CID119788977.
  9. ^Laney, C. D.; Stobie, R. S. (April 1992)."JHKL Observations of Galactic Cepheids".Astronomy & Astrophysics Supplement Series.93:93–120.Bibcode:1992A&AS...93...93L.Retrieved20 November2021.
  10. ^Shapley, H. (1918). "Studies based on the colors and magnitudes in stellar clusters. VIII. The luminosities and distances of 139 Cepheid variables".Astrophysical Journal.48:279.Bibcode:1918ApJ....48..279S.doi:10.1086/142435.
  11. ^Laney, C. D.; Stobie, R. S. (1995)."The radii of Galactic Cepheids".Monthly Notices of the Royal Astronomical Society.274(2): 337.Bibcode:1995MNRAS.274..337L.doi:10.1093/mnras/274.2.337.
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