Astronomy:RT Aurigae

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Short description: Star in the constellation Auriga
RT Aurigae
Auriga constellation map.svg
Red circle.svg
Location of RT Aur (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Auriga
Right ascension  06h 28m 34.08818s[1]
Declination +30° 29′ 34.9296″[1]
Apparent magnitude (V) 5.75[2] (5.00 - 5.82[3])
Characteristics
Spectral type F8Ib[4] (F4Ib - G4Ib[3])
U−B color index 0.5[5]
B−V color index 0.74[2]
Variable type δ Cep[3]
Astrometry
Radial velocity (Rv)20.30[6] km/s
Proper motion (μ) RA: −0.492[1] mas/yr
Dec.: −13.441[1] mas/yr
Parallax (π)1.8153 ± 0.1222[1] mas
Distance1,540 ly
(473[7] pc)
Absolute magnitude (MV)−3.09[7]
Details
Mass4.4[8] M☉
Radius35.1[7] R☉
Luminosity1,186[9] L☉
Surface gravity (log g)1.42[8] cgs
Temperature6,151[9] K
Metallicity0.1[7]
Rotational velocity (v sin i)8.8[10] km/s
Age85[11] Myr
Other designations
48 Aurigae, HD 45412, BD+30°1238, HIP 30827, SAO 59128, HR 2332
Database references
SIMBADdata
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

RT Aurigae (RT Aur, 48 Aurigae) is a yellow supergiant variable star in the constellation Auriga, about 1,500 light years from Earth.

A visual band light curve for RT Aurigae, adapted from Kiss (1998)[12]

RT Aurigae is an F to G type Classical Cepheid variable which varies from magnitude +5.00 to +5.82 with a period of 3.728309 days.[7] The variability was discovered in 1905.[13] It was quickly recognised as a member of the class of Cepheid variables, but their nature was not understood at that time. Radial velocity changes were detected corresponding to the brightness variations, but the idea that these were caused by stellar pulsations and temperature changes was largely dismissed in favour of orbital motions of a binary star.[14] More accurate observations eventually proved beyond doubt that the brightness variations were caused by pulsations in the atmospheres of the stars, with the stars being smallest and hottest near maximum brightness.[15]

RT Aurigae has been suspected to be a spectroscopic binary system, but this has not been confirmed.[16][17] The strongest evidence was found in 2013 using CHARA array optical interferometry. The companion would be 6.7 magnitudes fainter than the supergiant primary, cooler and fainter than an F0 main sequence star. The two stars are separated by 2.1 milli-arc seconds.[18]

References

  1. ↑ 1.0 1.1 1.2 1.3 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 Soubiran, C.; Le Campion, J. -F.; Cayrel De Strobel, G.; Caillo, A. (2010). "The PASTEL catalogue of stellar parameters". Astronomy and Astrophysics 515: A111. doi:10.1051/0004-6361/201014247. Bibcode: 2010A&A...515A.111S. 
  3. ↑ 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. Bibcode: 2009yCat....102025S. 
  4. ↑ Eggleton, P. P.; Tokovinin, A. A. (2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E. 
  5. ↑ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues 2237: 0. Bibcode: 2002yCat.2237....0D. 
  6. ↑ 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. Bibcode: 2006AstL...32..759G. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Groenewegen, M. A. T. (2013). "Baade-Wesselink distances to Galactic and Magellanic Cloud Cepheids and the effect of metallicity". Astronomy & Astrophysics 550: A70. doi:10.1051/0004-6361/201220446. Bibcode: 2013A&A...550A..70G. 
  8. ↑ 8.0 8.1 Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A. et al. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics 628: A94. doi:10.1051/0004-6361/201935765. ISSN 0004-6361. Bibcode: 2019A&A...628A..94A. 
  9. ↑ 9.0 9.1 Turner, D. G. (2010). "The PL calibration for Milky Way Cepheids and its implications for the distance scale". Astrophysics and Space Science 326 (2): 219–231. doi:10.1007/s10509-009-0258-5. Bibcode: 2010Ap&SS.326..219T. 
  10. ↑ De Medeiros, J. R.; Alves, S.; Udry, S.; Andersen, J.; Nordström, B.; Mayor, M. (January 2014). "A catalog of rotational and radial velocities for evolved stars: V. Southern stars⋆⋆⋆". Astronomy & Astrophysics 561: A126. doi:10.1051/0004-6361/201220762. ISSN 0004-6361. Bibcode: 2014A&A...561A.126D. 
  11. ↑ Acharova, I. A.; Mishurov, Yu. N.; Kovtyukh, V. V. (2012). "Galactic restrictions on iron production by various types of supernovae". Monthly Notices of the Royal Astronomical Society 420 (2): 1590–1605. doi:10.1111/j.1365-2966.2011.20161.x. Bibcode: 2012MNRAS.420.1590A. 
  12. ↑ Kiss, Laszlo L. (July 1998). "A photometric and spectroscopic study of the brightest northern Cepheids - I. Observations". Monthly Notices of the Royal Astronomical Society 297 (3): 825. doi:10.1046/j.1365-8711.1998.01559.x. Bibcode: 1998MNRAS.297..825K. 
  13. ↑ Turner, H. H. (1905). "New Variable 47.1905 Aurigae". Astronomische Nachrichten 168 (2): 29–30. doi:10.1002/asna.19051680209. Bibcode: 1905AN....168...29T. https://zenodo.org/record/1424811. 
  14. ↑ Duncan, J. C. (1909). "The Orbits of the Cepheid Variables Y Sagittarii and RT Auriga; with a Discussion of the Possible Causes of this Type of Stellar Variation". Publications of the Astronomical Society of the Pacific 21 (126): 119–136. doi:10.1086/121905. Bibcode: 1909PASP...21..119D. 
  15. ↑ Shapley, H. (1916). "The variations in spectral type of twenty Cepheid variables". Astrophysical Journal 44: 273. doi:10.1086/142295. Bibcode: 1916ApJ....44..273S. 
  16. ↑ Evans, Nancy R. (1992). "A magnitude-limited survey of Cepheid companions in the ultraviolet". Astrophysical Journal 384: 220. doi:10.1086/170865. Bibcode: 1992ApJ...384..220E. 
  17. ↑ Turner, D. G.; Bryukhanov, I. S.; Balyuk, I. I.; Gain, A. M.; Grabovsky, R. A.; Grigorenko, V. D.; Klochko, I. V.; Kosa‐Kiss, A. et al. (2007). "The Period Changes of the Cepheid RT Aurigae". Publications of the Astronomical Society of the Pacific 119 (861): 1247. doi:10.1086/523656. Bibcode: 2007PASP..119.1247T. 
  18. ↑ Gallenne, A.; Mérand, A.; Kervella, P.; Monnier, J. D.; Schaefer, G. H.; Baron, F.; Breitfelder, J.; Le Bouquin, J. B. et al. (2015). "Robust high-contrast companion detection from interferometric observations. The CANDID algorithm and an application to six binary Cepheids". Astronomy & Astrophysics 579: A68. doi:10.1051/0004-6361/201525917. Bibcode: 2015A&A...579A..68G. 



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