RT Aurigae

Last updated
RT Aurigae
Auriga constellation map.svg
Red circle.svg
Location of RT Aur (circled)
Observation data
Epoch J2000       Equinox J2000
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  mas/yr [1]
Dec.: −13.441  mas/yr [1]
Parallax (π)1.8153 ± 0.1222  mas [1]
Distance 473 [7]   pc
Absolute magnitude  (MV)−3.09 [7]
Details
Mass 4.4 [8]   M☉
Radius 35.1 [7]   R☉
Luminosity 1,186 [9]   L☉
Surface gravity (log g)1.42 [8]   cgs
Temperature 6,151 [9]   K
Metallicity 0.1 [7]
Rotational velocity (v sin i)8.8 [10]  km/s
Age 85 [11]   Myr
Other designations
48  Aurigae, HD  45412, BD+30°1238, HIP  30827, SAO  59128, HR  2332
Database references
SIMBAD data
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) RTAurLightCurve.png
A visual band light curve for RT Aurigae, adapted from Kiss (1998)

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]

Related Research Articles

<span class="mw-page-title-main">W Sagittarii</span> Star in the constellation Sagittarius

W Sagittarii is a multiple star system star in the constellation Sagittarius, and a Cepheid variable star.

<span class="mw-page-title-main">X Sagittarii</span> Variable star and possible binary star system in the constellation Sagittarius

X Sagittarii is a variable star and candidate binary star system in the southern constellation of Sagittarius, near the western constellation boundary with Ophiuchus. It has a yellow-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around 4.54. The star is located at a distance of approximately 950 light years from the Sun based on parallax, and is drifting closer with a radial velocity of −10 km/s. The star has an absolute magnitude of around −2.85.

<span class="mw-page-title-main">Pi Aurigae</span> Star in the constellation Auriga

Pi Aurigae, Latinized from π Aurigae, is the Bayer designation for a single, red-hued star in the northern constellation of Auriga. Located about one degree north of the 2nd magnitude star Beta Aurigae, Pi Aurigae is visible to the naked eye with an apparent visual magnitude of 4.25 Based upon parallax measurements, it is approximately 780 light-years away from Earth. At that distance, the brightness of the star is diminished by 0.54 in magnitude from extinction caused by interstellar gas and dust.

<span class="mw-page-title-main">9 Aurigae</span> Multiple star system in the constellation Auriga

9 Aurigae is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 86 light-years from the solar system, although individual Gaia Data Release 3 parallaxes place all three components at 88 light years.

<span class="mw-page-title-main">14 Aurigae</span> Quadruple star system in the constellation Auriga

14 Aurigae is a quadruple star system located 269 light years away from the Sun in the zodiac constellation of Auriga. It has the variable star designation KW Aurigae, whereas 14 Aurigae is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.01. The system is moving closer to the Sun with a heliocentric radial velocity of −9 km/s.

<span class="mw-page-title-main">Phi Aurigae</span> Star in the constellation Auriga

Phi Aurigae, Latinized from φ Aurigae, is a giant star in the northern constellation of Auriga. It is faintly visible to the naked eye with an apparent visual magnitude of 5.089. It lies 10′ from another faint naked-eye star HD 35520, between the three open clusters M36 and M38, and NGC 1893.

<span class="mw-page-title-main">UU Aurigae</span> Star in the constellation of Auriga

UU Aurigae is a carbon star in the constellation Auriga. It is approximately 341 parsecs from Earth.

41 Aurigae is a binary star system located around 310–316 light years away from the Sun in the northern constellation of Auriga. It is visible to the naked eye as a dim, white-hued star with a combined apparent visual magnitude of 5.83. This system is moving further from the Earth with a heliocentric radial velocity of 31 km/s. It is a probable member of the Hyades Supercluster.

<span class="mw-page-title-main">AR Aurigae</span> Binary star system in the constellation Auriga

AR Aurigae, also known by its Flamsteed designation 17 Aurigae, is a binary star in the constellation Auriga. Based on parallax measurements made by the Hipparcos spacecraft, it is approximately 461 light-years from Earth.

<span class="mw-page-title-main">Y Carinae</span> Star in the constellation Carina

Y Carinae is a Classical Cepheid variable, a type of variable star, in the constellation Carina. Its apparent magnitude varies from 7.53 to 8.48.

<span class="mw-page-title-main">V Centauri</span> Variable star in the constellation Centaurus

V Centauri is a Classical Cepheid variable, a type of variable star, in the constellation Centaurus. It is approximately 2,350 light-years away based on parallax.

<span class="mw-page-title-main">FF Aquilae</span> Star and possible star system in the constellation Aquila

FF Aquilae is a classical Cepheid variable star located in the constellation Aquila. It ranges from apparent magnitude 5.18 to 5.51 over a period of 4.470848 days, meaning it is faintly visible to the unaided eye in rural or suburban settings.

<span class="mw-page-title-main">IQ Aurigae</span> Star in the constellation Auriga

IQ Aurigae is a single, variable star in the northern constellation of Auriga. It is visible to the naked eye as a dim, white-hued star with an apparent visual magnitude that fluctuates around 5.38. The star is located at a distance of about 460 light-years from the Sun based on parallax and is drifting further away with a radial velocity of +28.6 km/s.

<span class="mw-page-title-main">V352 Aurigae</span> Star in the constellation Auriga

V352 Aurigae is a variable star in the northern constellation of Auriga. It dimly visible to the naked eye with an apparent visual magnitude that ranges from 6.13 down to 6.18. According to the Bortle scale, it is faintly visible to the naked eye from dark rural skies. The star is located at a distance of approximately 970 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −7 km/s.

<span class="mw-page-title-main">V538 Aurigae</span> Star in constellation Auriga

V538 Aurigae is a single star in the northern constellation of Auriga. With an apparent visual magnitude of 6.23, this star requires good dark sky conditions to view with the naked eye. It is located at a distance of 40.0 light-years (12.3 pc) from Sun based on parallax. The star is drifting further away with a radial velocity of 0.9 km/s. It is a member of the Local Association, and is most likely a thin disk star.

<span class="mw-page-title-main">NO Aurigae</span> Star in the constellation Auriga

NO Aurigae is a pulsating variable star in the constellation Auriga. It is an unusually-luminous asymptotic giant branch star about 3,500 light years away.

HD 102350 is a single star in the constellation Centaurus. It has a yellow hue and is visible to the naked eye with an apparent visual magnitude of 4.11. The distance to this star is approximately 390 light years based on parallax, but it is drifting closer with a radial velocity of −3 km/s. It has an absolute magnitude of −1.51.

<span class="mw-page-title-main">AX Circini</span> Binary star system in the constellation Circinus

AX Circini is a binary star system in the southern constellation of Circinus. It has a nominal magnitude of 5.91, which is bright enough to be visible to the naked eye. Based upon an annual parallax shift of 1.7 mas, it is located roughly 1,900 light-years from the Earth. The system is moving closer with a heliocentric radial velocity of −21 km/s.

<span class="mw-page-title-main">SZ Tauri</span>

SZ Tauri is a variable star in the equatorial constellation of Taurus. The brightness of this star varies from an apparent visual magnitude of 6.39 down to 6.69 with a period of 3.149 days, which is near the lower limit of visibility to the naked eye. The distance to this star is approximately 2,070 light years based on parallax measurements. There is some indication this may be a binary system, but the evidence is inconclusive.

<span class="mw-page-title-main">X Cygni</span> Variable star in the constellation Cygnus

X Cygni is a variable star in the northern constellation of Cygnus, abbreviated X Cyg. This is a Delta Cephei variable that ranges in brightness from an apparent visual magnitude of 5.85 down to 6.91 with a period of 16.386332 days. At it brightest, this star is dimly visible to the naked eye. The distance to this star is approximately 628 light years based on parallax measurements. It is drifting further away with a radial velocity of 8.1 km/s. This star is a likely member of the open cluster Ruprecht 173.

References

  1. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 Soubiran, C.; Le Campion, J. -F.; Cayrel De Strobel, G.; Caillo, A. (2010). "The PASTEL catalogue of stellar parameters". Astronomy and Astrophysics. 515: A111. arXiv: 1004.1069 . Bibcode:2010A&A...515A.111S. doi:10.1051/0004-6361/201014247. S2CID   118362423.
  3. 1 2 3 Samus, 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.
  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. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID   14878976.
  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. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  7. 1 2 3 4 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. S2CID   118665355.
  8. 1 2 Anders, F.; Khalatyan, A.; Chiappini, C.; Queiroz, A. B.; Santiago, B. X.; Jordi, C.; Girardi, L.; Brown, A. G. A.; Matijevič, G.; Monari, G.; Cantat-Gaudin, T.; Weiler, M.; Khan, S.; Miglio, A.; Carrillo, I.; Romero-Gómez, M.; Minchev, I.; de Jong, R. S.; Antoja, T.; Ramos, P.; Steinmetz, M.; Enke, H. (August 2019). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia DR2 stars brighter than G = 18". Astronomy & Astrophysics. 628: A94. arXiv: 1904.11302 . Bibcode:2019A&A...628A..94A. doi: 10.1051/0004-6361/201935765 . ISSN   0004-6361.
  9. 1 2 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. arXiv: 0912.4864 . Bibcode:2010Ap&SS.326..219T. doi:10.1007/s10509-009-0258-5. S2CID   119264970.
  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. arXiv: 1312.3474 . Bibcode:2014A&A...561A.126D. doi: 10.1051/0004-6361/201220762 . ISSN   0004-6361.
  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. arXiv: 1111.2152 . Bibcode:2012MNRAS.420.1590A. doi:10.1111/j.1365-2966.2011.20161.x. S2CID   118404944.
  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. Bibcode:1998MNRAS.297..825K. doi: 10.1046/j.1365-8711.1998.01559.x .
  13. ↑ Turner, H. H. (1905). "New Variable 47.1905 Aurigae". Astronomische Nachrichten. 168 (2): 29–30. Bibcode:1905AN....168...29T. doi:10.1002/asna.19051680209.
  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. Bibcode:1909PASP...21..119D. doi: 10.1086/121905 .
  15. ↑ Shapley, H. (1916). "The variations in spectral type of twenty Cepheid variables". Astrophysical Journal. 44: 273. Bibcode:1916ApJ....44..273S. doi: 10.1086/142295 .
  16. ↑ Evans, Nancy R. (1992). "A magnitude-limited survey of Cepheid companions in the ultraviolet". Astrophysical Journal. 384: 220. Bibcode:1992ApJ...384..220E. doi: 10.1086/170865 .
  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.; Kosinsky, A. S.; Kushmar, I. J.; Mamedov, V. T.; Narkevich, N. A.; Pogosyants, A. J.; Semenyuta, A. S.; Sergey, I. M.; Schukin, V. V.; Strigelsky, J. B.; Tamello, V. G.; Lane, D. J.; Majaess, D. J. (2007). "The Period Changes of the Cepheid RT Aurigae". Publications of the Astronomical Society of the Pacific. 119 (861): 1247. arXiv: 0709.3085 . Bibcode:2007PASP..119.1247T. doi:10.1086/523656. S2CID   18243829.
  18. ↑ Gallenne, A.; Mérand, A.; Kervella, P.; Monnier, J. D.; Schaefer, G. H.; Baron, F.; Breitfelder, J.; Le Bouquin, J. B.; Roettenbacher, R. M.; Gieren, W.; Pietrzyński, G.; McAlister, H.; Ten Brummelaar, T.; Sturmann, J.; Sturmann, L.; Turner, N.; Ridgway, S.; Kraus, S. (2015). "Robust high-contrast companion detection from interferometric observations. The CANDID algorithm and an application to six binary Cepheids". Astronomy & Astrophysics. 579: A68. arXiv: 1505.02715 . Bibcode:2015A&A...579A..68G. doi:10.1051/0004-6361/201525917. S2CID   1118066.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.