Astronomy:RT Andromedae

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Short description: Star in the constellation Andromeda
RT Andromedae
RT Andromedae system.png
RT Andromedae system.
Observation data
Equinox J2000.0]] (ICRS)
Constellation Andromeda
Right ascension  23h 11m 10.099s[1]
Declination +53° 01′ 33.04″[1]
Apparent magnitude (V) 9.043[2]
Characteristics
Spectral type F8-G0V + K1-3V [3]
Variable type RS CVn
Astrometry
Radial velocity (Rv)0.60±0.6[4] km/s
Proper motion (μ) RA: -7.01[1] mas/yr
Dec.: -20.80[1] mas/yr
Parallax (π)10.1267 ± 0.0424[5] mas
Distance322 ± 1 ly
(98.7 ± 0.4 pc)
Absolute bolometric
magnitude (Mbol)		5.707 / 4.079[6]
Orbit[7][6]
Period (P)0.62893095 ± 0.00000009 d
Semi-major axis (a)0.01787 AU (3.839 R☉)
Eccentricity (e)0.0049 ± 0.0005
Inclination (i)87.26 ± 0.07°
Periastron epoch (T)JD 2436697.857
Details[6]
RT And A
Mass1.088 ± 0.030 M☉
Radius1.286 ± 0.011 R☉
Temperature6,150 ± 132 K
RT And B
Mass0.837 ± 0.030 M☉
Radius0.956 ± 0.012 R☉
Temperature4,780 K
Other designations
RT And, GSC 03998-02167, HIP 114484, TYC 3998-2167-1, BD+52° 3383a, GCRV 14555, 2MASS J23111009+5301330
Database references
SIMBADdata

RT Andromedae is a variable star in the constellation of Andromeda. The system is estimated to be 322 light-years (98.7 parsecs) away.[3]

The Infrared (K band) light curve of RT Andromedae plotted from data presented in Arévalo & Lázaro (1995)[8]

RT Andromedae is classified as a RS Canum Venaticorum variable, a type of close eclipsing binary star. It varies from an apparent visual magnitude of 9.83 at minimum brightness to a magnitude of 8.97 at maximum brightness, with a period of 0.6289216 days.[9] The system consists of a G-type main-sequence star slightly more massive than the Sun, and a K-type main-sequence star slightly less massive; the light curve of this eclipsing binary exhibits secular variations of period and minima.[3]

Presence of a third body

According to Pribulla et al. (2000), the changes in variability could be ascribed to a third object in the system, with even a possible fourth. Its minimum mass is estimated to be 5 percent the mass of the Sun (roughly 50 times the mass of Jupiter), with an orbital period close to 75 years and an eccentricity that is thought to be fairly high (at 0.56).[3] Such an object could likely turn out to be a brown dwarf or even a massive jovian planet. However, a recent paper of Manzoori (2009) noticed that there is a decreasing trend in the orbital period, so magnetic braking could explain better the evolution of this orbital system.[6]

References

  1. ↑ 1.0 1.1 1.2 1.3 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL.  Vizier catalog entry
  2. ↑ Høg, E. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. Bibcode: 2000A&A...355L..27H. 
  3. ↑ 3.0 3.1 3.2 3.3 Pribulla (2000). "Active eclipsing binary RT Andromedae revisited". Astronomy & Astrophysics 362: 169–188. Bibcode: 2000A&A...362..169P. 
  4. ↑ Karataș, Yüksel; Bilir, Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R. et al. (2004). "Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution". Monthly Notices of the Royal Astronomical Society 349 (3): 1069–1092. doi:10.1111/j.1365-2966.2004.07588.x. Bibcode: 2004MNRAS.349.1069K. 
  5. ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. 
  6. ↑ 6.0 6.1 6.2 6.3 Manzoori, D. (2009). "Cyclic Variations of Orbital Period and Long-Term Luminosity in Close Binary RT Andromedae". The Astronomical Journal 138 (6): 1917–1924. doi:10.1088/0004-6256/138/6/1917. Bibcode: 2009AJ....138.1917M. 
  7. ↑ Erdem, A.; Demircan, O.; Güre, M. (2001). "The light and period changes of RT Andromedae". Astronomy & Astrophysics 379 (3): 878. doi:10.1051/0004-6361:20011357. Bibcode: 2001A&A...379..878E. 
  8. ↑ Arevalo, M. J.; Lázaro, C. (September 1995). "Infrared Light Curves and Absolute Parameters of the Active Binary RT Andromedae". The Astronomical Journal 110 (3): 1376. doi:10.1086/117611. Bibcode: 1995AJ....110.1376A. https://ui.adsabs.harvard.edu/abs/1995AJ....110.1376A. Retrieved 11 October 2021. 
  9. ↑ RT And, database entry, Combined General Catalog of Variable Stars (GCVS4.2, 2004 Ed.), N. N. Samus, O. V. Durlevich, et al., CDS ID II/250 Accessed on line 2009-06-22.




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