RT Andromedae

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Template:Short description

RT Andromedae
File:RT Andromedae system.png
RT Andromedae system.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Andromeda
Right ascension Template:RA[1]
Declination Template:DEC[1]
Apparent magnitude (V) 9.043[2]
Characteristics
Spectral type F8-G0V + K1-3V [3]
Variable type RS CVn
Astrometry
Radial velocity (Rv)Script error: No such module "val".[4] km/s
Proper motion (μ) RA: -7.01[1] mas/yr
Dec.: -20.80[1] mas/yr
Parallax (π)10.1267±0.0424 mas[5]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd 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 Template:Solar radius)
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 Template:Solar mass
Radius1.286 ± 0.011 Template:Solar radius
Temperature6,150 ± 132 K
RT And B
Mass0.837 ± 0.030 Template:Solar mass
Radius0.956 ± 0.012 Template:Solar radius
Temperature4,780 K
Metallicity [Fe/H]{{{metal_fe2}}} dex
Other designations
RT And, GSC 03998-02167, HIP 114484, TYC 3998-2167-1, BD+52° 3383a, GCRV 14555, 2MASS J23111009+5301330
Database references
SIMBADdata

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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]

File:RTAndLightCurve.png
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

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  1. ↑ a b c d Script error: No such module "Citation/CS1". Vizier catalog entry
  2. ↑ Script error: No such module "Citation/CS1".
  3. ↑ a b c d Script error: No such module "Citation/CS1".
  4. ↑ Script error: No such module "Citation/CS1".
  5. ↑ Template:Cite DR2
  6. ↑ a b c d Script error: No such module "Citation/CS1".
  7. ↑ Script error: No such module "Citation/CS1".
  8. ↑ Script error: No such module "Citation/CS1".
  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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Template:Stars of Andromeda


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