| |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 23h11m 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 mas[5] |
| Distance | 322 ± 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 | |
| Mass | 1.088 ± 0.030 M☉ |
| Radius | 1.286 ± 0.011 R☉ |
| Temperature | 6,150 ± 132 K |
| RT And B | |
| Mass | 0.837 ± 0.030 M☉ |
| Radius | 0.956 ± 0.012 R☉ |
| Temperature | 4,780 K |
| Other designations | |
RT And, GSC 03998-02167, HIP 114484, TYC 3998-2167-1, BD+52° 3383a, GCRV 14555, 2MASS J23111009+5301330 | |
| Database references | |
| SIMBAD | data |
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]
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]
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]
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 | This variable star–related article is a stub. You can help Wikipedia by expanding it. |
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