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Binary star in the constellation Triangulum From Wikipedia, the free encyclopedia
Beta Trianguli (Beta Tri, β Trianguli, β Tri) is the Bayer designation for a binary star[11] system in the constellation Triangulum, located about 127 light years from Earth.[1] Although it is only a third-magnitude star,[2] it is the brightest star in the constellation Triangulum.[12]
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Triangulum |
Right ascension | 02h 09m 32.62712s[1] |
Declination | +34° 59′ 14.2694″[1] |
Apparent magnitude (V) | +3.00[2] |
Characteristics | |
Spectral type | A5IV[3] |
U−B color index | +0.11[2] |
B−V color index | +0.14[2] |
Astrometry | |
Radial velocity (Rv) | +9.9[4] km/s |
Proper motion (μ) | RA: 149.16[1] mas/yr Dec.: –39.10[1] mas/yr |
Parallax (π) | 25.71 ± 0.34 mas[1] |
Distance | 127 ± 2 ly (38.9 ± 0.5 pc) |
Absolute magnitude (MV) | +0.05[5] |
Orbit[6] | |
Period (P) | 31.3884 d |
Eccentricity (e) | 0.53 |
Periastron epoch (T) | 2432004.255 JD |
Argument of periastron (ω) (secondary) | 318.4° |
Semi-amplitude (K1) (primary) | 33.3 km/s |
Semi-amplitude (K2) (secondary) | 69.2 km/s |
Details | |
Mass | 3.5[7] M☉ |
Luminosity | 74 (combined)[7] L☉ |
Surface gravity (log g) | 3.70[3] cgs |
Temperature | 8,186[3] K |
Rotational velocity (v sin i) | 70[8] km/s |
Age | 0.73[9] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
This is a double-lined spectroscopic binary star system with an orbital period of 31.39 days and an eccentricity of 0.53.[6] The members are separated by a distance of less than 5 AU.[13] The primary component has a stellar classification of A5IV, indicating that it has evolved away from the main sequence and is now a subgiant star. However, the classification is uncertain and not consistent with the mass derived from the orbit.[7] It is among the least variable of the stars that were observed by the Hipparcos spacecraft, with a magnitude varying by only 0.0005.[14]
Based on observations using the Spitzer Space Telescope, as reported in 2005, this system is emitting an excess of infrared radiation. This emission can be explained by a circumbinary ring of dust. The dust is emitting infrared radiation at a blackbody temperature of 100 K.[13] It is thought to extend from 50 to 400 AU away from the stars.[7]