Alpha Trianguli
 Location of α Trianguli (circled) |
|
| Observation data Epoch J2000.0 Equinox J2000.0 |
|
|---|---|
| Constellation | Triangulum |
| Right ascension | 01h 53m 04.90710s |
| Declination | +29° 34′ 43.7801″ |
| Apparent magnitude (V) | +3.42 |
| Characteristics | |
| Spectral type | F5III to F6IV + M |
| U−B color index | +0.06 |
| B−V color index | +0.48 |
| Variable type | Ellipsoidal variable |
| Astrometry | |
| Radial velocity (Rv) | –12.6 km/s |
| Proper motion (μ) |
RA: 10.82 mas/yr Dec.: –234.24 mas/yr |
| Parallax (π) | 51.50 ± 0.23mas |
| Distance | 63.3 ± 0.3 ly (19.42 ± 0.09 pc) |
| Absolute magnitude (MV) | 1.98 |
| Details | |
| α Tri A | |
| Mass | 1.70 M☉ |
| Radius | 3.22 R☉ |
| Surface gravity (log g) | 3.91 cgs |
| Temperature | 6,288 K |
| Metallicity [Fe/H] | –0.09 to 0.00 dex |
| Rotational velocity (v sin i) | 81.6 km/s |
| Age | 1.6 Gyr |
| α Tri B | |
| Mass | 0.11 M☉ |
| Other designations | |
Alpha Trianguli (α Trianguli, abbreviated Alpha Tri, α Tri), also named Mothallah, is a binary star in the constellation of Triangulum.
α Trianguli (Latinised to Alpha Trianguli) is the system's Bayer designation.
The system bore the traditional names Ras al Muthallah or Mothallah and Caput Trianguli derived from the Arabic رأس المثلث ra’s al-muθallaθ "the head of the triangle" and its Latin translation. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name Mothallah for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names.
In combination with Beta Trianguli, these stars were called Al Mīzān, which is Arabic for "The Scale Beam".
In Babylonian astronomy, Alpha Trianguli is listed as UR.BAR.RA "The Wolf", bearing the epithet "the seeder of the plough" in the MUL.APIN, listed after "The Plough", the name for a constellation formed of Triangulum plus Gamma Andromedae.
Estimates of the combined stellar classification for this system range from F5III to F6IV, with the luminosity class of 'IV' or 'III' indicating the primary component is a subgiant or giant star, respectively. It is a member of a close binary system—a spectroscopic binary—whose components complete an orbit about their center of mass once every 1.736 days. Because the primary star is rotating rapidly, it has assumed the shape of an oblate spheroid. The ellipsoidal profile of the star, as viewed from Earth, varies over the course of an orbit causing the luminosity to vary in magnitude during the same period. Such stars are termed ellipsoidal variables. Within a few million years, as the primary continues to evolve into a red giant star, the system may become a semi-detached binary with the Roche lobe becoming filled to overflowing.
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