This star has a
stellar classification of A1Vnn,[3] which indicates it is an
A-type main sequence star. It has 2.7[6] times the mass of the Sun and nearly double the Sun's radius.[7] Gamma Trianguli is radiating about 33[6] times the luminosity of the Sun from its outer envelope at an
effective temperature of 9,440 K,[8] giving the star a white hue.[12] The star is roughly 300 million years old.[6]
Rotation
It is rotating rapidly, with a
projected rotational velocity of 254 km/s along the equator,[9] which causes the star to take the pronounced shape of an
oblate spheroid like
Altair.[11] Because the inclination of the star's
axial tilt is unknown, this means that the azimuthal equatorial velocity is at least this amount and possibly higher.[9] By comparison, the Sun is a slow rotator with an equatorial azimuthal velocity of 2 km/s.[13] The
doppler shift from the rapid rotation results in very diffuse
absorption lines in the star's spectrum, as indicated by the 'nn' in the classification.[14]
Debris disk
Orbiting the star is a dusty
debris disk with a combined mass of about 2.9 × 10−2 times the mass of the
Earth. This disk can be detected because it is being heated to a temperature of about 75 K by Gamma Trianguli and is radiating this as infrared energy. The disk is separated from the host star by an angle of 2.24
arcseconds, corresponding to a physical radius of 80
AU, or 80 times the separation of the Earth from the Sun.[7]
^
abcJohnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99,
Bibcode:
1966CoLPL...4...99J
^
abCowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406,
Bibcode:
1969AJ.....74..375C,
doi:
10.1086/110819
^Wielen, R.; et al. (1999), "Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions", Veroeffentlichungen des Astronomischen Rechen-Instituts Heidelberg, 35, Veröffentlichungen des Astronomisches Rechen-Institut Heidelberg: 1,
Bibcode:
1999VeARI..35....1W