j Centauri
11h49m 41.05745s[1]
−63° 47′ 18.4299″[1]
Characteristics
B3V[4]
U−B color index
−0.59
B−V color index
−0.15
Radial velocity (Rv)
+29.0±4.1[2] km/s
Proper motion (μ)
RA: -20.76 ± 0.56[5] mas/yr
Dec.: 4.30 ± 0.48[5] mas/yr
Parallax (π)
Absolute magnitude (MV)
−1.98[2]
Details
Surface gravity (log g)
Rotational velocity (v sin i)
200±4[8] km/s
Database references
HD 102776, also known by its Bayer designation j Centauri, is a suspected astrometric binary[10] star system in the southern constellationofCentaurus. It has a blue-white hue and is faintly visible to the naked eye with a typical apparent visual magnitude of 4.30.[2] The distance to this star is approximately 600 light years based on parallax, and it is drifting further away with a radial velocity of ~29 km/s.[2] It is a member of the Lower Centaurus Crux subgroup of the Sco OB2 association.[11] HD 102776 has a relatively large peculiar velocityof31.1 km/s and is a candidate runaway star that was ejected from its association, most likely by a supernova explosion.[12]
The stellar classification of the visible component is B3V,[4] matching a B-type main-sequence star. It is around 32[7] million years old and is spinning rapidly with estimates of its projected rotational velocity ranging from 200[8] up to 270 km, giving it an equatorial bulge that is up to 11% larger than the polar radius.[13] This is a Be star showing emission features in its Balmer lines due to a circumstellar disk of decreated gas.[14] It is classified as a suspected Gamma Cassiopeiae type variable star with a visual magnitude varying from +4.30 down to +4.39.[3]
Other
Other