Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Lacerta |
Right ascension | 22h 56m 25.997s[1] |
Declination | +49° 44′ 00.716″[1] |
Apparent magnitude (V) | +4.94[2] |
Characteristics | |
Spectral type | K5 Ib[3] |
U−B color index | +1.95[2] |
B−V color index | +1.77[2] |
Variable type | Lc[4] |
Astrometry | |
Radial velocity (Rv) | −9.50[5] km/s |
Proper motion (μ) | RA: −0.709 ± 0.298[6] mas/yr Dec.: −2.317 ± 0.294[6] mas/yr |
Parallax (π) | 1.5762 ± 0.1858 mas[6] |
Distance | approx. 2,100 ly (approx. 630 pc) |
Absolute magnitude (MV) | −4.27[7] |
Details | |
Mass | 6.8[8] M☉ |
Radius | 274+4 −3[9] R☉ |
Luminosity | 13,100 - 14,200[1] L☉ |
Surface gravity (log g) | +0.50[8] cgs |
Temperature | 3,790[1] K |
Other designations | |
Database references | |
SIMBAD | data |
V424 Lacertae (V424 Lac) is a red supergiant variable star in the constellation Lacerta. It is a member of the Lacerta OB1 stellar association.
The MK spectral type of V424 Lac has been determined to be K5,[3] but it has also been classified as M0.[7] It was discovered to be slightly variable using analysis of Hipparcos photometry. The total range is less than a tenth of a magnitude.[11] Multiple short periods are detected, as well as slow variations with a period of 1,100 or 1,601 days. Although listed in the General Catalogue of Variable Stars as a slow irregular variable, it has been considered to be either a semiregular variable or long secondary period variable.[10]
There is an ultraviolet excess from V424 Lacertae, that may be due to an unseen companion, which could also explain the long secondary period. On this assumption, a sub-stellar companion in a 1,382 day 6.2 AU orbit has been suggested.[8]