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Star in the constellation Lacerta From Wikipedia, the free encyclopedia
V424 Lacertae (V424 Lac) is a red supergiant variable star in the constellation Lacerta. It is a member of the Lacerta OB1 stellar association.
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Lacerta |
Right ascension | 22h 56m 25.99839s[1] |
Declination | +49° 44′ 00.7587″[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: −0.649 mas/yr[1] Dec.: −2.768 mas/yr[1] |
Parallax (π) | 1.4018 ± 0.1129 mas[1] |
Distance | 2,300 ± 200 ly (710 ± 60 pc) |
Absolute magnitude (MV) | −4.27[6] |
Details | |
Mass | 6.8[7] M☉ |
Radius | 288+26 −21[8] R☉ |
Luminosity | 16,600+4,300 −3,400[9] L☉ |
Surface gravity (log g) | +0.50[7] cgs |
Temperature | 3749±49[9] K |
Other designations | |
Database references | |
SIMBAD | data |
The MK spectral type of V424 Lac has been determined to be K5,[3] but it has also been classified as M0.[6] 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.[7]
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