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]
Lambda Ursae Minoris is a star in the constellation Ursa Minor. It is an M-type red giant with an apparent magnitude of +6.38 and is approximately 880 light years from Earth.
Sigma Canis Majoris, also named Unurgunite, is a variable star in the southern constellation of Canis Major. It is approximately 1,120 light-years from the Sun and has an average apparent visual magnitude of +3.41.
V533 Carinae is a white A-type supergiant variable star with a mean apparent magnitude of +4.59 in the constellation Carina. It is over 10,000 light years from Earth.
DL Crucis is a variable star in the constellation Crux.
V385 Andromedae is a variable star in the constellation Andromeda, about 360 parsecs (1,200 ly) away. It is a red giant over a hundred times larger than the sun. It has an apparent magnitude around 6.4, just about visible to the naked eye in ideal conditions.
NO Aurigae is a pulsating variable star in the constellation Auriga. It is an unusually-luminous asymptotic giant branch star about 3,500 light years away.
89 Herculis is a binary star system located about 4,700 light years away from the Sun in the northern constellation of Hercules. It is visible to the naked eye as a faint, fifth magnitude star. The system is moving closer to the Earth with a heliocentric radial velocity of −28.5 km/s.
V381 Cephei is a triple star system in the northern constellation of Cepheus. Its apparent magnitude is slightly variable between 5.5 and 5.7.
5 Lacertae is a spectroscopic binary in the constellation Lacerta. Its apparent magnitude is 4.36.
10 Lacertae is a star in the constellation Lacerta. With an apparent magnitude of 4.9, it is located around 700 parsecs (2,300 ly) distant in the small Lacerta OB1 association. It is a hot blue main-sequence star of spectral type O9V, a massive star that is currently fusing its core hydrogen. It is a suspected Beta Cephei variable star.
Sigma Ophiuchi, Latinized from σ Ophiuchi, is a single, orange-hued star in the equatorial constellation Ophiuchus. Its apparent visual magnitude is 4.31, which is bright enough to be faintly visible to the naked eye. The annual parallax shift of 3.62 mas as seen from Earth provides a distance estimate of roughly 900 light years. It is moving closer to the Sun with a radial velocity of −28 km/s.
KQ Puppis is a spectroscopic binary variable star in the constellation Puppis. A red supergiant star and a hot main sequence star orbit each other every 9,742 days. Its apparent magnitude varies between 4.82 and 5.17.
V1073 Scorpii is a variable star in the constellation Scorpius. It has a non-Greek Bayer designation of k Scorpii. The star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +4.87. Parallax measurements yield a distance estimate of approximately 2,920 ly (896 pc) from the Sun, and it is drifting further away with a radial velocity of +7 km/s. It has an absolute magnitude of −6.8
10 Persei is a blue supergiant star in the constellation Perseus. Its apparent magnitude is 6.26 although it is slightly variable.
QU Normae, also known as HR 6131, is a blue supergiant star in the constellation Norma. It is also a variable star, thought to be an α Cyg variable.
3 Geminorum is a blue supergiant star in the constellation Gemini. It is a small amplitude pulsating variable and a close double star, with a mean combined apparent visual magnitude of about 5.7.
RW Cygni is a semiregular variable star in the constellation Cygnus, about a degree east of 2nd magnitude γ Cygni. Its apparent magnitude varies between 8.05 and 9.70 and its spectral type between M3 and M4.
BI Cygni(BI Cyg, IRC +40408, BD+36 4025) is a red supergiant in the constellation Cygnus. It is an irregular variable star with a maximum brightness of magnitude 8.4 and a minimum of magnitude 9.9. It is considered a member of the stellar Cygnus OB1 association, its distance is around 2,600 parsecs (8,500 ly) of the Solar System. It is less than a degree south of another variable red supergiant, BC Cygni.
U Lacertae is a spectroscopic binary star in the constellation Lacerta.
V538 Carinae is a variable star in the constellation of Carina, and a possible red supergiant. If this star replaced the Sun in the Solar System, its photosphere would at least engulf the orbit of Mars.