V602 Carinae (V602 Car, HD 97671) is a red supergiant and variable star of spectral type of M3 in the constellation Carina. It is one of largest known stars.
Location of V602 Car | |
Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Carina |
Right ascension | 11h 13m 29.9740s[1] |
Declination | −60° 05′ 28.838″[1] |
Apparent magnitude (V) | 8.39[2] (7.6 - 9.1[3]) |
Characteristics | |
Spectral type | M3 Ia-Iab[4] |
U−B color index | +2.59[2] |
B−V color index | +2.52[2] |
Variable type | SRc[3] |
Astrometry | |
Proper motion (μ) | RA: −5.425[5] mas/yr Dec.: 2.183[5] mas/yr |
Parallax (π) | 0.4366 ± 0.0698 mas[5] |
Distance | 1,190[6] pc |
Absolute magnitude (MV) | –4.83 (variable)[6] |
Details | |
Mass | 17.7[7] M☉ |
Radius | 932[8] R☉ |
Luminosity | 125,000 - 131,000[8] L☉ |
Surface gravity (log g) | −0.3±0.16[9] cgs |
Temperature | 3,550±170[8] K |
Other designations | |
Database references | |
SIMBAD | data |
In 2005, V602 Car was calculated to have a bolometric luminosity below 110,000 L☉ and a radius around 860 R☉ based on the assumption of an effective temperature of 3,550 K.[10] A 2015 study derived a slightly higher bolometric luminosity of 138,000+66,000
−45,000 L☉ based on the measured flux and an assumed distance, and a larger radius of 1,050±165 R☉ based on the measured angular diameter and luminosity. An effective temperature of 3,432±280 K was then calculated from the luminosity and radius.[9] More recent measurements based on a Gaia Data Release 2 parallax of 0.4366±0.0698 mas gives a luminosity at 125,000–131,000 L☉ with a corresponding radius of 932 R☉ based on the same effective temperature derived in 2005.[8]
V602 Car has an estimated mass loss rate of 1.9×10−6 M☉ per year.[2] An excess of emission at long wavelengths from this star, as well as a small amount of silicate emission, suggests that it may be enclosed by an extensive cloud of dust.[11]
V602 Car is a semiregular variable star with a maximum brightness range of magnitude 7.6 - 9.1[12] and a period of 635[12] or 672[3] days. Despite the large amplitude of variation, it was only named as a variable star in 2006.[3][12]