Observation data Equinox J2000.0]] (ICRS) | |
---|---|
Constellation | Puppis |
Right ascension | 07h 33m 47.96383s[1] |
Declination | −14° 31′ 26.0026″[1] |
Apparent magnitude (V) | +4.97[2] (4.82 - 5.17[3]) |
Characteristics | |
Spectral type | M2Iab + B0Ve[4] |
U−B color index | +0.29[2] |
B−V color index | +1.41[2] |
Variable type | LC[3] |
Astrometry | |
Radial velocity (Rv) | +22[5] km/s |
Proper motion (μ) | RA: -6.584[6] mas/yr Dec.: +3.34[6] mas/yr |
Parallax (π) | 1.4894 ± 0.2296[6] mas |
Distance | approx. 2,200 ly (approx. 700 pc) |
Orbit[7] | |
Period (P) | 9,752 days |
Eccentricity (e) | 0.46 |
Inclination (i) | 60-80° |
Details | |
Cool primary | |
Mass | 13-20[7] M☉ |
Radius | 415[8] R☉ |
Luminosity | 26,500 - 28,100[8] L☉ |
Temperature | 3,662[9][8] K |
Hot secondary | |
Mass | 17[7] M☉ |
Radius | 4.35[7] R☉ |
Luminosity | 13,800[7] L☉ |
Temperature | 30,000[7] K |
Other designations | |
Primary: HD 60414 | |
Secondary: HD 60415 | |
Database references | |
SIMBAD | data |
KQ Puppis (KQ Pup) 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.
The KQ Puppis system consists of a fairly typical M2 supergiant, in orbit with a hotter less luminous star. The hotter star is surrounded by a disc of material being transferred from the cool supergiant. This type of binary is referred to a VV Cephei system, although in this case there are no eclipses of either star.[7] A portion of the disc does appear to be eclipsed and this is detected as a strong drop in far-ultraviolet radiation for about a third of the orbit.[4]
The red supergiant primary star has been compared to Betelgeuse.[7] It shows small amplitude irregular pulsations, and also some variation associated with the orbital motion.[11] The nature of the secondary is less certain. The spectrum shows high excitation features that would indicate an early B or hotter spectral type, but these may be associated with the disc rather than that star itself. Other studies have found a spectrum similar to an A supergiant, but this is thought to be an artefact of a B-type shell star.[12]
KQ Puppis has been catalogued as an outlying member of the open cluster Messier 47 (NGC 2422) and would be the brightest member of that cluster.[13] Membership is uncertain as it appears to be more distant than the other stars in the cluster.[14]
Original source: https://en.wikipedia.org/wiki/KQ Puppis.
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