Observation data Epoch J2000 Equinox J2000 | |
---|---|
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 | |
Cool primary | |
Evolutionary stage | Red supergiant |
Spectral type | M2Iab [4] |
U−B color index | +0.29 [2] |
B−V color index | +1.41 [2] |
Variable type | Slow irregular variable [3] |
Hot secondary | |
Evolutionary stage | B-type main-sequence star |
Spectral type | B0Ve [4] |
Astrometry | |
Radial velocity (Rv) | +22 [5] km/s |
Proper motion (μ) |
RA: -7
[6]
mas/
yr Dec.: +4 [6] mas/ yr |
Parallax (π) | 1.353 ± 0.144 mas [6] |
Distance | 2720+260 −230 ly (833.4+79.8 −70.4 pc) [7] |
Orbit [8] | |
Period (P) | 9,752 days (26.70 years) |
Eccentricity (e) | 0.46 |
Inclination (i) | 60-80° |
Details | |
Cool primary | |
Mass | 13-20 [8] M☉ |
Radius | 570 [8] R☉ |
Luminosity | 59,800 [8] L☉ |
Temperature | 3,662 [9] K |
Age | 12.6±1.4 [10] Myr |
Hot secondary | |
Mass | 17 [8] M☉ |
Radius | 4.35 [8] R☉ |
Luminosity | 13,800 [8] L☉ |
Temperature | 30,000 [8] K |
Age | 12.6±1.4 [10] Myr |
Other designations | |
Primary: HD 60414 | |
Secondary: HD 60415 | |
Database references | |
SIMBAD | data |
KQ Puppis (KQ Pup) is a spectroscopic binary located about 2,700 light-years from Earth in the constellation Puppis. A red supergiant star and a B-type main-sequence star orbit each other every 27 years. Its apparent magnitude varies between 4.82 and 5.17, making it faintly visible to the naked eye.
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. [8] 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. [8] It shows small amplitude irregular pulsations, and also some variation associated with the orbital motion. [12] 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. [13]
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. [14] Membership is uncertain as it appears to be more distant than the other stars in the cluster. [15]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
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 | |
Cool primary | |
Evolutionary stage | Red supergiant |
Spectral type | M2Iab [4] |
U−B color index | +0.29 [2] |
B−V color index | +1.41 [2] |
Variable type | Slow irregular variable [3] |
Hot secondary | |
Evolutionary stage | B-type main-sequence star |
Spectral type | B0Ve [4] |
Astrometry | |
Radial velocity (Rv) | +22 [5] km/s |
Proper motion (μ) |
RA: -7
[6]
mas/
yr Dec.: +4 [6] mas/ yr |
Parallax (π) | 1.353 ± 0.144 mas [6] |
Distance | 2720+260 −230 ly (833.4+79.8 −70.4 pc) [7] |
Orbit [8] | |
Period (P) | 9,752 days (26.70 years) |
Eccentricity (e) | 0.46 |
Inclination (i) | 60-80° |
Details | |
Cool primary | |
Mass | 13-20 [8] M☉ |
Radius | 570 [8] R☉ |
Luminosity | 59,800 [8] L☉ |
Temperature | 3,662 [9] K |
Age | 12.6±1.4 [10] Myr |
Hot secondary | |
Mass | 17 [8] M☉ |
Radius | 4.35 [8] R☉ |
Luminosity | 13,800 [8] L☉ |
Temperature | 30,000 [8] K |
Age | 12.6±1.4 [10] Myr |
Other designations | |
Primary: HD 60414 | |
Secondary: HD 60415 | |
Database references | |
SIMBAD | data |
KQ Puppis (KQ Pup) is a spectroscopic binary located about 2,700 light-years from Earth in the constellation Puppis. A red supergiant star and a B-type main-sequence star orbit each other every 27 years. Its apparent magnitude varies between 4.82 and 5.17, making it faintly visible to the naked eye.
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. [8] 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. [8] It shows small amplitude irregular pulsations, and also some variation associated with the orbital motion. [12] 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. [13]
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. [14] Membership is uncertain as it appears to be more distant than the other stars in the cluster. [15]