KQ Puppis

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KQ Puppis
M47 tel114.png
KQ Puppis is the bright red star on the right, with Messier 47 on the left.
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☉
Luminosity13,800 [8]   L☉
Temperature 30,000 [8]   K
Age 12.6±1.4 [10]   Myr
Other designations
KQ Pup, BD −14°1971, HIP  36773, HR  2902, NGC  2422 9, SAO  153072
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]

A light curve for KQ Puppis, plotted from Hipparcos data KQPupLightCurve.png
A light curve for KQ Puppis, plotted from Hipparcos data

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]

Related Research Articles

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<span class="mw-page-title-main">HD 63032</span> Binary star system in the constellation Puppis

c Puppis, also known as HD 63032 and HR 3017, is a spectroscopic binary star in the constellation Puppis. Its apparent magnitude is 3.61. Located around 347 parsecs (1,130 ly) distant, the primary is an orange-red bright giant or supergiant of spectral type K2.5Ib-IIa or K5IIa, while the secondary, discovered in 1983, is a blue main-sequence star of spectral type B9V. The system is the brightest member of the open cluster NGC 2451, over two magnitudes brighter than every other star in the cluster. As the turnoff point of the cluster is currently around B7, the parameters of the system fit with cluster membership.

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<span class="mw-page-title-main">1 Puppis</span> Star in the constellation Puppis

1 Puppis is a single star in the southern constellation of Puppis. It lies in the northern part of the constellation at a distance of about 790 ly, east of Aludra in Canis Major and just north of the white supergiant, 3 Puppis. This object is visible to the naked eye as a faint, red-hued star with an apparent visual magnitude of 4.59. It is moving further from the Earth with a heliocentric radial velocity of +32.4 km/s.

<span class="mw-page-title-main">V1073 Scorpii</span> Variable star in the constellation Scorpius

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<span class="mw-page-title-main">DS Crucis</span> Star in the constellation Crux

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<span class="mw-page-title-main">BU Crucis</span> Star in the constellation Crux

BU Crucis is a variable star in the open cluster NGC 4755, which is also known as the Kappa Crucis Cluster or Jewel Box Cluster.

<span class="mw-page-title-main">DU Crucis</span> Star in the constellation Crux

DU Crucis is a red supergiant and slow irregular variable star in the open cluster NGC 4755, which is also known as the Kappa (κ) Crucis Cluster or Jewel Box Cluster.

<span class="mw-page-title-main">MZ Puppis</span> Red supergiant star in the constellation of Puppis

MZ Puppis is a red supergiant star in the constellation of Puppis. It has a radius of 400 R☉.

<span class="mw-page-title-main">R Puppis</span> Variable star in the constellation Puppis

R Puppis is a variable star in the constellation Puppis. It is a rare yellow hypergiant and a candidate member of the open cluster NGC 2439. It is also an MK spectral standard for the class G2 0-Ia.

References

  1. 1 2 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600.
  2. 1 2 3 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
  3. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1: 02025. Bibcode:2009yCat....102025S.
  4. 1 2 3 González-Riestra, R.; Rossi, C.; Viotti, R. F. (2003). "First far-UV observations of KQ Puppis with FUSE". Astronomy and Astrophysics. 399 (2): 681. Bibcode:2003A&A...399..681G. doi: 10.1051/0004-6361:20021830 .
  5. ↑ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington: 0. Bibcode:1953GCRV..C......0W.
  6. 1 2 3 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  7. ↑ Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (2021-03-01). "Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3". The Astronomical Journal. 161 (3): 147. arXiv: 2012.05220 . Bibcode:2021AJ....161..147B. doi: 10.3847/1538-3881/abd806 . ISSN   0004-6256. Data about this star can be seen here.
  8. 1 2 3 4 5 6 7 8 9 10 Rossi, C.; Altamore, A.; Baratta, G. B.; Friedjung, M.; Viotti, R. (1992). "The spectrum of the VV Cephei star KQ Puppis (Boss 1985). III - A possible model". Astronomy and Astrophysics. 256: 133. Bibcode:1992A&A...256..133R.
  9. ↑ McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012). "Fundamental parameters and infrared excesses of Hipparcos stars". Monthly Notices of the Royal Astronomical Society. 427: 343. arXiv: 1208.2037 . Bibcode:2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x.
  10. 1 2 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1): 190–200. arXiv: 1007.4883 . Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID   118629873. KQ Puppis' database entry at VizieR.
  11. ↑ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  12. ↑ Viotti, R.; Rossi, C.; Muratorio, G. (1998). "Optical and near-IR observations of variable stars with AURELIE". Astronomy and Astrophysics Supplement. 128 (3): 447. Bibcode:1998A&AS..128..447V. doi: 10.1051/aas:1998156 .
  13. ↑ Parsons, Sidney B.; Ake, Thomas B. (1998). "Ultraviolet and Optical Studies of Binaries with Luminous Cool Primaries and Hot Companions. V. The Entire IUE Sample". The Astrophysical Journal Supplement Series. 119 (1): 83. Bibcode:1998ApJS..119...83P. doi: 10.1086/313152 .
  14. ↑ Van Schewick, H. (1966). "Untersuchungen uber die Eigenbewegungen von Sternhaufen. XII. NGC 2422, NGC 2423, NGC 7209 und An. Bakhatova I im Sel. Area 40". Veroeff. Univ. Sternw. Bonn. 74: 1. Bibcode:1966VeBon..74....1V.
  15. ↑ Baumgardt, H.; Dettbarn, C.; Wielen, R. (2000). "Absolute proper motions of open clusters. I. Observational data". Astronomy and Astrophysics Supplement. 146 (2): 251. arXiv: astro-ph/0010306 . Bibcode:2000A&AS..146..251B. doi:10.1051/aas:2000362. S2CID   7180188.
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