HD 63032

Last updated
c Puppis
NGC 2451 a.jpg
The field of cluster NGC 2451; c Puppis is the brightest star in the frame
Observation data
Epoch J2000       Equinox J2000
Constellation Puppis
Right ascension 07h 45m 15.29613s [1]
Declination −37° 58′ 06.9069″ [1]
Apparent magnitude  (V)3.61 [2]
Characteristics
Spectral type K2.5Ib-IIa（K5IIa） + B9V [3]
Apparent magnitude  (U)7.06 [2]
Apparent magnitude  (B)5.34 [2]
Apparent magnitude  (R)2.26 [2]
Apparent magnitude  (I)1.26 [2]
Apparent magnitude  (J)0.68 [2]
Apparent magnitude  (H)-0.075 ± 0.220 [4]
Apparent magnitude  (K)-0.47 [4]
U−B color index 1.72
B−V color index 1.73
Astrometry
Radial velocity (Rv)16.83 ± 0.14 [5]  km/s
Proper motion (μ)RA: −10.54  mas/yr [1]
Dec.: 5.584  mas/yr [1]
Parallax (π)2.9460 ± 0.1482  mas [1]
Distance 1,114+66.9
−34.2  ly
(341.7+20.5
−19.5  pc) [6]
Details
A
Mass 12.1±1.2 [7]   M☉
Radius 274±14 –301 [8]   R☉
Luminosity 15,152 [9]   L☉
Temperature 3,781 [9]   K
Age 15.8±0.4 [7]   Myr
B
Radius 2.0±0.3 [10]   R☉
Temperature 10,200 ± 300 [10]   K
Other designations
CD −37 3863, CPD −37 1558, HD 63032, HIP 37819, HR 3017, SAO 198398
Database references
SIMBAD data

c Puppis, also known as HD 63032 and HR 3017, is a spectroscopic binary star [3] in the constellation Puppis. Its apparent magnitude is of 3.61, [2] making it the eight-brightest star in Puppis. 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. [10]

The primary component of the system is a red supergiant or bright giant of spectral classification K2.5Ib-IIa. [3] It is twelve times more massive than the Sun, and is estimated 16 million years old. [7] At this evolutionary stage, it has expanded to 280 times the size of the Sun [8] and is 15,000 more luminous. Its surface has cooled to an effective temperature of 3,781  K, [9] giving it a red-orange hue. [11] The secondary component is a late B-type star, about two times the size of the Sun. c Puppis was first discovered to be a spectroscopic binary in 1982, by D. Groote and D. Reimers. [10]

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<span class="mw-page-title-main">Tau Puppis</span> Orange-hued giant star in the southern constellation of Puppis

Tau Puppis, Latinized from τ Puppis, is a star in the southern constellation of Puppis, near the southern constellation boundary with Carina. It is visible to the naked with an apparent visual magnitude of +2.95 and is located at a distance of about 182 light-years from Earth. The variable radial velocity of this system was detected by H. D. Curtis and H. K. Palmer in 1908, based on observations made at the D. O. Mills Observatory. It is a spectroscopic binary star system, with the presence of the secondary component being revealed by the shifts of absorption lines in the spectrum resulting from the Doppler effect. The two components orbit each other with a period of 1,066.0 days and a low eccentricity of 0.090.

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<span class="mw-page-title-main">HD 64440</span> Star in the constellation Puppis

HD 64440, also known as a Puppis, is a spectroscopic binary star in the constellation Puppis. Its apparent magnitude is 3.71. Located around 108 parsecs (350 ly) distant, the primary is a bright giant of spectral type K1.5II and the secondary is an early A-type star. They orbit with a period just under 7 years and eccentricity 0.38.

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

QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.

<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">Chi Puppis</span> Star in the constellation Puppis

χ Puppis, Latinised as Chi Puppis, is a single star in the southern constellation of Puppis. It has a white hue and is faintly visible to the eye at night with an apparent visual magnitude of 4.79. The star is located at a distance of approximately 1,800 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +30 km/s. O. J. Eggen listed this star as a member of the Hyades Stream based on its space motion.

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

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

KQ Puppis 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.

<span class="mw-page-title-main">HD 70555</span> Star in the constellation Puppis

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<span class="mw-page-title-main">HD 61831</span> Star in the constellation Puppis

HD 61831 is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.84 and it is approximately 556 light years away based on parallax.

<span class="mw-page-title-main">20 Puppis</span> Star in the constellation Puppis

20 Puppis is a solitary star in the southern constellation of Puppis. It is visible to the naked eye as a faint, yellow-hued star with an apparent visual magnitude of 4.99. The star lies approximately 990 light years away from the Sun based on parallax. It is receding from the Earth with a heliocentric radial velocity of +16.8 km/s.

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

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

HD 83332 is a solitary, orange hued star located in the southern constellation Antlia. It has an apparent magnitude of 5.68, making it faintly visible to the naked eye if viewed under ideal conditions. The star is located 285 light years away based on its annual parallax shift, but is drifting away with a radial velocity of 30 km/s.

HD 63399 is an orange hued star located in the southern constellation Puppis, the poop deck. It has an apparent magnitude of 6.45, placing it near the limit for naked eye visibility. Based on parallax measurements from Gaia DR3, the object is estimated to be 445 light years distant. It appears to be receding with a spectroscopic radial velocity of 28.5 km/s. At its current distance, HD 63399 is diminished by 0.29 magnitudes due to interstellar dust.

<span class="mw-page-title-main">HD 57197</span> Star in the constellation Puppis

HD 57197, also known as M Puppis or HR 2789, is a suspected astrometric binary located in the southern constellation Puppis, the poop deck. It has an apparent magnitude of 5.84, making it faintly visible to the naked eye under ideal conditions. Based on parallax measurements from the Gaia satellite, the system is estimated to be 629 light years away from the Solar System. The value is poorly constrained, but it appears to be receding with a heliocentric radial velocity of 13 km/s. At its current distance, HD 57197's brightness is diminished by 0.3 magnitudes due to interstellar dust. It has an absolute magnitude of -0.43.

<span class="mw-page-title-main">HD 27022</span> Star in the constellation Camelopardalis

HD 27022, also known as HR 1327, is a star located in the northern circumpolar constellation Camelopardalis. The object has also been designated as 20 H. Camelopardalis, but is not commonly used in modern times. It has an apparent magnitude of 5.27, allowing it to be faintly visible to the naked eye. Based on parallax measurements from Gaia DR3, the star has been estimated to be 347 light years away. It appears to be approaching the Solar System, having a heliocentric radial velocity of −19.5 km/s.

References

  1. 1 2 3 4 5 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.
  2. 1 2 3 4 5 6 7 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 3 Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society . 389 (2): 869–879. arXiv: 0806.2878 . Bibcode:2008MNRAS.389..869E. doi: 10.1111/j.1365-2966.2008.13596.x . S2CID   14878976.
  4. 1 2 Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  5. ↑ Mermilliod, J. C.; Mayor, M.; Udry, S. (2008), "Red giants in open clusters. XIV. Mean radial velocities for 1309 stars and 166 open clusters" (PDF), Astronomy and Astrophysics, 485 (1): 303–314, Bibcode:2008A&A...485..303M, doi: 10.1051/0004-6361:200809664
  6. ↑ 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.
  7. 1 2 3 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011-01-01). "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 . ISSN   0035-8711. c Puppis' database entry at VizieR.
  8. 1 2 Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (2022-01-01). "Stellar and substellar companions from Gaia EDR3. Proper-motion anomaly and resolved common proper-motion pairs". Astronomy and Astrophysics. 657: A7. arXiv: 2109.10912 . Bibcode:2022A&A...657A...7K. doi:10.1051/0004-6361/202142146. ISSN   0004-6361. c Puppis' database entry at VizieR.
  9. 1 2 3 McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012-11-01), "Fundamental parameters and infrared excesses of Hipparcos stars", Monthly Notices of the Royal Astronomical Society, 427: 343–357, arXiv: 1208.2037 , Bibcode:2012MNRAS.427..343M, doi: 10.1111/j.1365-2966.2012.21873.x , ISSN   0035-8711 c Puppis' database entry at VizieR.
  10. 1 2 3 4 Groote, D.; Reimers, D. (1983). "Detection of a late B star companion of the bright cluster giant c Pup = HD 63032". Astronomy and Astrophysics. 119 (2): 319–320. Bibcode:1983A&A...119..319G.
  11. ↑ "The Colour of Stars". Australia National Telescope Facility. 6 March 2024. Retrieved 2024-05-27.
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