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  • 21 Aug, 2019

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HD 33564
HD 33564 (K Camelopardalis) is a single star with an exoplanetary companion in the northern constellation of Camelopardalis. It has an apparent visual magnitude of 5.08, which means it is a 5th magnitude star that is faintly visible to the naked eye. The system is located at a distance of 68 light years from the Sun based on parallax, and it is drifting closer with a radial velocity of −11 km/s. It is a candidate member of the Ursa Major Moving Group.

This is an ordinary F-type main-sequence star with a stellar classification of F7V, indicating that the star is hotter and more massive than the Sun, giving it a yellow-white hue. The star is about two billion years old and is chromospherically quiet, with a projected rotational velocity of 14.3 km/s. It has about 1.5 times the radius and 1.3 times the mass of the Sun. The star is radiating 3.4 times the luminosity of the Sun from its photosphere at an effective temperature of 6,396 K.

Planetary system

In September 2005, a massive planet was found on an eccentric orbit about the star, based on radial velocity variations measured by the ELODIE spectrograph. An infrared excess had been detected at a wavelength of 60 μm, suggesting the star may host a circumstellar disk. However, the existence of a disk is unlikely because the infrared radiation is coming from a background galaxy.

The HD 33564 planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b >9.1 MJ 1.1 388 ± 3 0.34 ± 0.02 — —

See also

References

  1. ^ 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. ^ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  3. ^ Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
  4. ^ Huang, W.; et al. (2012). "A catalogue of Paschen-line profiles in standard stars". Astronomy & Astrophysics. 547: A62. arXiv:1210.7893. Bibcode:2012A&A...547A..62H. doi:10.1051/0004-6361/201219804. S2CID 119286159.
  5. ^ Luck, R. Earle (January 2017). "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants". The Astronomical Journal. 153 (1): 19. arXiv:1611.02897. Bibcode:2017AJ....153...21L. doi:10.3847/1538-3881/153/1/21. S2CID 119511744. 21.
  6. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  7. ^ Halbwachs, J. -L; et al. (2018). "Multiplicity among solar-type stars. IV. The CORAVEL radial velocities and the spectroscopic orbits of nearby K dwarfs". Astronomy and Astrophysics. 619: A81. arXiv:1808.04605. Bibcode:2018A&A...619A..81H. doi:10.1051/0004-6361/201833377. S2CID 119437322.
  8. ^ Montes, D.; et al. (November 2001). "Late-type members of young stellar kinematic groups - I. Single stars". Monthly Notices of the Royal Astronomical Society. 328 (1): 45–63. arXiv:astro-ph/0106537. Bibcode:2001MNRAS.328...45M. doi:10.1046/j.1365-8711.2001.04781.x. S2CID 55727428.
  9. ^ Galland, F.; et al. (2005). "Extrasolar planets and brown dwarfs around A-F type stars II. A planet found with ELODIE around the F6V star HD 33564". Astronomy and Astrophysics. 444 (2): L21–L24. arXiv:astro-ph/0509112. Bibcode:2005A&A...444L..21G. doi:10.1051/0004-6361:200500176. S2CID 119341964.


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