HD 33564

HD 33564
Location of HD 33564 (circled in red)
Observation data
Epoch J2000      Equinox ICRS
Constellation Camelopardalis
Right ascension 05h 22m 33.5306s
Declination +79° 13′ 52.143″
Apparent magnitude (V) 5.08
Characteristics
Evolutionary stage main sequence
Spectral type F7V
U−B color index −0.13
B−V color index 0.506±0.002
Astrometry
Radial velocity (Rv)−11.09(13) km/s
Proper motion (μ) RA: −78.661(67) mas/yr
Dec.: 162.098(77) mas/yr
Parallax (π)48.1098±0.0727 mas
Distance67.8 ± 0.1 ly
(20.79 ± 0.03 pc)
Absolute magnitude (MV)3.59
Details
Mass1.29 M☉
Radius1.51+0.02
−0.06 R☉
Luminosity3.428±0.017 L☉
Surface gravity (log g)4.22 cgs
Temperature6,396+135
−36 K
Metallicity [Fe/H]0.14 dex
Rotational velocity (v sin i)14.3 km/s
Age1.80 Gyr
Other designations
BD+79°169, GC 6455, GJ 196, HD 33564, HIP 25110, HR 1686, SAO 5496
Database references
SIMBADdata
Exoplanet Archivedata

HD 33564 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.

Description

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.

Possible planetary system

In September 2005, a massive planet was found on an eccentric orbit about the star, based on a small sample of 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 planet has not been confirmed by any subsequent study. Based on the limited data used to detect it and lack of follow-up observations, a 2025 study considered it a dubious planet detection.: 49 

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

See also

References

  1. 1 2 3 4 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. XHIP record for this object at VizieR.
  2. 1 2 3 4 5 6 7 8 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.
  3. 1 2 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. 1 2 3 4 5 6 7 8 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. 1 2 3 4 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. 1 2 3 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.
  10. ↑ Harada, Caleb K.; Dressing, Courtney D.; et al. (December 2025). "SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring". The Astronomical Journal. 170 (6): 343. arXiv:2409.10679. Bibcode:2025AJ....170..343H. doi:10.3847/1538-3881/ae0b62.