Astronomy:HD 33564

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Short description: Star in the constellation Camelopardalis
HD 33564
Location of HD 33564 (circled in red)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Camelopardalis[1]
Right ascension  05h 22m 33.5306s[2]
Declination +79° 13′ 52.143″[2]
Apparent magnitude (V) 5.08[1]
Characteristics
Evolutionary stage main sequence[2]
Spectral type F7V[3]
U−B color index −0.13
B−V color index 0.506±0.002[1]
Astrometry
Radial velocity (Rv)−11.09(13)[2] km/s
Proper motion (μ) RA: −78.661(67)[2] mas/yr
Dec.: 162.098(77)[2] mas/yr
Parallax (π)48.1098 ± 0.0727[2] mas
Distance67.8 ± 0.1 ly
(20.79 ± 0.03 pc)
Absolute magnitude (MV)3.59[4]
Details
Mass1.29[5] M☉
Radius1.51+0.02
−0.06[6] R☉
Luminosity3.428±0.017[6] L☉
Surface gravity (log g)4.22[5] cgs
Temperature6,396+135
−36[6] K
Metallicity [Fe/H]0.14[5] dex
Rotational velocity (v sin i)14.3[5] km/s
Age1.80[5] 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[7] star with an exoplanetary companion in the northern constellation of Camelopardalis. It has an apparent visual magnitude of 5.08,[1] 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.[2] It is a candidate member of the Ursa Major Moving Group.[8]

Description

This is an ordinary F-type main-sequence star with a stellar classification of F7V,[3] indicating that the star is hotter and more massive than the Sun, giving it a yellow-white hue. The star is about two[5] billion years old and is chromospherically quiet,[9] with a projected rotational velocity of 14.3 km/s. It has about 1.5[6] times the radius and 1.3[5] 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.[5]

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.[9]

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.[10]: 49 

The HD 33564 planetary system[9]
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

  • List of extrasolar planets

References

  1. ↑ 1.0 1.1 1.2 1.3 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A  XHIP record for this object at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  3. ↑ 3.0 3.1 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. doi:10.1086/504637. Bibcode: 2006AJ....132..161G. 
  4. ↑ Huang, W. et al. (2012). "A catalogue of Paschen-line profiles in standard stars". Astronomy & Astrophysics 547: A62. doi:10.1051/0004-6361/201219804. Bibcode: 2012A&A...547A..62H. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 Luck, R. Earle (January 2017). "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants". The Astronomical Journal 153 (1): 19. doi:10.3847/1538-3881/153/1/21. 21. Bibcode: 2017AJ....153...21L. 
  6. ↑ 6.0 6.1 6.2 6.3 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  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. doi:10.1051/0004-6361/201833377. Bibcode: 2018A&A...619A..81H. 
  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. doi:10.1046/j.1365-8711.2001.04781.x. Bibcode: 2001MNRAS.328...45M. 
  9. ↑ 9.0 9.1 9.2 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. doi:10.1051/0004-6361:200500176. Bibcode: 2005A&A...444L..21G. 
  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. doi:10.3847/1538-3881/ae0b62. Bibcode: 2025AJ....170..343H. 

Coordinates: Sky map 05h 22m 33.5319s, +79° 13′ 52.135″



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