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HD 52265

Coordinates: Sky map 07h 00m 18.0363s, −05° 22′ 01.783″
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HD 52265 / Citalá
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Monoceros
Right ascension 07h 00m 18.036s[1]
Declination −05° 22′ 01.78″[1]
Apparent magnitude (V) 6.29[2]
Characteristics
Spectral type G0 V[3]
B−V color index 0.572±0.003[2]
Variable type None[4]
Astrometry
Radial velocity (Rv)53.86±0.09[2] km/s
Proper motion (μ) RA: −116.513 mas/yr[1]
Dec.: 80.633 mas/yr[1]
Parallax (π)33.425 ± 0.0223 mas[1]
Distance97.58 ± 0.07 ly
(29.92 ± 0.02 pc)
Absolute magnitude (MV)3.98[2]
Details
Mass1.21±0.02[5] M☉
Radius1.27±0.03[5] R☉
Luminosity2.08±0.01[5] L☉
Surface gravity (log g)4.31±0.03[5] cgs
Temperature6,163±41[5] K
Metallicity [Fe/H]+0.11[4] dex
Rotation12.3±0.15 d[6]
Rotational velocity (v sin i)3.6+0.3
−1.0[6] km/s
Age2.6±0.6[5] Gyr
Other designations
Citalá, BD−05°1910, HD 52265, HIP 33719, HR 2622, SAO 134031[7]
Database references
SIMBADdata

HD 52265 is a star with an orbiting exoplanet companion in the equatorial constellation of Monoceros. It is dimly visible to the naked eye with an apparent visual magnitude of 6.29.[2] The star is located at a distance of 98 light-years based n parallax measurements, and is drifting further away with a heliocentric radial velocity of 54 km/s.[2] It has been given the proper name Citalá, after "river of stars" in the native Nahuat language. The name was selected in the NameExoWorlds campaign by El Salvador, during the 100th anniversary of the IAU.[8][9]

This is a G-type main-sequence star with a stellar classification of G0 V.[3] It is 21% more massive than the Sun and is 27% larger in radius. The star is 2.6 billion years,[5] and is spinning with a rotation period of 12.3 days.[6] It is radiating more than double the luminosity of the Sun from its photosphere at an effective temperature of 6,163 K.[5] The level of chromospheric activity is similar to the Sun.[4]

Planetary system

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In 2000 the California and Carnegie Planet Search team announced the discovery of an extrasolar planet orbiting the star.[4] It was independently discovered by the Geneva Extrasolar Planet Search team.[10][11] The second planet in the system is suspected since 2013.[12] The planet has since been designated Cayahuanca by the IAU, which means "the rock" in the Nahuat language.[9]

The HD 52265 planetary system[13]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b / Cayahuanca ≥1.21±0.05 MJ 0.520±0.009 119.27±0.02 0.27±0.02 — —

See also

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References

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  1. ^ a b c d 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. ^ a b c d e f 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. ^ a b Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars". Michigan Spectral Survey. 5. Bibcode:1999MSS...C05....0H.
  4. ^ a b c d Butler, R. Paul; et al. (2000). "Planetary Companions to the Metal-rich Stars BD -10°3166 and HD 52265". The Astrophysical Journal. 545 (1): 504–511. Bibcode:2000ApJ...545..504B. doi:10.1086/317796.
  5. ^ a b c d e f g h Bonfanti, A.; et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics. 575. A18. arXiv:1411.4302. Bibcode:2015A&A...575A..18B. doi:10.1051/0004-6361/201424951.
  6. ^ a b c Ballot, J.; et al. (2011). "Accurate p-mode measurements of the G0V metal-rich CoRoT target HD 52265". Astronomy and Astrophysics. 530. A97. arXiv:1105.3551. Bibcode:2011A&A...530A..97B. doi:10.1051/0004-6361/201116547.
  7. ^ "HD 52265". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-23.
  8. ^ "Approved names". NameExoworlds. Retrieved 2020-01-02.
  9. ^ a b "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
  10. ^ "Exoplanets Galore!" (Press release). Garching, Germany: European Southern Observatory. April 15, 2000. Retrieved December 30, 2012.
  11. ^ Naef, D.; et al. (2001). "The CORALIE survey for southern extrasolar planets V. 3 new extrasolar planets". Astronomy and Astrophysics. 375 (1): 205–218. arXiv:astro-ph/0106255. Bibcode:2001A&A...375..205N. doi:10.1051/0004-6361:20010841.
  12. ^ Wittenmyer, Robert A.; et al. (2013), "Forever alone? Testing single eccentric planetary systems for multiple companions", The Astrophysical Journal Supplement Series, 208 (1): 2, arXiv:1307.0894, Bibcode:2013ApJS..208....2W, doi:10.1088/0067-0049/208/1/2, S2CID 14109907
  13. ^ Wittenmyer, Robert A.; et al. (2019). "Truly eccentric – I. Revisiting eight single-eccentric planetary systems". Monthly Notices of the Royal Astronomical Society. 484 (4): 5859–5867. arXiv:1901.08471. Bibcode:2019MNRAS.484.5859W. doi:10.1093/mnras/stz290. S2CID 118915974.
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