Astronomy:HD 52265

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Short description: Star in the constellation Monoceros
HD 52265 / Citalá
Observation data
Equinox J2000.0]] (ICRS)
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[1] mas/yr
Dec.: 80.633[1] mas/yr
Parallax (π)33.425 ± 0.0223[1] mas
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 has a 27% greater girth. 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

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

  • List of extrasolar planets

References

  1. ↑ 1.0 1.1 1.2 1.3 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.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. 
  3. ↑ 3.0 3.1 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. ↑ 4.0 4.1 4.2 4.3 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. doi:10.1086/317796. Bibcode: 2000ApJ...545..504B. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 Bonfanti, A. et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics 575: A18. doi:10.1051/0004-6361/201424951. Bibcode: 2015A&A...575A..18B. 
  6. ↑ 6.0 6.1 6.2 Ballot, J. et al. (2011). "Accurate p-mode measurements of the G0V metal-rich CoRoT target HD 52265". Astronomy and Astrophysics 530: A97. doi:10.1051/0004-6361/201116547. Bibcode: 2011A&A...530A..97B. 
  7. ↑ "HD 52265". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+52265. 
  8. ↑ "Approved names" (in en). http://www.nameexoworlds.iau.org/final-results. 
  9. ↑ 9.0 9.1 "International Astronomical Union | IAU". https://www.iau.org/news/pressreleases/detail/iau1912/. 
  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. doi:10.1051/0004-6361:20010841. Bibcode: 2001A&A...375..205N. 
  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, doi:10.1088/0067-0049/208/1/2, Bibcode: 2013ApJS..208....2W 
  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. doi:10.1093/mnras/stz290. Bibcode: 2019MNRAS.484.5859W. 

External links

Coordinates: Sky map 07h 00m 18.0363s, −05° 22′ 01.783″



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