WASP-63
Observation data
Epoch J2000      Equinox J2000
Constellation Columba
Right ascension 06h 17m 20.7485s[1]
Declination −38° 19′ 23.754″[1]
Apparent magnitude (V) 11.10±0.08[2]
Characteristics
Evolutionary stage subgiant[1][2]
Spectral type G8[3]
B−V color index 0.741±0.022[4]
J−K color index 0.425±0.032[4]
Astrometry
Radial velocity (Rv)−23.55±0.25[1] km/s
Proper motion (μ) RA: −17.469 mas/yr[1]
Dec.: −27.292 mas/yr[1]
Parallax (π)3.4609 ± 0.0118 mas[1]
Distance942 ± 3 ly
(288.9 ± 1.0 pc)
Details
Mass1.10+0.06
−0.04[5] M☉
Radius1.76+0.11
−0.08[5] R☉
Luminosity2.76[1] L☉
Surface gravity (log g)4.01±0.03[6] cgs
Temperature5715±60[6] K
Metallicity [Fe/H]0.08±0.07 dex[5]
0.28±0.05[6] dex
Rotational velocity (v sin i)2.8±0.5[5] km/s
Age8.3+1.3
−1.2[5] Gyr
Other designations
Kosjenka, CD−38 2551, TOI-483, WASP-63, TYC 7612-556-1, GSC 07612-00556, 2MASS J06172074-3819237[7]
Database references
SIMBADdata

WASP-63 or Kosjenka, also known as CD-38 2551, is a single star with an exoplanetary companion in the southern constellation of Columba. It is too faint to be visible with the naked eye, having an apparent visual magnitude of 11.1.[2] The distance to this system is approximately 942 light-years (289 parsecs) based on parallax measurements, but it is drifting closer with a radial velocity of −24 km/s.

Nomenclature

The designation WASP-63 indicates that this was the 63rd star found to have a planet by the Wide Angle Search for Planets.

In August 2022, this planetary system was included among 20 systems to be named by the third NameExoWorlds project.[8] The approved names, proposed by a team from Croatia, were announced in June 2023. WASP-63 is named Kosjenka and its planet is named Regoč, after characters from Croatian Tales of Long Ago by Ivana Brlić-Mažuranić.[9]

Stellar properties

This is a G-type star with a stellar classification of G8;[3] the luminosity class is currently unknown. The star is much older than the Sun at approximately 8.3+1.3
−1.2 billion years. WASP-63 is slightly enriched in heavy elements, having 120% of the solar abundance of iron.[5] The stellar radius is enlarged for a G8 star,[3] and models suggest it has evolved into a subgiant star.[1] It has 1.1 times the mass of the Sun and is spinning with a projected rotational velocity of 3 km/s.[5]

Planetary system

In 2012 a transiting gas giant planet WASP-63b was detected on a tight, circular orbit.[3] Its equilibrium temperature is 1536±37 K, and measured dayside temperature is 1547±308 K.[10] The planet is similar to Saturn in mass but is highly inflated due to proximity to the parent star. The planetary atmosphere contains water and likely has a high cloud deck of indeterminate composition.[11]

The WASP-63 planetary system[5]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b / Regoč 0.339±0.03 MJ 0.05417+0.00067
−0.00089		 4.3780900±0.000006 0.026+0.040
−0.029		 87.8±1.3° 1.33±0.24 RJ

References

  1. 1 2 3 4 5 6 7 8 9 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. 1 2 3 Santos, N. C.; et al. (August 2013), "SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs. I. New atmospheric parameters and masses for 48 stars with planets", Astronomy & Astrophysics, 556: 11, arXiv:1307.0354, Bibcode:2013A&A...556A.150S, doi:10.1051/0004-6361/201321286, S2CID 55237847, A150.
  3. 1 2 3 4 Hellier, Coel; et al. (2012), "Seven transiting hot-Jupiters from WASP-South, Euler and TRAPPIST: WASP-47b, WASP-55b, WASP-61b, WASP-62b, WASP-63b, WASP-66b & WASP-67b", Monthly Notices of the Royal Astronomical Society, 426 (1): 739–750, arXiv:1204.5095, Bibcode:2012MNRAS.426..739H, doi:10.1111/j.1365-2966.2012.21780.x, S2CID 54713354
  4. 1 2 Brown, D. J. A. (2014), "Discrepancies between isochrone fitting and gyrochronology for exoplanet host stars?", Monthly Notices of the Royal Astronomical Society, 442 (2): 1844–1862, arXiv:1406.4402, Bibcode:2014MNRAS.442.1844B, doi:10.1093/mnras/stu950, S2CID 56052792.
  5. 1 2 3 4 5 6 7 8 Bonomo, A. S.; et al. (2017), "The GAPS Programme with HARPS-N at TNG", Astronomy & Astrophysics, 602: A107, arXiv:1704.00373, Bibcode:2017A&A...602A.107B, doi:10.1051/0004-6361/201629882, S2CID 118923163
  6. 1 2 3 Stassun, Keivan G.; et al. (2016), "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes", The Astronomical Journal, 153 (3): 136, arXiv:1609.04389, Bibcode:2017AJ....153..136S, doi:10.3847/1538-3881/aa5df3, S2CID 119219062
  7. ↑ "CD-38 2551". SIMBAD. Centre de données astronomiques de Strasbourg.
  8. ↑ "List of ExoWorlds 2022". nameexoworlds.iau.org. IAU. 8 August 2022. Retrieved 27 August 2022.
  9. ↑ "2022 Approved Names". nameexoworlds.iau.org. IAU. Retrieved 7 June 2023.
  10. ↑ Garhart, Emily; et al. (2020), "Statistical Characterization of Hot Jupiter Atmospheres Using Spitzer's Secondary Eclipses", The Astronomical Journal, 159 (4): 137, arXiv:1901.07040, Bibcode:2020AJ....159..137G, doi:10.3847/1538-3881/ab6cff, S2CID 119209434
  11. ↑ Kilpatrick, Brian M.; et al. (2017), "Community Targets of JWST's Early Release Science Program: Evaluation of WASP-63b", The Astronomical Journal, 156 (3): 103, arXiv:1704.07421, Bibcode:2018AJ....156..103K, doi:10.3847/1538-3881/aacea7, S2CID 52831173
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.