WASP-63

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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]
Distance 942 ± 3  ly
(288.9 ± 1.0  pc)
Details
Mass 1.10+0.06
−0.04 [5]   M☉
Radius 1.76+0.11
−0.08 [5]   R☉
Luminosity 2.76 [1]   L☉
Surface gravity (log g)4.01±0.03 [6]   cgs
Temperature 5715±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
Age 8.3+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
SIMBAD data

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.

Contents

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 / Regoč0.339±0.03  MJ 0.05417+0.00067
−0.00089		4.3780900±0.0000060.026+0.040
−0.029		87.8±1.3° 1.33±0.24  RJ

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<span class="mw-page-title-main">WASP-4b</span> Extrasolar planet in the constellation Phoenix

WASP-4b is an exoplanet, specifically a hot Jupiter, approximately 891 light-years away in the constellation of Phoenix.

BD-17°63 b, formally named Finlay, is an exoplanet located approximately 112.5 light-years away in the constellation of Cetus, orbiting the 10th magnitude K-type main sequence star BD−17 63. This planet has a minimum mass of 5.1 MJ and orbits at a distance of 1.34 astronomical units from the star. The distance ranges from 0.62 AU to 2.06 AU, corresponding to the eccentricity of 0.54. One revolution takes about 656 days.

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<span class="mw-page-title-main">HAT-P-14b</span> Exoplanet in the constellation of Hercules

HAT-P-14b, officially named Sissi also known as WASP-27b, is an extrasolar planet located approximately 224.2 ± 0.6 parsecs (731.2 ± 2.0 ly) away in the constellation of Hercules, orbiting the 10th magnitude F-type main-sequence star HAT-P-14. This planet was discovered in 2010 by the HATNet Project using the transit method. It was independently detected by the SuperWASP project.

<span class="mw-page-title-main">WASP-43b</span> Extrasolar planet in the constellation Sextans

WASP-43b, formally named Astrolábos, is a transiting planet in orbit around the young, active, and low-mass star WASP-43 in the constellation Sextans. The planet is a hot Jupiter with a mass twice that of Jupiter, but with a roughly equal radius. WASP-43b was flagged as a candidate by the SuperWASP program, before they conducted follow-ups using instruments at La Silla Observatory in Chile, which confirmed its existence and provided orbital and physical characteristics. The planet's discovery was published on April 14, 2011.

WASP-62, formally named Naledi, is a single star about 573 light-years away. It is an F class main-sequence star, orbited by a planet, WASP-62b. The age of WASP-62 is much younger than the Sun at 0.8±0.6 billion years, and it has a metal abundance similar to the Sun.

WASP-61 is a single F-type main-sequence star about 1560 light-years away. The star age is much likely younger than the Sun's at approximately 3.8+1.8
−0.9 billion years. WASP-61 is depleted in heavy elements, having just 40% of the solar abundance of iron.

WASP-69, also named Wouri, is a K-type main-sequence star 164 light-years away. Its surface temperature is 4782±15 K. WASP-69 is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.10±0.01, and is much younger than the Sun at 2 billion years. The data regarding starspot activity of WASP-69 are inconclusive, but spot coverage of the photosphere may be very high.

WASP-75 is a F-type main-sequence star about 980 light-years away. The star is much younger than the Sun at approximately 2.9±0.2 billion years. WASP-75 is similar to the Sun in its concentration of heavy elements.

<span class="mw-page-title-main">Gliese 486</span> Star in constellation of Virgo

Gliese 486, also known as Wolf 437 and formally named Gar, is a red dwarf star 26.4 light-years away in the constellation Virgo. It hosts one known exoplanet.

HD 212771, also named Lionrock, is a solitary star in the southern zodiac constellation Aquarius. It has an apparent magnitude of 7.60, making it readily visible with binoculars but not the naked eye. Parallax measurements place the object at a distance of 364 light years, and is currently receding with a radial velocity of 15 km/s.

LHS 3844 is a red dwarf star located 48.5 light-years away from the Solar System in the constellation of Indus. The star has about 15% the mass and 19% the radius of the Sun. It is a relatively inactive red dwarf with a slow rotation period of about 128 days, though UV flares have been observed. LHS 3844 is orbited by one known exoplanet.

LTT 9779 is a G-type main-sequence star located 264 light-years away from the Solar System in the constellation of Sculptor. The star is about 95% the radius and about the same mass as the Sun, but younger than the Sun at 1.7 billion years old, hence its lower luminosity. It has a temperature of 5,443 K and a rotation period of 45 days. LTT 9779 is orbited by one known exoplanet.

CD−34°8618, also known as KELT-13 or WASP-167, is a yellowish-white hued star located in the southern constellation of Centaurus. It has an apparent magnitude of 10.52, making it readily visible in medium sized telescopes, but not to the naked eye. Based on parallax measurements from the Gaia spacecraft, the object is estimated to be approximately 1,350 light years away from the Solar System. It appears to be drifting closer to it, having a radial velocity of −0.53 km/s.

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
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