Categories
WASP-52
Topic: Astronomy
From HandWiki - Reading time: 4 min
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 23h 13m 58.7576s[1] |
| Declination | 08° 45′ 40.5713″[1] |
| Apparent magnitude (V) | 12.0 |
| Characteristics | |
| Evolutionary stage | Main sequence |
| Spectral type | K2V[2] |
| Astrometry | |
| Radial velocity (Rv) | −26.604[1] km/s |
| Proper motion (μ) | RA: −6.942[1] mas/yr Dec.: −44.330[1] mas/yr |
| Parallax (π) | 5.7262 ± 0.0134[1] mas |
| Distance | 570 ± 1 ly (174.6 ± 0.4 pc) |
| Details[3] | |
| Mass | 0.87±0.03 M☉ |
| Radius | 0.79±0.02 R☉ |
| Surface gravity (log g) | 4.58±0.01[4] cgs |
| Temperature | 5,000±100 K |
| Metallicity [Fe/H] | 0.03±0.12 dex |
| Rotation | 16±2 d[4] |
| Rotational velocity (v sin i) | 1.77+0.19−0.20[5] km/s |
| Age | 10.7+1.9−4.5 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
WASP-52 is a K-type main-sequence star about 570 light-years away. It is older than the Sun at 10.7+1.9
−4.5 billion years, but it has a similar fraction of heavy elements.[3]
The star has prominent starspot activity, with 3% to 14% of the stellar surface covered by areas 575±150 K cooler than the rest of the photosphere.[6]
A multiplicity survey in 2015 did not detect any stellar companions.[7] The star was named Anadolu in 2019 by Turkish astronomers as part of the NameExoWorlds contest.[8]
Planetary system
In 2012 a transiting hot Jupiter planet, WASP-52b, was detected in a tight, circular orbit.[4] The planet was named Göktürk by Turkish astronomers in December 2019.[8] The planet has a small measured temperature difference between dayside (1481±34 K) and nightside (1224±77 K).[9] Planetary orbit is well aligned with the equatorial plane of the star, the misalignment being 5.47+4.61−4.21°.[5]
Search for transit timing variation did not result in detection of additional planets in system as in 2021.[10]
A transmission spectrum taken in 2020 has revealed the presence of hydrogen, sodium and potassium,[11] although the sodium and potassium lines may be attributable to volcanically active moons of the gas giant, not the planet itself.[12] The atmosphere has no high winds and relatively low-lying clouds, indicating it is not significantly enriched by heavy elements.[13] No signs of the planetary atmosphere escaping to space were detected in 2020,[14] but updated measurement in 2022 showed signs of helium escape, consistent with mass loss rate of 0.5% per billion years.[15]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| WASP-52b (Göktürk) | 0.459+0.022−0.021 MJ | 0.02713+0.00031−0.00032 | 1.7497835±0.0000011 | <0.092 | 85.35±0.20° | 1.27±0.03 RJ |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 2.0 2.1 "WASP-52". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=WASP-52.
- ↑ 3.0 3.1 3.2 Bonomo, A. S.; Desidera, S.; Benatti, S.; Borsa, F.; Crespi, S.; Damasso, M.; Lanza, A. F.; Sozzetti, A. et al. (2017), "The GAPS Programme with HARPS-N@TNG XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets", Astronomy & Astrophysics A107: 602, doi:10.1051/0004-6361/201629882, Bibcode: 2017A&A...602A.107B
- ↑ 4.0 4.1 4.2 Hébrard, G.; Collier Cameron, A.; Brown, D. J. A.; Díaz, R. F.; Faedi, F.; Smalley, B.; Anderson, D. R.; Armstrong, D. et al. (2012), "WASP-52b, WASP-58b, WASP-59b, and WASP-60b: four new transiting close-in giant planets", Astronomy & Astrophysics 549: A134, doi:10.1051/0004-6361/201220363
- ↑ 5.0 5.1 Oshagh, M.; Triaud, A. H. M. J.; Burdanov, A.; Figueira, P.; Reiners, Ansgar; Santos, N. C.; Faria, J.; Boue, G. et al. (2018), "Activity induced variation in spin-orbit angles as derived from Rossiter-McLaughlin measurements", Astronomy & Astrophysics 619: A150, doi:10.1051/0004-6361/201833709, Bibcode: 2018A&A...619A.150O
- ↑ Rosich, A.; Herrero, E.; Mallonn, M.; Ribas, I.; Morales, J. C.; Perger, M.; Anglada-Escudé, G.; Granzer, T. (2020), "Correcting for chromatic stellar activity effects in transits with multiband photometric monitoring: Application to WASP-52", Astronomy and Astrophysics 641: A82, doi:10.1051/0004-6361/202037586, Bibcode: 2020A&A...641A..82R
- ↑ Wöllert, Maria; Brandner, Wolfgang; Bergfors, Carolina; Henning, Thomas (2015), "A Lucky Imaging search for stellar companions to transiting planet host stars", Astronomy & Astrophysics 575: A23, doi:10.1051/0004-6361/201424091, Bibcode: 2015A&A...575A..23W
- ↑ 8.0 8.1 'Anadolu' and 'Göktürk': Turkey names its star and planet
- ↑ May, E. M.; Stevenson, K. B.; Bean, Jacob L.; Bell, Taylor J.; Cowan, Nicolas B.; Dang, Lisa; Desert, Jean-Michel; Fortney, Jonathan J. et al. (2022), "A New Analysis of Eight Spitzer Phase Curves and Hot Jupiter Population Trends: Qatar-1b, Qatar-2b, WASP-52b, WASP-34b, and WASP-140b", The Astronomical Journal 163 (6): 256, doi:10.3847/1538-3881/ac6261, Bibcode: 2022AJ....163..256M
- ↑ Sonbas, E.; Karaman, N.; Özdönmez, A.; Er, H.; Dhuga, K. S.; Göğüş, E.; Nasiroglu, I.; Zejmo, M. (2022), "Probing Transit Timing Variations of three hot Jupiters: HATP-36b, HATP-56b, and WASP-52b", Monthly Notices of the Royal Astronomical Society 509 (4): 5102–5116, doi:10.1093/mnras/stab3270
- ↑ Chen, G.; Casasayas-Barris, N.; Pallé, E.; Yan, F.; Stangret, M.; Cegla, H. M.; Allart, R.; Lovis, C. (2020), "Detection of Na, K, and Hα absorption in the atmosphere of WASP-52b using ESPRESSO", Astronomy & Astrophysics 635: A171, doi:10.1051/0004-6361/201936986, Bibcode: 2020A&A...635A.171C
- ↑ Oza, Apurva V.; Johnson, Robert E.; Lellouch, Emmanuel; Schmidt, Carl; Schneider, Nick; Huang, Chenliang; Gamborino, Diana; Gebek, Andrea et al. (2019), "Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets", The Astrophysical Journal 885 (2): 168, doi:10.3847/1538-4357/ab40cc, Bibcode: 2019ApJ...885..168O
- ↑ Bruno, Giovanni; Lewis, Nikole K.; Alam, Munazza K.; López-Morales, Mercedes; Barstow, Joanna K.; Wakeford, Hannah R.; Sing, David K.; Henry, Gregory W. et al. (2020), "WASP-52b. The effect of starspot correction on atmospheric retrievals", Monthly Notices of the Royal Astronomical Society 491 (4): 5361–5375, doi:10.1093/mnras/stz3194, Bibcode: 2020MNRAS.491.5361B
- ↑ Vissapragada, Shreyas; Knutson, Heather A.; Jovanovic, Nemanja; Harada, Caleb K.; Oklopčić, Antonija; Eriksen, James; Mawet, Dimitri; Millar-Blanchaer, Maxwell A. et al. (2020), "Constraints on Metastable Helium in the Atmospheres of WASP-69b and WASP-52b with Ultra-Narrowband Photometry", The Astronomical Journal 159 (6): 278, doi:10.3847/1538-3881/ab8e34, Bibcode: 2020AJ....159..278V
- ↑ Kirk, James; Dos Santos, Leonardo A.; López-Morales, Mercedes; Alam, Munazza K.; Oklopčić, Antonija; MacLeod, Morgan; Zeng, Li; Zhou, George (2022), "Keck/NIRSPEC Studies of He i in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b", The Astronomical Journal 164 (1): 24, doi:10.3847/1538-3881/ac722f, Bibcode: 2022AJ....164...24K
Coordinates: 
23h 13m 58.7576s, +08° 45′ 40.5713″
 |  |
EncycloReader
is supported by the 
KSF