WASP-29

Last updated
WASP-29
Observation data
Epoch J2000       Equinox J2000
Constellation Phoenix
Right ascension 23h 51m 31.08391s [1]
Declination −39° 54′ 24.2582″ [1]
Apparent magnitude  (V)11.33 [2]
Characteristics
WASP-29A
Evolutionary stage main sequence star
Spectral type K4V [3]
B−V color index 0.82
J−H color index 0.478
J−K color index 0.570
WASP-29B
Spectral type M3V [3]
Astrometry
Radial velocity (Rv)24.31±0.20 [1]  km/s
Proper motion (μ)RA: −56.767(14)  mas/yr [1]
Dec.: −88.988(13)  mas/yr [1]
Parallax (π)11.4349 ± 0.0151  mas [1]
Distance 285.2 ± 0.4  ly
(87.5 ± 0.1  pc)
Position (relative to WASP-29A) [3]
ComponentWASP-29B
Epoch of observation 2021
Angular distance 125.2″
Projected separation 10994 AU
Details [4]
WASP-29A
Mass 0.825±0.033  M☉
Radius 0.808±0.044  R☉
Surface gravity (log g)4.5±0.2  cgs
Temperature 4800±150  K
Metallicity [Fe/H]0.11±0.14  dex
Rotational velocity (v sin i)1.50±0.60 km/s
Age 14+0
−7  Gyr
WASP-29B
Mass 0.38 [3]   M☉
Other designations
CD−40 15273, TOI-192, TIC  183537452, WASP-29, TYC  8015-1020-1, 2MASS J23513108-3954241, DENIS J235131.0-395423 [2]
WASP-29A: Gaia DR3 6534414719318886144
WASP-29B: Gaia DR3 6534426740931264896
Database references
SIMBAD data

WASP-29 is a binary star system 285 light-years (87 parsecs ) away in the constellation of Phoenix. The primary star is a K-type main-sequence star. Its comoving companion, a red dwarf star, was discovered in 2021. [3] The star system kinematically belongs to the thin disk of the Milky Way. [5] The primary is an old star with small starspot activity and low x-ray flux. [6]

Planetary system

The "hot Saturn" class planet WASP-29b was discovered around WASP-29 in 2010. [5] The planet would have an equilibrium temperature of 960±30 K. [7] The planetary atmosphere has abundant carbon monoxide but likely lacks methane [8] and sodium, [9] although the high and dense cloud deck of WASP-29b prevents high-quality spectroscopic measurements. [10]

A study in 2018 revealed the stability of planetary orbits in the habitable zone of WASP-29 is significantly affected by the WASP-29b planet. [11]

The WASP-29 planetary system [7]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b0.243+0.020
−0.019  MJ 		0.0470±0.00253.92271218(25)<0.059 [4] 89.468+0.018
−0.017 ° 		0.775±0.031  RJ

Related Research Articles

<span class="mw-page-title-main">WASP-121b</span> Hot Jupiter exoplanet orbiting WASP-121

WASP-121b, formally named Tylos, is an exoplanet orbiting the star WASP-121. WASP-121b is the first exoplanet found to contain water in an extrasolar planetary stratosphere. WASP-121b is in the constellation Puppis, and is about 858 light-years from Earth.

WASP-49 is a yellow dwarf main-sequence star. Its surface temperature is 5600 K. WASP-49 is depleted of heavy elements relative to Sun, with metallicity Fe/H index of -0.23, meaning it has an abundance of iron 59% of the Sun's level.

Kepler-51 is a Sun-like star that is about 500 million years old. It is orbited by three super-puff planets—Kepler-51b, c, and d—which have the lowest known densities of any known exoplanet. The planets are similar in radius to gas giants like Jupiter, but have unusually small masses for their size, only a few times greater than Earth’s.

GJ 3470 is a red dwarf star located in the constellation of Cancer, 96 light-years away from Earth. With a faint apparent magnitude of 12.3, it is not visible to the naked eye. It hosts one known exoplanet.

WASP-78, is a single F-type main-sequence star about 2500 light-years away. It is likely to be younger than the Sun at 3.4+1.5
−0.8 billion years. WASP-78 is depleted in heavy elements, having a 45% concentration of iron compared to the Sun.

BD-07 436, also known as WASP-77 since 2012, is a binary star system about 344 light-years away. The star's components appears to have a different age, with the secondary older than 9 billion years, while the primary's age is 5 billion years. The BD-07 436 system's concentration of heavy elements is similar to the Sun. Its stars display moderate chromospheric activity, including x-ray flares.

WASP-72 is the primary of a binary star system. It is an F7 class dwarf star, with an internal structure just on the verge of the Kraft break. It is orbited by a planet WASP-72b. The age of WASP-72 is younger than the Sun at 3.55±0.82 billion years.

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-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. The distance to this system is approximately 942 light-years based on parallax measurements, but it is drifting closer with a radial velocity of −24 km/s.

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. 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.

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.

HAT-P-41 is a binary star system. Its primary is a F-type main-sequence star. Its surface temperature is 6390±100 K. compared to the Sun, HAT-P-41 is enriched in heavy elements, with a metallicity Fe/H index of 0.21±0.10, but is much younger at an age of 2.2±0.4 billion years.

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.

WASP-88 is a F-type main-sequence star. Its surface temperature is 6450±61 K. WASP-88 is similar to the Sun in its concentration of heavy elements, with a metallicity Fe/H index of 0.03±0.04, and is younger at an age of 3.0±1.3 billion years.

WASP-80 is a K-type main-sequence star about 162 light-years away. The star's age is much younger than the Sun's at 1.352±0.222 billion years. WASP-80 is similar to the Sun in concentration of heavy elements, although this measurement is highly uncertain.

References

  1. 1 2 3 4 5 6 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 "WASP-29". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 5 November 2023.
  3. 1 2 3 4 5 Fontanive, Clémence; Daniella Bardalez Gagliuffi (2021), "The Census of Exoplanets in Visual Binaries: population trends from a volume-limited Gaia DR2 and literature search", Frontiers in Astronomy and Space Sciences, 8: 16, arXiv: 2101.12667 , Bibcode:2021FrASS...8...16F, doi: 10.3389/fspas.2021.625250
  4. 1 2 Bonomo, A. S.; Desidera, S.; et al. (June 2017). "The GAPS Programme with HARPS-N at TNG. XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets". Astronomy & Astrophysics . 602: A107. arXiv: 1704.00373 . Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882. S2CID   118923163.
  5. 1 2 Hellier, Coel; Anderson, D. R.; Collier Cameron, A.; Gillon, M.; Lendl, M.; Maxted, P. F. L.; Queloz, D.; Smalley, B.; Triaud, A. H. M. J.; West, R. G.; Brown, D. J. A.; Enoch, B.; Lister, T. A.; Pepe, F.; Pollacco, D.; Ségransan, D.; Udry, S. (2010). "WASP-29b: A SATURN-SIZED TRANSITING EXOPLANET". The Astrophysical Journal. 723 (1): L60–L63. arXiv: 1009.5318 . Bibcode:2010ApJ...723L..60H. doi:10.1088/2041-8205/723/1/L60. S2CID   64119308.
  6. ↑ Dos Santos, L. A.; Bourrier, V.; Ehrenreich, D.; Sanz-Forcada, J.; López-Morales, M.; Sing, D. K.; García Muñoz, A.; Henry, G. W.; Lavvas, P.; Lecavelier Des Etangs, A.; Mikal-Evans, T.; Vidal-Madjar, A.; Wakeford, H. R. (2021), "HST PanCET program: Non-detection of atmospheric escape in the warm Saturn-sized planet WASP-29 B", Astronomy & Astrophysics, 649: A40, arXiv: 2103.15688 , Bibcode:2021A&A...649A..40D, doi:10.1051/0004-6361/202140491, S2CID   232417342
  7. 1 2 Saha, Suman; Sengupta, Sujan (2021), "Critical Analysis of Tess Transit Photometric Data: Improved Physical Properties for Five Exoplanets", The Astronomical Journal, 162 (5): 221, arXiv: 2109.11366 , Bibcode:2021AJ....162..221S, doi: 10.3847/1538-3881/ac294d , S2CID   237605336
  8. ↑ Matthew Hardin, Joseph Harrington, K. Stevenson, "WASP-29b: Another Cool Exoplanet With Abundant CO?"
  9. ↑ A Gemini ground-based transmission spectrum of WASP-29b: a featureless spectrum from 515 to 720 nm
  10. ↑ Wong, Ian; Chachan, Yayaati; Knutson, Heather A.; Henry, Gregory W.; Adams, Danica; Kataria, Tiffany; Benneke, Björn; Gao, Peter; Deming, Drake; López-Morales, Mercedes; Sing, David K.; Alam, Munazza K.; Ballester, Gilda E.; Barstow, Joanna K.; Buchhave, Lars A.; Dos Santos, Leonardo A.; Fu, Guangwei; Muñoz, Antonio García; MacDonald, Ryan J.; Mikal-Evans, Thomas; Sanz-Forcada, Jorge; Wakeford, Hannah R. (2022), "The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b", The Astronomical Journal, 164 (1): 30, arXiv: 2205.10765 , Bibcode:2022AJ....164...30W, doi: 10.3847/1538-3881/ac7234 , S2CID   248987053
  11. ↑ Georgakarakos, Nikolaos; Eggl, Siegfried; Dobbs-Dixon, Ian (April 2018). "Giant Planets: Good Neighbors for Habitable Worlds?". The Astrophysical Journal . 856 (2): 155. arXiv: 1804.02183 . Bibcode:2018ApJ...856..155G. doi: 10.3847/1538-4357/aaaf72 .
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