WASP-25

Last updated
WASP-25
Observation data
Epoch J2000       Equinox
Constellation Hydra
Right ascension 13h 01m 26.3760s [1]
Declination −27° 31′ 19.9208″ [1]
Apparent magnitude  (V)11.87 [2]
Characteristics
Evolutionary stage main sequence star
Spectral type G4 [3]
B−V color index 0.45
J−H color index 0.328[ citation needed ]
J−K color index 0.422[ citation needed ]
Astrometry
Radial velocity (Rv)-2.698±0.0028 [4]  km/s
Proper motion (μ)RA: -29.268±0.061 [1]   mas/yr
Dec.: -6.293±0.047 [1]   mas/yr
Parallax (π)4.714 ± 0.0324  mas [1]
Distance 692 ± 5  ly
(212 ± 1  pc)
Details [3] [5]
Mass 1.00±0.03  M☉
Radius 0.92  R☉
Surface gravity (log g)4.50±0.15  cgs
Temperature 5615±55  K
Metallicity [Fe/H]-0.07±0.1  dex
Rotational velocity (v sin i)3.0±1 km/s
Age 0.02+3.96
−0.01  Gyr
Other designations
WASP-25, Gaia DR2  6186950525042445824, TYC  6706-861-1, 2MASS J13012637-2731199, DENIS J130126.3-273120 [6]
Database references
SIMBAD data

WASP-25 is a yellow main sequence star in the constellation of Hydra.

Contents

Star characteristics

WASP-25 is slightly metal-poor (85% of Solar amount) and is probably a young star which has just entered the main sequence. [3]

Planetary system

The "Hot Jupiter" class planet WASP-25b was discovered around WASP-25 in 2010. [3] The planet would have an equilibrium temperature of 1212±35 K. A Rossiter-McLaughlin effect based study in 2011 found a modest misalignment of the planetary orbit to the rotational axis of the parent star, equal to 14.6±6.7 degrees. [7] A habitability study in 2018 found WASP-25b does not adversely affect the stability of planetary orbits in the habitable zone of WASP-25. [8]

The WASP-25 planetary system [9] [10]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 0.58±0.04  MJ 0.0474±0.00043.764825±0.000005088.33±0.32° 1.26+0.06
−0.05  RJ

Related Research Articles

<span class="mw-page-title-main">Wide Angle Search for Planets</span> Exoplanet search project

WASP or Wide Angle Search for Planets is an international consortium of several academic organisations performing an ultra-wide angle search for exoplanets using transit photometry. The array of robotic telescopes aims to survey the entire sky, simultaneously monitoring many thousands of stars at an apparent visual magnitude from about 7 to 13.

WASP-16 is a magnitude 11 yellow dwarf main sequence star, with characteristics similar to the Sun, located in the Virgo constellation.

WASP-79b, also known as Pollera, is an extrasolar planet orbiting the star CD-30 1812. This planet is in the constellation Eridanus, and is about 810 light-years from Earth.

WASP-76, also known as BD+01 316, is a yellow-white main sequence star in the constellation of Pisces. Since 2014, it has had one suspected stellar companion at a projected separation of 85 astronomical units.

WASP-32 is a yellow main-sequence star in the constellation of Pisces. The star was given the formal name Parumleo in January 2020, Latin for small lion and referencing the national animal of Singapore.

WASP-29 is a binary star system 285 light-years 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. The star system kinematically belongs to the thin disk of the Milky Way.

WASP-26 is a yellow main sequence star in the constellation of Cetus.

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.

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.

BD+00 316 is an ordinary star with a close-orbiting planetary companion in the equatorial constellation of Cetus. It is also known as WASP-71 since 2019; BD+00 316 is the stellar identifier from the Bonner Durchmusterung catalogue. With an apparent visual magnitude of 10.56, it is too faint to be visible to the naked eye. This star is located at a distance of 1,160 light-years based on parallax measurements, and is drifting further away with a heliocentric radial velocity of 7.7 km/s.

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-59 is a K-type main-sequence star about 379 light-years away. The star's age is essentially unconstrained by observations. WASP-59 is slightly depleted in heavy elements, having 70% of the solar abundance of iron. The star produces extremely low levels of ultraviolet light, indicating an absence of flare activity.

WASP-42 is a K-type main-sequence star. Its surface temperature is 5315±79 K. WASP-42 is similar to the Sun in concentration of heavy elements, with metallicity ([Fe/H]) of 0.05±0.13, and is much older than the Sun at 11.3+1.5
−4.8 billion years. The star does exhibit starspot activity as is typical for its spectral class.

WASP-84, also known as BD+02 2056, is a G-type main-sequence star 327 light-years away in the constellation Hydra. Its surface temperature is 5350±31 K and is slightly enriched in heavy elements compared to the Sun, with a metallicity Fe/H index of 0.05±0.02. It is rich in carbon and depleted of oxygen. WASP-84's age is probably older than the Sun at 8.5+4.1
−5.5 billion years. The star appears to have an anomalously small radius, which can be explained by the unusually high helium fraction or by it being very young.

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 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. ↑ Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
  3. 1 2 3 4 Enoch, B.; Cameron, A. Collier; Anderson, D. R.; Lister, T. A.; Hellier, C.; Maxted, P. F. L.; Queloz, D.; Smalley, B.; Triaud, A. H. M. J.; West, R. G.; Brown, D. J. A.; Gillon, M.; Hebb, L.; Lendl, M.; Parley, N.; Pepe, F.; Pollacco, D.; Segransan, D.; Simpson, E.; Street, R. A.; Udry, S. (2010). "WASP-25b: A 0.6 MJ planet in the Southern hemisphere". Monthly Notices of the Royal Astronomical Society: no. arXiv: 1009.5917 . doi:10.1111/j.1365-2966.2010.17550.x. S2CID   6314762.
  4. ↑ Soubiran, C.; Jasniewicz, G.; Chemin, L.; Zurbach, C.; Brouillet, N.; Panuzzo, P.; Sartoretti, P.; Katz, D.; Le Campion, J. -F.; Marchal, O.; Hestroffer, D.; Thévenin, F.; Crifo, F.; Udry, S.; Cropper, M.; Seabroke, G.; Viala, Y.; Benson, K.; Blomme, R.; Jean-Antoine, A.; Huckle, H.; Smith, M.; Baker, S. G.; Damerdji, Y.; Dolding, C.; Frémat, Y.; Gosset, E.; Guerrier, A.; Guy, L. P.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv: 1804.09370 . Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID   52952408.
  5. ↑ Maxted, P. F. L., Koen, C., Smalley, B., 2011, MNRAS, 418, 1039
  6. ↑ WASP-25 -- Star
  7. ↑ Brown, D. J. A.; Cameron, A. Collier; Anderson, D. R.; Enoch, B.; Hellier, C.; Maxted, P. F. L.; Miller, G. R. M.; Pollacco, D.; Queloz, D.; Simpson, E.; Smalley, B.; Triaud, A. H. M. J.; Boisse, I.; Bouchy, F.; Gillon, M.; Hébrard, G. (2012). "Rossiter-Mc Laughlin effect measurements for WASP-16, WASP-25 and WASP-31★". Monthly Notices of the Royal Astronomical Society. 423 (2): 1503–1520. arXiv: 1203.4971 . Bibcode:2012MNRAS.423.1503B. doi:10.1111/j.1365-2966.2012.20973.x. S2CID   53445367.
  8. ↑ Georgakarakos, Nikolaos; Eggl, Siegfried; Dobbs-Dixon, Ian (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 . S2CID   119522834.
  9. ↑ Planet WASP-25 b at exoplanet.eu
  10. ↑ Southworth, John; Hinse, T. C.; Burgdorf, M.; Calchi Novati, S.; Dominik, M.; Galianni, P.; Gerner, T.; Giannini, E.; Gu, S.-H.; Hundertmark, M.; Jørgensen, U. G.; Juncher, D.; Kerins, E.; Mancini, L.; Rabus, M.; Ricci, D.; Schäfer, S.; Skottfelt, J.; Tregloan-Reed, J.; Wang, X.-B.; Wertz, O.; Alsubai, K. A.; Andersen, J. M.; Bozza, V.; Bramich, D. M.; Browne, P.; Ciceri, S.; d'Ago, G.; Damerdji, Y.; et al. (2014). "High-precision photometry by telescope defocussing – VI. WASP-24, WASP-25 and WASP-26★". Monthly Notices of the Royal Astronomical Society. 444 (1): 776–789. arXiv: 1407.6253 . Bibcode:2014MNRAS.444..776S. doi:10.1093/mnras/stu1492. S2CID   53641330.
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