WASP-11b/HAT-P-10b

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WASP-11b/HAT-P-10b
Exoplanet Comparison WASP-11-HAT-P-10 b.png
Size comparison of WASP-11b/HAT-P-10b with Jupiter.
Discovery
Discovered by West et al. (SuperWASP)
Bakos et al. (HATNet)
Discovery site SAAO
Discovery dateApril 1, 2008 (announced)
September 26, 2008 (preprints)
Transit
Orbital characteristics
0.0439+0.0006
−0.0009 [1] AU
Eccentricity 0 [1]
3.7224690 ± 0.0000067 [1] d
Inclination 88.5 ± 0.6 [1]
Semi-amplitude 69.1 ± 3.5 [1]
Star WASP-11/HAT-P-10 [2]
Physical characteristics
Mean radius
1.045+0.050
−0.033 [1] RJ
Mass 0.460 ± 0.028 [1] MJ
Mean density
498 ± 64  kg/m3 (839 ± 108  lb/cu yd) [1]
10.5  m/s2 (34  ft/s2) [1]
Temperature 1030+26
−19 [1] [note 1]

WASP-11b/HAT-P-10b or WASP-11Ab/HAT-P-10Ab [3] is an extrasolar planet discovered in 2008. The discovery was announced (under the designation WASP-11b) by press release by the SuperWASP project in April 2008 along with planets WASP-6b through to WASP-15b, however at this stage more data was needed to confirm the parameters of the planets and the coordinates were not given. [4] On 26 September 2008, the HATNet Project's paper describing the planet which they designated HAT-P-10b appeared on the arXiv preprint server. [1] The SuperWASP team's paper appeared as a preprint on the Extrasolar Planets Encyclopaedia on the same day, confirming that the two objects (WASP-11b and HAT-P-10b) were in fact the same, and the teams agreed to use the combined designation. [2]

Contents

The planet had the third lowest insolation of the known transiting planets at the time of the discovery (prior to this, Gliese 436 b and HD 17156 b were known to have lower insolation). The temperature implies it falls into the pL class of hot Jupiters: planets which lack significant quantities of titanium(II) oxide and vanadium(II) oxide in their atmospheres and do not have temperature inversions. [5] An alternative classification system for hot Jupiters is based on the equilibrium temperature and the planet's Safronov number. [note 2] In this scheme, for a given temperature, class I planets have high Safronov numbers and tend to be in orbit around cooler host stars, while class II planets have lower Safronov numbers. [6] In the case of WASP-11b/HAT-P-10b, the equilibrium temperature is 1030 K [note 1] and the Safronov number is 0.047±0.003, which means it is located close to the dividing line between the class I and class II planets. [1]

The planet is in a binary star system, the second star is WASP-11 B, with a mass 0.34 ± 0.05 of the Sun and a temperature of 3483 ± 43 K. [7]

Notes

  1. 1 2 Assumes the planet has zero albedo. Its secondary transit of the planet behind its star has not yet been observed and so the temperature provided is a hypothetical "equilibrium temperature".
  2. ↑ The Safronov number is defined as

See also

Related Research Articles

<span class="mw-page-title-main">Hot Jupiter</span> Class of high mass planets orbiting close to a star

Hot Jupiters are a class of gas giant exoplanets that are inferred to be physically similar to Jupiter but that have very short orbital periods. The close proximity to their stars and high surface-atmosphere temperatures resulted in their informal name "hot Jupiters".

<span class="mw-page-title-main">Sudarsky's gas giant classification</span>

Sudarsky's classification of gas giants for the purpose of predicting their appearance based on their temperature was outlined by David Sudarsky and colleagues in the paper Albedo and Reflection Spectra of Extrasolar Giant Planets and expanded on in Theoretical Spectra and Atmospheres of Extrasolar Giant Planets, published before any successful direct or indirect observation of an extrasolar planet atmosphere was made. It is a broad classification system with the goal of bringing some order to the likely rich variety of extrasolar gas-giant atmospheres.

<span class="mw-page-title-main">WASP-1b</span> Extrasolar planet in the Andromeda constellation

WASP-1b is an extrasolar planet orbiting the star WASP-1 located 1,300 light-years away in the constellation Andromeda.

The Hungarian Automated Telescope Network (HATNet) project is a network of six small fully automated "HAT" telescopes. The scientific goal of the project is to detect and characterize extrasolar planets using the transit method. This network is used also to find and follow bright variable stars. The network is maintained by the Center for Astrophysics | Harvard & Smithsonian.

<span class="mw-page-title-main">WASP-5b</span> Jovian size planet orbiting WASP-5

WASP-5b is an exoplanet orbiting the star WASP-5 located approximately 1000 light-years away in the constellation Phoenix. The planet's mass and radius indicate that it is a gas giant with a similar bulk composition to Jupiter. The small orbital distance of WASP-5 b around its star means it belongs to a class of planets known as hot Jupiters. The planetary equilibrium temperature would be 1717 K, but the measured dayside temperature is higher, with a 2015 study finding 2500±100 K and a 2020 study finding 2000±90 K.

<span class="mw-page-title-main">WASP-8b</span> Planet orbiting a star in a binary system in the constellation of Sculptor

WASP-8b is an exoplanet orbiting the star WASP-8A in the constellation of Sculptor. The star is similar to the Sun and forms a binary star with a red dwarf star (WASP-8B) of half the Sun's mass that orbits WASP-8A 4.5 arcseconds away. The system is 294 light-years away and is therefore located closer to Earth than many other star systems that are known to feature planets similar to WASP-8b. The planet and its parent star were discovered in the SuperWASP batch -6b to -15b. On 1 April 2008, Dr. Don Pollacco of Queen's University Belfast announced them at the RAS National Astronomy Meeting.

WASP-10 is a star in the constellation Pegasus. The SuperWASP project has observed and classified this star as a variable star, perhaps due to the eclipsing planet.

WASP-11/HAT-P-10 is a binary star. It is a primary main-sequence orange dwarf star. Secondary is M-dwarf with a projected separation of 42 AU. The system is located about 424 light-years away in the constellation Aries.

<span class="mw-page-title-main">WASP-12b</span> Hot Jupiter exoplanet in the constellation Auriga

WASP-12b is a hot Jupiter orbiting the star WASP-12, discovered on April 1, 2008, by the SuperWASP planetary transit survey. The planet takes only a little over one Earth day to orbit its star, in contrast to about 365.25 days for the Earth to orbit the Sun. Its distance from the star is only the Earth's distance from the Sun, with an eccentricity the same as Jupiter's. Consequently, it has one of the lowest densities for exoplanets. On December 3, 2013, scientists working with the Hubble Space Telescope (HST) reported detecting water in the atmosphere of the exoplanet. In July 2014, NASA announced finding very dry atmospheres on three exoplanets orbiting sun-like stars.

<span class="mw-page-title-main">OGLE-TR-111b</span> Hot Jupiter orbiting OGLE-TR-111

OGLE-TR-111b is an extrasolar planet approximately 5,000 light-years away in the constellation of Carina. The planet is currently the only confirmed planet orbiting the star OGLE-TR-111.

HAT-P-32b is a planet orbiting the G-type or F-type star HAT-P-32, which is approximately 950 light years away from Earth. HAT-P-32b was first recognized as a possible planet by the planet-searching HATNet Project in 2004, although difficulties in measuring its radial velocity prevented astronomers from verifying the planet until after three years of observation. The Blendanal program helped to rule out most of the alternatives that could explain what HAT-P-32b was, leading astronomers to determine that HAT-P-32b was most likely a planet. The discovery of HAT-P-32b and of HAT-P-33b was submitted to a journal on 6 June 2011.

<span class="mw-page-title-main">HAT-P-27</span> Star in the constellation Virgo

HAT-P-27, also known as WASP-40, is the primary of a binary star system about 650 light-years away. It is a G-type main-sequence star. The star's age is similar to the Sun's at 4.4 billion years. HAT-P-27 is enriched in heavy elements, having a 195% concentration of iron compared to the Sun.

WASP-36 is a yellow main sequence star in the Hydra constellation.

HAT-P-20 is a K-type main-sequence star about 232 light-years away. The star has a strong starspot activity, and its equatorial plane is misaligned by 36+10
−12° with the planetary orbit. Although star with a giant planet on close orbit is expected to be spun-up by tidal forces, only weak indications of tidal spin-up were detected.

HAT-P-16 is a F-type main-sequence star about 740 light-years away. The star has a concentration of heavy elements slightly higher than solar abundance, and low starspot activity. The survey in 2015 have failed to find any stellar companions to it. The spectral analysis in 2014 have discovered the HAT-P-16 has a carbon to oxygen molar ratio of 0.58±0.08, close to Sun`s value of 0.55.

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 Bakos, G. Á.; et al. (2009). "HAT-P-10b: A Light and Moderately Hot Jupiter Transiting A K Dwarf". The Astrophysical Journal. 696 (2): 1950–1955. arXiv: 0809.4295 . Bibcode:2009ApJ...696.1950B. doi:10.1088/0004-637X/696/2/1950. S2CID   12146075.
  2. 1 2 Schneider, J. "Notes for star WASP-11/HAT-P-10". Extrasolar Planets Encyclopaedia . Archived from the original on 2008-10-01. Retrieved 2008-09-29.
  3. ↑ West, R. G; Collier Cameron, A; Hebb, L; Joshi, Y. C; Pollacco, D; Simpson, E; Skillen, I; Stempels, H. C; Wheatley, P. J; Wilson, D; Anderson, D; Bentley, S; Bouchy, F; Enoch, B; Gibson, N; Hébrard, G; Hellier, C; Loeillet, B; Mayor, M; Maxted, P; McDonald, I; Moutou, C; Pont, F; Queloz, D; Smith, A. M. S; Smalley, B; Street, R. A; Udry, S (2011). "The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets". arXiv: 1109.2497 [astro-ph.EP].
  4. ↑ "WASP Planets". SuperWASP. 5 December 2013. Retrieved 2016-01-26.
  5. ↑ Fortney, J. J.; et al. (2008). "A Unified Theory for the Atmospheres of the Hot and Very Hot Jupiters: Two Classes of Irradiated Atmospheres". The Astrophysical Journal . 678 (2): 1419–1435. arXiv: 0710.2558 . Bibcode:2008ApJ...678.1419F. doi:10.1086/528370. S2CID   17502177.
  6. ↑ Hansen, B. M. S. & Barman, T. (2007). "Two Classes of Hot Jupiters". The Astrophysical Journal . 671 (1): 861–871. arXiv: 0706.3052 . Bibcode:2007ApJ...671..861H. doi:10.1086/523038. S2CID   16630784.
  7. ↑ Open Exoplanet Catalogue WASP-11 20b

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