HAT-P-2b

Last updated
HAT-P-2b / Magor
Exoplanet Comparison HAT-P-2 b.png
Size comparison of HAT-P-2b with Jupiter.
Discovery
Discovered by HATNet Project [1]
Discovery date2007-05-01 [2]
Transit
Designations
HD 147506 b, Magor
Orbital characteristics [3]
0.06880+0.00065
−0.00070  AU
Eccentricity 0.50833+0.00082
−0.00075
5.6334754±0.0000026  d
Inclination 86.72°+1.1°
−0.87°
2455289.4721±0.0038 [4]
186.96°+0.87°
−0.88°
Semi-amplitude 938.1+10.0
−9.9  m/s
Star HD 147506
Physical characteristics [3]
Mean radius
1.157+0.073
−0.063  RJ
Mass 8.70+0.19
−0.20  MJ
Mean density
7.3+1.4
−1.1  g/cm3
162±27 m/s²
Temperature 1540±30  K [5]

    HAT-P-2b is an extrasolar planet detected by the HATNet Project in May 2007. It orbits a class F star HAT-P-2, (bigger and hotter than the Sun), located about 420 light-years away in the constellation Hercules.

    Contents

    The planet is officially named Magor. The name was selected in the NameExoWorlds campaign by Hungary, during the 100th anniversary of the International Astronomical Union. Magor was a legendary ancestor of the Magyar people and the Hungarian nation, and brother of Hunor (name of the star HAT-P-2). [6] [7]

    Physical properties

    The planet's mass has been estimated to be 8.7 times that of Jupiter, while its diameter is 1.157 times Jupiter's. [3] Its small size, despite the bloating of the planet's atmosphere, is caused by the strong gravity of the planet. The planetary atmosphere has indeed the smallest scale height, equal to 26km, among exoplanets with measurable atmospheres as of 2021. [8]

    This indicates its mean density is twice that of Earth and its surface gravity approximately 24 times that of Earth, almost equal to the Sun.

    In addition to heat from its primary star, tidal heating is thought to have played a significant role in this planet's evolution. [9]

    Orbit

    The planetary orbital period is 5 days 15 hours, and its inclination is such that it crosses directly in front of the star as viewed from Earth. [1] [2] The orbit is very eccentric, ranging from 4.90 million to 15.36 million miles from the star. [2]

    As of August 2008, the most recent calculation of HAT-P-2b's Rossiter–McLaughlin effect and so spin-orbit angle was that of Winn in 2007 but Loeillet has in 2008 disputed it. [10] [11] For Winn, this is +1 ± 13 degrees. [12] The study in 2012 determined the planetary orbit is probably aligned with the equatorial plane of the star, with misalignment equal to 9±10°. [13]

    Other planets in the system

    It has been suggested that there is a second outer planet perturbing HAT-P-2b. [2] In 2023, the presence of a second planet, HAT-P-2c, was confirmed. [14]

    Related Research Articles

    <span class="mw-page-title-main">HAT-P-1b</span> Hot Jupiter orbiting HAT-P-1

    HAT-P-1b is an extrasolar planet orbiting the Sun-like star HAT-P-1, also known as ADS 16402 B. HAT-P-1 is the dimmer component of the ADS 16402 binary star system. It is located roughly 521 light years away from Earth in the constellation Lacerta. HAT-P-1b is among the least dense of any of the known extrasolar planets.

    HD 147506, also known as HAT-P-2 and formally named Hunor, is a magnitude 8.7 F8 dwarf star that is somewhat larger and hotter than the Sun. The star is approximately 419 light-years from Earth and is positioned near the keystone of Hercules. It is estimated to be 2 to 3 billion years old, towards the end of its main sequence life. There is one known transiting exoplanet, and a second planet not observed to transit.

    <span class="mw-page-title-main">XO-3b</span> Extrasolar planet in the constellation Camelopardalis

    XO-3b is an exoplanet with about 11.79 times the mass of Jupiter, and it orbits its parent star in about 3.2 days. The radius of this object is 1.217 times that of Jupiter. Astronomers announced their discovery on May 30, 2007, at the American Astronomical Society in Honolulu, Hawaii. Its discovery is attributed to the combined effort of amateur and professional astronomers working together on the XO Project using a telescope located on the Haleakala summit in Hawaii.

    <span class="mw-page-title-main">HAT-P-4b</span> Exoplanet orbiting HAT-P-4b in the constellation Boötes

    HAT-P-4b is a confirmed extrasolar planet orbiting the star HAT-P-4 over 1000 light years away in Boötes constellation. It was discovered by transit on October 2, 2007, which looks for slight dimming of stars caused by planets that passed in front of them. It is the fourth planet discovered by the HATNet Project. It is also called BD+36 2593b, TYC 2569-01599-1b, 2MASS J15195792+3613467b, SAO 64638b.

    <span class="mw-page-title-main">CoRoT-2b</span> Extrasolar planet in the constellation Aquila

    CoRoT-2b is the second extrasolar planet to be detected by the French-led CoRoT mission, and orbits the star CoRoT-2 at a distance of 700 light years from Earth towards the constellation Aquila. Its discovery was announced on 20 December 2007. After its discovery via the transit method, its mass was confirmed via the radial velocity method.

    <span class="mw-page-title-main">HAT-P-7b</span> Super Jupiter orbiting HAT-P-7

    HAT-P-7b is an extrasolar planet discovered in 2008. It orbits very close to its host star and is larger and more massive than Jupiter. Due to the extreme heat that it receives from its star, the dayside temperature is predicted to be 2,630–2,880 K K, while nightside temperatures are 2,211–2,238 K. HAT-P-7b is also one of the darkest planets ever observed, with an albedo of less than 0.03—meaning it absorbs more than 97% of the visible light that strikes it.

    <span class="mw-page-title-main">WASP-7b</span> Extrasolar planet in the constellation Microscopium

    WASP-7b is an extrasolar planet discovered in 2008. This 5-day period planet is slightly smaller than Jupiter, roughly the same mass and more dense.

    <span class="mw-page-title-main">HD 80606 b</span> Eccentric hot Jupiter in the constellation Ursa Major

    HD 80606 b is an eccentric hot Jupiter 217 light-years from the Sun in the constellation of Ursa Major. HD 80606 b was discovered orbiting the star HD 80606 in April 2001 by a team led by Michel Mayor and Didier Queloz. With a mass 4 times that of Jupiter, it is a gas giant. Because the planet transits the host star its radius can be determined using the transit method, and was found to be about the same as Jupiter's. Its density is slightly less than Earth's. It has an extremely eccentric orbit like a comet, with its orbit taking it very close to its star and then back out very far away from it every 111 days.

    <span class="mw-page-title-main">HD 17156 b</span> Extrasolar planet in the constellation of Cassiopeia

    HD 17156 b, named Mulchatna by the IAU, is an extrasolar planet approximately 255 light-years away in the constellation of Cassiopeia. The planet was discovered orbiting the yellow subgiant star HD 17156 in April 2007. The planet is classified as a relatively cool hot Jupiter planet slightly smaller than Jupiter but slightly larger than Saturn. This highly-eccentric three-week orbit takes it approximately 0.0523 AU of the star at periastron before swinging out to approximately 0.2665 AU at apastron. Its eccentricity is about the same as 16 Cygni Bb, a so-called "eccentric Jupiter". Until 2009, HD 17156 b was the transiting planet with the longest orbital period.

    CoRoT-2 is a yellow dwarf main sequence star a little cooler than the Sun. This star is located approximately 700 light-years away in the constellation of Aquila. The apparent magnitude of this star is 12, which means it is not visible to the naked eye but can be seen with a medium-sized amateur telescope on a clear dark night.

    HAT-P-13, also known as GSC 03416-00543, is a G-type main sequence star approximately 800 light-years away in the constellation Ursa Major. In 2009 it was discovered that this star is orbited by two massive planets, the innermost of which transits the star. This was the first known example of an extrasolar transiting planet with an additional planet in the same system.

    <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.

    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.

    HAT-P-17 is a K-type main-sequence star about 92.4 parsecs (301 ly) away. It has a mass of about 0.857 ± 0.039 M☉. It is the host of two planets, HAT-P-17b and HAT-P-17c, both discovered in 2010. A search for a binary companion star using adaptive optics at the MMT Observatory was negative. A candidate companion was detected by a spectroscopic search of high-resolution K band infrared spectra taken at the Keck observatory.

    HAT-P-27, also known as WASP-40, is the primary of a binary star system about 659 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.

    HD 146389, is a star with a yellow-white hue in the northern constellation of Hercules. The star was given the formal name Irena by the International Astronomical Union in January 2020. It is invisible to the naked eye with an apparent visual magnitude of 9.4 The star is located at a distance of approximately 446 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s. The star is known to host one exoplanet, designated WASP-38b or formally named 'Iztok'.

    HAT-P-16 is a F-type main-sequence star about 725 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.

    Qatar-2 is a K-type main-sequence star about 595 light-years away in the constellation of Virgo. The star is much older than Sun, and has a concentration of heavy elements similar to solar abundance. The star features a numerous and long-lived starspots, and belongs to a peculiar variety of inflated K-dwarfs with strong magnetic activity inhibiting internal convection.

    References

    1. 1 2 Bakos, G. Á.; et al. (2007). "HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star". The Astrophysical Journal. 670 (1): 826–832. arXiv: 0705.0126 . Bibcode: 2007ApJ...670..826B . doi: 10.1086/521866 .
    2. 1 2 3 4 Aguilar, David A.; Pulliam, Christine (2007-05-01). "Astronomers find super-massive planet" (Press release). Harvard-Smithsonian Center for Astrophysics . Retrieved 2019-01-05.
    3. 1 2 3 Bonomo, A. S.; et al. (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 and Astrophysics. 602 (107) A107. arXiv: 1704.00373 . Bibcode: 2017A&A...602A.107B . doi: 10.1051/0004-6361/201629882 .
    4. ↑ Lewis, Nikole K.; et al. (2013). "Orbital Phase Variations of the Eccentric Giant Planet HAT-P-2b". The Astrophysical Journal. 766 (2) 95. arXiv: 1302.5084 . Bibcode: 2013ApJ...766...95L . doi: 10.1088/0004-637X/766/2/95 .
    5. ↑ Pál, András; et al. (2010). "Refined stellar, orbital and planetary parameters of the eccentric HAT-P-2 planetary system". Monthly Notices of the Royal Astronomical Society. 401 (4): 2665–2674. arXiv: 0908.1705 . Bibcode: 2010MNRAS.401.2665P . doi: 10.1111/j.1365-2966.2009.15849.x .
    6. ↑ "Approved names". NameExoworlds. Retrieved 2020-01-02.
    7. ↑ "International Astronomical Union | IAU". www.iau.org. Retrieved 2020-01-02.
    8. ↑ Baxter, Claire; Désert, Jean-Michel; Tsai, Shang-Min; Todorov, Kamen O.; Bean, Jacob L.; Deming, Drake; Parmentier, Vivien; Fortney, Jonathan J.; Line, Michael; Thorngren, Daniel; Pierrehumbert, Raymond T.; Burrows, Adam; Showman, Adam P. (2021), "Evidence for disequilibrium chemistry from vertical mixing in hot Jupiter atmospheres", Astronomy & Astrophysics, 648: A127, arXiv: 2103.07185 , doi:10.1051/0004-6361/202039708, S2CID   232222174
    9. ↑ Jackson, Brian; et al. (2008). "Tidal Heating of Extra-Solar Planets". Astrophysical Journal. 681 (2): 1631. arXiv: 0803.0026 . Bibcode:2008ApJ...681.1631J. doi:10.1086/587641. S2CID   42315630.
    10. ↑ Joshua N. Winn (2008). "Measuring accurate transit parameters". Proceedings of the International Astronomical Union. 4: 99–109. arXiv: 0807.4929 . Bibcode:2009IAUS..253...99W. doi:10.1017/S174392130802629X. S2CID   34144676.
    11. ↑ Loeillet, B.; et al. (2008). "Refined parameters and spectroscopic transit of the super-massive planet HD 147506b". Astronomy and Astrophysics. 481 (2): 529–533. arXiv: 0707.0679 . Bibcode: 2008A&A...481..529L . doi: 10.1051/0004-6361:20078167 .
    12. ↑ Winn; et al. (2007). "Spin-Orbit Alignment for the Eccentric Exoplanet HD 147506b". Astrophysical Journal Letters. 665 (2): L167. arXiv: 0707.0503 . Bibcode:2007ApJ...665L.167W. doi:10.1086/521362. S2CID   330965.
    13. ↑ Albrecht, Simon; Winn, Joshua N.; Johnson, John A.; Howard, Andrew W.; Marcy, Geoffrey W.; Butler, R. Paul; Arriagada, Pamela; Crane, Jeffrey D.; Shectman, Stephen A.; Thompson, Ian B.; Hirano, Teruyuki; Bakos, Gaspar; Hartman, Joel D. (2012), "Obliquities of Hot Jupiter Host Stars: Evidence for Tidal Interactions and Primordial Misalignments", The Astrophysical Journal, 757 (1): 18, arXiv: 1206.6105 , Bibcode:2012ApJ...757...18A, doi:10.1088/0004-637X/757/1/18, S2CID   17174530
    14. ↑ de Beurs, Zoë L.; et al. (October 2023). "Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c". The Astronomical Journal. 166 (4) 136. arXiv: 2309.03256 . Bibcode: 2023AJ....166..136D . doi: 10.3847/1538-3881/acedf1 .

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