CoRoT-2

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CoRoT-2
Morgan-Keenan spectral classification zoom.png

CoRoT-2 is a G7V class star somewhat less massive than the Sun (G2V)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Aquila
Right ascension 19h 27m 06.4944s [1]
Declination +01° 23′ 01.360″ [1]
Apparent magnitude  (V)12.57 [2]
Characteristics
Spectral type G7V [3]
K0V (SIMBAD) [2]
Apparent magnitude  (V)~12.577
Apparent magnitude  (I)11.49 ±0.03
Apparent magnitude  (J)10.5783 ±0.028
Apparent magnitude  (H)10.44 ±0.04
Apparent magnitude  (K)10.31 ±0.03
Astrometry
Proper motion (μ)RA: −3.360(16)  mas/yr [1]
Dec.: −11.101(12)  mas/yr [1]
Parallax (π)4.6895 ± 0.0143  mas [1]
Distance 696 ± 2  ly
(213.2 ± 0.7  pc)
Details
Mass 0.97 ±0.06  M☉
Radius 0.902 ±0.018  R☉
Temperature 5625 ±120  K
Metallicity 0 ±0.1
Age ? years
Other designations
GSC 00465-01282, CoRoT-Exo-2, GSC2 N023200075, UCAC2 32263596, CoRoT 101206560, DENIS-P J192706.4+012301, 2MASS J19270649+0123013, USNO-B1.0 0913-00447544 [2]
Database references
SIMBAD data

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. [2]

Contents

It has a true physical companion, 2MASS J19270636+0122577, with a spectral type of K9, as earlier hypothesized by Alonso et al. (2008), making CoRoT-2 a wide binary system with at least one planet. [4]

Planetary system

This star is home to exoplanet CoRoT-2b discovered by the CoRoT Mission spacecraft using the transit method. [3] CoRoT-2b (formerly known as CoRoT-Exo-2b [5] ) is the second extrasolar planet to be detected by the French-led CoRoT mission, and orbits the star CoRoT-2 at a distance of 930 light years from Earth towards the constellation Aquila. Its discovery was announced on 20 December 2007. [6] After its discovery via the transit method, its mass was confirmed via the radial velocity method.

The radial velocity trend of CoRoT-2, caused by the presence of CoRoT-2 b. CoRoT-2 b rv.pdf
The radial velocity trend of CoRoT-2, caused by the presence of CoRoT-2 b.

The planet is a large hot Jupiter, about 1.43 times the radius of Jupiter and approximately 3.3 times as massive. Its huge size is due to the intense heating from its parent star, which causes the outer layers of its atmosphere to bloat. The extremely large radius of the planet indicates that CoRoT-2b is really hot, estimated to be around 1500 K, even hotter than would be expected given its location close to its parent star. This fact may be a sign of tidal heating due to interactions with another planet. [7] At Jupiter-like distances its radius would roughly be the same as Jupiter. [8] The complete phase curve of this planet has been observed. [9]

CoRoT-2b orbits its star approximately once every 1.7 days, and orbits the star in a prograde direction close to the star's equator. [10] Its parent star is a G-type star, a bit cooler than the Sun but more active. It is located about 800 light-years from Earth.

It takes 125 minutes to transit its star. [11]

As of August 2008, the CoRoT-2b spin-orbit angle (that is, the angle between the equator of the star and the plane of the planet orbit) was calculated by Bouchy et al. by means of the Rossiter–McLaughlin effect [12] with a value of +7.2 ± 4.5 degrees. [10]

The CoRoT-2 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 3.31±0.16  MJ 0.0281±0.00091.74299705(15)  d [13] 0—1.429±0.047  RJ

See also

Related Research Articles

<span class="mw-page-title-main">CoRoT</span> European space telescope that operated between 2006 - 2014

CoRoT was a space telescope mission which operated from 2006 to 2013. The mission's two objectives were to search for extrasolar planets with short orbital periods, particularly those of large terrestrial size, and to perform asteroseismology by measuring solar-like oscillations in stars. The mission was led by the French Space Agency (CNES) in conjunction with the European Space Agency (ESA) and other international partners.

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">CoRoT-1b</span> Extrasolar planet orbiting CoRoT-1

CoRoT-1b is a transiting extrasolar planet approximately 2,630 light-years away in the constellation of Monoceros. The planet was discovered orbiting the yellow dwarf star CoRoT-1 in May 2007. The planet was the first discovery by the French-led CoRoT Mission.

HAT-P-6 also named Sterrennacht is a star in the constellation Andromeda, located approximately 895 light years or 274 parsecs away from the Earth. It is an F-type star, implying that it is hotter and more massive than the Sun. The apparent magnitude of the star is +10.54, which means that it can only be visible through the telescope. The absolute magnitude of +3.36 is brighter than the Sun's +4.83, meaning that the star itself is brighter than the Sun. A search for a binary companion star using adaptive optics at the MMT Observatory turned out negative.

<span class="mw-page-title-main">HAT-P-6b</span> Extrasolar planet in the Andromeda constellation

HAT-P-6b is a transiting extrasolar planet discovered by Noyes et al. on October 15, 2007. It is located approximately 910 light-years away in the constellation of Andromeda, orbiting the star HAT-P-6. This hot Jupiter planet orbits with a semi-major axis of about 0.05 AU, and takes 92 hours, 28 minutes, 17 seconds to orbit the star. It has true mass of 5.7% greater than Jupiter and a radius 33% greater than Jupiter, corresponding to a density of 0.583 g/cm3, which is less than water.

<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.

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">CoRoT-3b</span> Brown dwarf or exoplanet orbiting CoRoT-3

CoRoT-3b is a brown dwarf or massive extrasolar planet with a mass 21.66 times that of Jupiter. The object orbits an F-type star in the constellation of Aquila. The orbit is circular and takes 4.2568 days to complete. It was discovered by the French-led CoRoT mission which detected the dimming of the parent star's light as CoRoT-3b passes in front of it.

CoRoT-4 is a yellow-white dwarf main-sequence star in the constellation Monoceros.

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<span class="mw-page-title-main">CoRoT-1</span> Yellow dwarf star in the constellation Monoceros

CoRoT-1 is a yellow dwarf main sequence star similar to the Sun. The star is located approximately 2,510 light-years away in the constellation of Monoceros. The apparent magnitude of this star is 13.6, which means it is not visible to the naked eye; however, it can be seen through a medium-sized amateur telescope on a clear, dark night. The first exoplanet discovered in the course of the CoRoT mission orbits this star; it is considered to be a "hot Jupiter", and is approximately as massive as the planet Jupiter itself.

CoRoT-7 is a binary star system made up of a late G-type star and a M-dwarf star that was discovered in 2021. The primary star has three exoplanets, including CoRoT-7b, an super-Earth exoplanet that is remarkable due to its extremly high temperature and very short orbital period, around 20 hours. It was the first exoplanet shown to be rocky. The system has the name CoRoT-7 after the CoRoT space telescope, which discovered the exoplanets around the star CoRoT-7A. The stellar system is 520 light-years from the Earth.

CoRoT-6 is a magnitude 13.9 star located in the Ophiuchus constellation.

CoRoT-5 is a magnitude 14 star located in the Monoceros constellation.

WASP-121, also known as CD-38 3220, is a magnitude 10.4 star located approximately 858 light-years away in the constellation Puppis. WASP-121 has a mass and radius similar to the Sun's. It hosts one known exoplanet.

<span class="mw-page-title-main">CoRoT-16b</span> Extrasolar planet in the constellation Scutum

CoRoT-16b is a transiting exoplanet orbiting the G or K type main sequence star CoRoT-16 2,433 light years away in the southern constellation Scutum. The planet was discovered in June 2011 by the French-led CoRoT mission.

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-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.

References

  1. 1 2 3 4 5 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 3 4 "GSC 00465-01282". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2009-04-27.
  3. 1 2 Alonso, R.; et al. (2008). "Transiting exoplanets from the CoRoT space mission. II. CoRoT-Exo-2b: a transiting planet around an active G star". Astronomy and Astrophysics. 482 (3): L21–L24. arXiv: 0803.3207 . Bibcode: 2008A&A...482L..21A . doi: 10.1051/0004-6361:200809431 . S2CID   14288300.
  4. ↑ S. Czesla; S. Schröter; U. Wolter; C. von Essen; K. F. Huber; J. H. M. M. Schmitt; D. E. Reichart; J. P. Moore (March 2012). "The extended chromosphere of CoRoT-2A: Discovery and analysis of the chromospheric Rossiter-McLaughlin effect". Astronomy and Astrophysics. 539: A150. Bibcode:2012A&A...539A.150C. doi: 10.1051/0004-6361/201118042 .
  5. ↑ Schneider, J. (10 March 2009). "Change in CoRoT planets names". Exoplanets (Mailing list). Archived from the original on 18 January 2010. Retrieved 2009-03-19.
  6. ↑ "COROT surprises a year after launch" . Retrieved 2007-12-21.
  7. ↑ "CoRoT-exo-2 c?" . Retrieved 2007-12-21.
  8. ↑ Gibor Basri; Brown (20 August 2006). "Planetesimals to Brown Dwarfs: What is a Planet?". Annu. Rev. Earth Planet. Sci. 34: 193–216. arXiv: astro-ph/0608417 . Bibcode:2006AREPS..34..193B. doi:10.1146/annurev.earth.34.031405.125058. S2CID   119338327.
  9. ↑ Cowan, Nicolas; Deming, Drake; Gillon, Michael; Knutson, Heather; Madhusudhan, Nikku; Rauscher, Emily (2011). "Phase Variations, Transits and Eclipses of the Misfit CoRoT-2b". Spitzer Proposal: 80044. Bibcode:2011sptz.prop80044C.
  10. 1 2 Bouchy, F.; Queloz, D.; Deleuil, M.; Loeillet, B.; Hatzes, A. P.; Aigrain, S.; Alonso, R.; Auvergne, M.; Baglin, A.; Barge, P.; Benz, W.; Bordé, P.; Deeg, H. J.; De La Reza, R.; Dvorak, R.; Erikson, A.; Fridlund, M.; Gondoin, P.; Guillot, T.; Hébrard, G.; Jorda, L.; Lammer, H.; Léger, A.; Llebaria, A.; Magain, P.; Mayor, M.; Moutou, C.; Ollivier, M.; Pätzold, M.; et al. (2008). "Transiting exoplanets from the CoRoT space mission". Astronomy and Astrophysics. 482 (3): L25. arXiv: 0803.3209 . Bibcode:2008A&A...482L..25B. doi:10.1051/0004-6361:200809433. S2CID   15766192.
  11. ↑ "Predicted Transit Epochs: CoRoTExo2 b". TransitSearch (Oklo Corporation). Retrieved 2009-07-15.[ permanent dead link ]
  12. ↑ 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.
  13. ↑ Kokori, A.; et al. (14 February 2023). "ExoClock Project. III. 450 New Exoplanet Ephemerides from Ground and Space Observations". The Astrophysical Journal Supplement Series. 265 (1) 4. arXiv: 2209.09673 . Bibcode: 2023ApJS..265....4K . doi: 10.3847/1538-4365/ac9da4 . Vizier catalog entry
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