CoRoT-1

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CoRoT-1
CoRoT-1.jpg
An artist's depiction of CoRoT-1 and its "hot Jupiter" exoplanet
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Monoceros
Right ascension 06h 48m 19.1724s [1]
Declination −03° 06′ 07.7104″ [1]
Apparent magnitude  (V)13.6 [2]
Characteristics
Spectral type G0V [2]
Apparent magnitude  (V)~13.6 [2]
Apparent magnitude  (I)12.88 ±0.04 [2]
Apparent magnitude  (J)12.462 ±0.029 [2]
Apparent magnitude  (H)12.218 ±0.026 [2]
Apparent magnitude  (K)12.149 ±0.027 [2]
Variable type Pulsating variable [3]
Astrometry
Proper motion (μ)RA: −6.015±0.047 [1]   mas/yr
Dec.: 0.547±0.041 [1]   mas/yr
Parallax (π)1.2418 ± 0.0375  mas [1]
Distance 2,630 ± 80  ly
(810 ± 20  pc)
Details
Mass 0.95 ±0.15  M☉
Temperature 5950 ±150  K
Metallicity -0.3 ±0.25
Age ? years
Other designations
GSC 04804-02268, DENIS-P J064819.1-030607, 2MASS J06481917-0306077, USNO-B1.0 0868-00112004, CoRoT-Exo-1, GSC2 S1002112279, UCAC2 30655657 [2]
Database references
SIMBAD data
Extrasolar Planets
Encyclopaedia 		data

CoRoT-1 is a yellow dwarf main sequence star similar to the Sun. The star is located approximately 2,630 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. [2] 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.

Contents

Nomenclature

The designation "CoRoT" is a result of its observation by the French-directed Convection, Rotation, and Planetary Transits mission, which was launched in late December 2006 with one goal involving the search for exoplanets by measuring the varying brightness of candidate stars when transited by any present exoplanets; [4] CoRoT's second goal pertains to the study of the interiors of stars, which is done by analyzing the characteristics and behavior of light released from the star. [5] The numerical designation was assigned because the first exoplanet discovered by the CoRoT telescope was found in orbit of this star. [6] CoRoT-1 does not have a common or colloquial name like that of Sirius or Procyon.

Characteristics

CoRoT-1 is a G-type star, meaning the light it emits is similar to that of the Sun's. Likewise, the star is of nearly the same temperature and mass of the Sun. [2] At an apparent magnitude of approximately +13.6, [2] doubly dimmer than the dimmest star visible with the naked eye, CoRoT-1 cannot be seen from Earth without magnification apparatus. [7]

A search for a binary companion star using Lucky imaging observations with the Danish 1.54 m telescope at La Silla Observatory in Chile did not find any candidate companion stars. [8]

Variability

When CoRoT-1 was observed by the CoRoT telescope over a continuous period of sixty days since the preliminary results release on 23 May 2007, the star's light exhibited patterns identical to pulsating variable stars with characteristics similar to that of the Sun. [3]

Planetary system

The transit method, which can be documented when planets eclipse their star in respect to Earth's position, was used to discover CoRoT-1b. Planetary transit.svg
The transit method, which can be documented when planets eclipse their star in respect to Earth's position, was used to discover CoRoT-1b.

This star is home to the transiting exoplanet CoRot-1b, the first exoplanet discovered by the CoRoT Mission spacecraft. [9] The planet, which is similar to that of the planet Jupiter's in terms of mass, orbits approximately .02 AU away from its parent star. [5] In comparison, the planet Mercury orbits at approximately .387 AU from the Sun. [10] CoRoT-1b is presumed to be tidally locked to its star. [11]

The planet was the first to be sighted optically rather than through infrared. [12] Unlike other "hot Jupiters," this occurrence seems to imply that the heat transfer between the hemisphere of the planet facing the star and the hemisphere facing away is not significant. [11]

The CoRoT-1 planetary system [13] [14] [9]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b 1.23±0.10  MJ 0.02752+0.00022
−0.00023		1.5089682±0.0000005<0.03685.10±0.50 ° 1.715±0.030  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.

<span class="mw-page-title-main">HD 189733</span> Binary star system in the constellation Vulpecula

HD 189733, also catalogued as V452 Vulpeculae, is a binary star system approximately 64.5 light-years away in the constellation of Vulpecula. The primary star is suspected to be an orange dwarf star, while the secondary star is a red dwarf star. Given that this system has the same visual magnitude as HD 209458, it promises much for the study of close transiting extrasolar planets. The star can be found with binoculars 0.3 degrees east of the Dumbbell Nebula (M27).

<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.

WASP-2 is a binary star system in the Delphinus constellation located about 500 light-years away. The primary is magnitude 12 orange dwarf star, orbited by red dwarf star on wide orbit. The star system shows an infrared excess noise of unknown origin.

<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">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.

<span class="mw-page-title-main">CoRoT-5b</span>

CoRoT-5b is an extrasolar planet orbiting the F type star CoRoT-5. It was first reported by the CoRoT mission team in 2008 using a transit method. This planet has been confirmed by a Doppler follow-up study.

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

Lupus-TR-3 is a star located in the southern constellation Lupus. It has an apparent magnitude of 17.4, making it visible only in power telescopes. Its distance is not well known, but it is estimated to be roughly 2,000 parsecs away from the Solar System.

XO-2 is a binary star. It consists of two components: XO-2S and XO-2N.

<span class="mw-page-title-main">CoRoT-7b</span> Hot Super-Earth orbiting CoRoT-7

CoRoT-7b is an exoplanet orbiting the star CoRoT-7 in the constellation of Monoceros, 489 light-years from Earth. It was first detected photometrically by the French-led CoRoT mission and reported in February 2009. Until the announcement of Kepler-10b in January 2011, it was the smallest exoplanet to have its diameter measured, at 1.58 times that of the Earth and the first potential extrasolar terrestrial planet to be found. The exoplanet has a very short orbital period, revolving around its host star in about 20 hours.

<span class="mw-page-title-main">GSC 03549-02811</span> Main sequence - star in the constellation Draco

GSC 03549-02811, also known as Kepler-1) is a yellow main-sequence star similar to the Sun. This star is located approximately 704 light-years away in the constellation of Draco. The apparent magnitude of this star is 11.41, 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. The age of this star is about 5 billion years.

GSC 02620-00648 is a double star in the constellation Hercules. The brighter of the pair is a magnitude 12 star located approximately 1,660 light-years away. This star is about 1.18 times as massive as the Sun.

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.

CoRoT-3 is a white-yellow dwarf main sequence star hotter than the Sun. This star is located approximately 2560 light-years away in the constellation of Aquila. The apparent magnitude of this star is 13, 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.

CoRoT-7 is a binary star system. The primary, CoRoT-7A is a G-type main sequence star, slightly smaller, cooler, and younger than the Sun. It has an apparent magnitude of 11.67, fainter than Proxima Centauri, the nearest star to the Sun. This star is approximately 520 light-years away from the Solar System in the constellation Monoceros.

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.

<span class="mw-page-title-main">CoRoT-9b</span> Extrasolar planet in the constellation Serpens

COROT-9b is an exoplanet orbiting the star COROT-9, approximately 1500 light years away in the constellation Serpens. COROT-9b's distance of nearest approach to its parent star of approximately 0.36 AU was the largest of all known transiting planets at the time of its discovery, with an orbital period of 95 days. The transit of this planet lasts 8 hours. The planet is at a distance from its star where there is a strong increase in albedo as the temperature decreases, because of the condensation of reflective water clouds in the atmosphere. This suggests its atmosphere may be locked into one of two states: a cloudless state with temperatures between 380 K and 430 K, or covered in water clouds with a temperature in the range 250 K to 290 K.

<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.

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. 1 2 3 4 5 6 7 8 9 10 11 "CoRoT-1". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2009-04-27.
  3. 1 2 "Success of the First CoRoT Satellite Observation: First Exoplanet and First Stellar Oscillations" (PDF). Centre National d'Études Spatiales . Centre National de la Recherche Scientifique. 23 May 2007. Archived from the original (PDF) on 7 April 2010. Retrieved 2009-05-30.
  4. ↑ "COROT Home Page". Convection, Rotation, and Planetary Transits Mission. Centre National D'Études Spatiales (CNES). 2009. Archived from the original on 2008-11-08. Retrieved 2009-05-29.
  5. 1 2 "COROT discovers its first exoplanet and catches scientists by surprise". European Space Agency . European Space Agency. 3 May 2007. Retrieved 2009-05-29.
  6. ↑ "Corot detecta un nuevo planeta más grande que Júpiter". PortalCiencia: Noticias en Astronomía (in Spanish). PortalCiencia.com. 2007. Retrieved 2009-05-29.
  7. ↑ "Stellar Magnitudes". Astrophysics 162 Unit. University of Tennessee. 2008. Retrieved 28 May 2009.
  8. ↑ Evans, D. F; et al. (2016). "High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)". Astronomy and Astrophysics. 589. A58. arXiv: 1603.03274 . Bibcode:2016A&A...589A..58E. doi:10.1051/0004-6361/201527970. S2CID   14215845.
  9. 1 2 Barge, P.; et al. (2008). "Transiting exoplanets from the CoRoT space mission I. CoRoT-Exo-1b: a low-density short-period planet around a G0V star". Astronomy and Astrophysics. 482 (3): L17–L20. arXiv: 0803.3202 . Bibcode:2008A&A...482L..17B. doi:10.1051/0004-6361:200809353. S2CID   16507802.
  10. ↑ "Mercury Statistics". Windows to the Universe program. University Corporation for Atmospheric Research (UCAR). 2003. Archived from the original on 2009-02-21. Retrieved 2009-05-29.
  11. 1 2 Andrea Thompson (2009-05-27). "Exoplanet Phases Seen in Optical Light". Space.com. Retrieved 2009-05-29.
  12. ↑ Ignas A. G. Snellen; Ernst J. W. de Mooij; Simon Albrecht (2009-05-29). "The changing phases of extrasolar planet CoRoT-1b". Nature. 459 (7246): 543–545. arXiv: 0904.1208 . Bibcode:2009Natur.459..543S. doi:10.1038/nature08045. PMID   19478779. S2CID   4347612.
  13. ↑ 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. A107. arXiv: 1704.00373 . Bibcode:2017A&A...602A.107B. doi:10.1051/0004-6361/201629882. S2CID   118923163.
  14. ↑ Sada, Pedro V.; et al. (2012). "Extrasolar Planet Transits Observed at Kitt Peak National Observatory". Publications of the Astronomical Society of the Pacific. 124 (913): 212–229. arXiv: 1202.2799 . Bibcode:2012PASP..124..212S. doi:10.1086/665043. S2CID   29665395.

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