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CoRoT-1

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Yellow dwarf star in the constellation Monoceros
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CoRoT-1

An artist's depiction of CoRoT-1 and its "hot Jupiter" exoplanet
Observation data
Epoch J2000.0Equinox ICRS
Constellation Monoceros [1]
Right ascension 06h 48m 19.1724s[2]
Declination −03°06′07.711′′[2]
Apparentmagnitude(V) 13.6[3]
Characteristics
Evolutionarystage main sequence [2]
Spectraltype G0V[3]
Apparent magnitude(V) ~13.6[3]
Apparentmagnitude(I) 12.88 ±0.04[3]
Apparentmagnitude(J) 12.462 ±0.029[3]
Apparentmagnitude(H) 12.218 ±0.026[3]
Apparentmagnitude(K) 12.149 ±0.027[3]
Variabletype Pulsating variable [4]
Astrometry
Proper motion (μ) RA:−5.978(16) mas/yr [2]
Dec.:0.570(14) mas/yr [2]
Parallax (π)1.3000±0.0167mas [2]
Distance 2,510 ± 30ly
(769 ± 10pc)
Details
Mass 1.3[5] M☉
Radius 1.3[5] R☉
Luminosity 2.4[5] L☉
Surface gravity (logg)4.32[5] cgs
Temperature 6,355[5] K
Metallicity 0.03[6]
Rotational velocity (vsini)4.70[6] km/s
Age 1.0–6.5[6] 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[3]
Database references
SIMBAD data

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.[3] 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.

Nomenclature

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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;[7] 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.[8] The numerical designation was assigned because the first exoplanet discovered by the CoRoT telescope was found in orbit of this star.[9] CoRoT-1 does not have a common or colloquial name like that of Sirius or Procyon.

Characteristics

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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.[3] At an apparent magnitude of approximately +13.6,[3] doubly dimmer than the dimmest star visible with the naked eye, CoRoT-1 cannot be seen from Earth without magnification apparatus.[10]

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.[11]

Variability

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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.[4]

Planetary system

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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.[12] 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.[8] In comparison, the planet Mercury orbits at approximately .387 AU from the Sun.[13] CoRoT-1b is presumed to be tidally locked to its star.[14]

The planet was the first to be sighted optically rather than through infrared.[15] 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.[14]

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The CoRoT-1 planetary system[16] [17] [12]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination
(°) 		Radius
b 1.23±0.10MJ 0.02752+0.00022
−0.00023		 1.5089682±0.0000005 <0.036 85.10±0.50 1.715±0.030RJ

See also

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References

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  1. ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific . 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034 . Constellation record for this object at VizieR.
  2. 1 2 3 4 5 6 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.
  3. 1 2 3 4 5 6 7 8 9 10 11 "CoRoT-1". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2009年04月27日.
  4. 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年05月30日.
  5. 1 2 3 4 5 Stassun, Keivan G.; et al. (2019). "The Revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694 . Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467 .
  6. 1 2 3 Llorente De Andrés, F.; Chavero, C.; de la Reza, R.; Roca-Fàbrega, S.; Cifuentes, C. (2021). "The evolution of lithium in FGK dwarf stars. The lithium-rotation connection and the Li desert". Astronomy and Astrophysics. 654. arXiv:2108.05852 . Bibcode:2021A&A...654A.137L. doi:10.1051/0004-6361/202141339.
  7. ↑ "COROT Home Page". Convection, Rotation, and Planetary Transits Mission. Centre National D'Études Spatiales (CNES). 2009. Archived from the original on 2008年11月08日. Retrieved 2009年05月29日.
  8. 1 2 "COROT discovers its first exoplanet and catches scientists by surprise". European Space Agency . European Space Agency. 3 May 2007. Retrieved 2009年05月29日.
  9. ↑ "Corot detecta un nuevo planeta más grande que Júpiter". PortalCiencia: Noticias en Astronomía (in Spanish). PortalCiencia.com. 2007. Retrieved 2009年05月29日.
  10. ↑ "Stellar Magnitudes". Astrophysics 162 Unit. University of Tennessee. 2008. Retrieved 28 May 2009.
  11. ↑ 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 .
  12. 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 .
  13. ↑ "Mercury Statistics". Windows to the Universe program. University Corporation for Atmospheric Research (UCAR). 2003. Archived from the original on 2009年02月21日. Retrieved 2009年05月29日.
  14. 1 2 Andrea Thompson (2009年05月27日). "Exoplanet Phases Seen in Optical Light". Space.com. Retrieved 2009年05月29日.
  15. ↑ Ignas A. G. Snellen; Ernst J. W. de Mooij; Simon Albrecht (2009年05月29日). "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.
  16. ↑ 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 .
  17. ↑ 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 .
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