CoRoT's first seven planets: An overview

0.57 MB·

by  R. Dvorak

CoRoT’s first seven planets: An Overview⋆
R.Dvorak1,J.Schneider2,H.Lammer3,P.Barge4,G.Wuchterl5andtheCoRoTteam
1 InstituteforAstronomy,Tu¨rkenschanzstrasse17,A-1180Vienna,Austria
2 LUTH,ObservatoiredeParis-Meudon,5placeJ.Jansen,F-92195Meudon,Paris,France
3 SpaceResearchInstitute,AustrianAcademyofSciences,Schmiedlstrasse6,A-8042Graz,Austria
0 4 Laboratoired’AstrophysiquedeMarseille,TechnopoledeMarseille-Etoile,F-13388MarseilleCedex13,France
1
5 Thu¨ringerLandessternwarteTautenburg,Sternwarte5,D-07778,Tautenburg,Germany
0
2

n
Abstract. Theupto150dayuninterruptedhigh-precisionphotometryofabout100000stars–providedsofar
a
J by theexoplanet channel of the CoRoTspace telescope –gaveanew perspective ontheplanet population of
ourgalacticneighbourhood. Thesevenplanetswithveryaccurateparameterswidentherangeofknownplanet
3
1 propertiesinalmostanyrespect.Giantplanetshavebeendetectedatlowmetallicity,rapidlyrotatingandactive,
spotted stars. CoRoT-3 populated the brown dwarf desert and closed the gap of measured physical properties

] between standard giant planets and very low mass stars. CoRoT extended the known range of planet masses
P down-to 5 Earth masses and up to 21 Jupiter masses, the radii to less than 2 Earth radii and up to the most
E inflatedhotJupiterfoundsofar,andtheperiodsofplanetsdiscoveredbytransitsto9days.TwoCoRoTplanets
. havehost starswiththelowest content ofheavy elementsknown toshow atransit hintingtowardsadifferent
h
planet-host-star-metallicityrelationthentheonefoundbyradial-velocitysearchprograms.Finallytheproperties
p
oftheCoRoT-7bprovethatterrestrialplanetswithadensityclosetoEarthexistoutsidetheSolarSystem.The
-
o detectionofthesecondarytransitofCoRoT-1atthe10−5-levelandtheverycleardetectionofthe1.7Earthradii
r ofCoRoT-7bat3.510−4relativefluxarepromisingevidenceofCoRoTbeingabletodetectevensmaller,Earth
t
s sizedplanets.
a
[

2 1 Introduction Becausethereexistalreadyseveralintroductionarypa-
v pers describing the mission and the instrument in detail
5 (liketheonecitedabovebyBargeetal.)wejustmention
5 The space mission CoRoT is a joint adventure of differ-
themaincharacteristicsofthesatellite:The4mlongand
6 ent European countries, namely CNES, the French space
630kgmassivesatellitehasameandiameterof2m.The
4 agencyas leadingorganisationand other onesin Austria,
accuracyofthepointingis0.5arcsecwithacapacityofthe
2. Brazil, Belgium, Germany and Spain and also the Euro- telemetryof1.5Gbit/day.Threesystemsareoperatingon
1 peanSpaceAgencyESA.Theoriginalgoalwastoobserve
thesatellite:
9 variable stars but – with the discovery of the first exo-
0 planetintheearly90’s–thesearchforexoplanetswasin- 1. CoRoTel is an afocal telescope with 2 parabolicmir-
v: cludedintheresearchprogram(seeSchneiderandChevre- rorsandapertureof27cmacylindricbaffle2mlong,
i ton ([17]) and turned out to be also very important. Al- 2. CoRoTcamisawidefieldcameraconsistingofadiop-
X
ready in the name of the mission CoRoT both research tricobjectiveof6lenseswherethefocalunitisequip-
r tasks are mentioned Convection, Rotation and planetary pedwith4frame-transfer-CCD2048x4096.Twoofthe
a
Transits. The satellite was successfully launched on De- fourCCDs arefortheexoplanetprogramandtwoare
cember, 27th 2006 from Baikonour, observations started fortheseismologyprogram.
in February 2007 and first results concerning extrasolar 3. CoRoTcaseishostingtheelectronicsandthesoftware
planettransitsrespectivelyanoverviewoftheCoRoTmis- managingtheaperturephotometryprocessing.
sionwerepublishedbyBargeetal.[4].Thelife-timewas
scheduledfor3yearsofobservationsandrecentlytheex- For the exoplanet CCD the total number of stars is
tensionforanotherthreeyearswasapproved.Someofthe 12000andthemagnitudesarebetween11and16;theflux
resultsobtainedwithmeasurementsoftheCoRoTmission ismeasuredevery512sconsistingof16individualexpo-
were published in a whole volume of the journalAstron- sures of 32 s. A bi-prism in the focal block dedicated to
omyandAstrophysicsthisyear(Baglinetal.[6]). exoplanetsallowstogetchromaticinformation(red,green
andblue)forbrighterstars,butforfaintstarsonlythestan-
⋆ TheCoRoTspacemissionhasbeendeveloped andisoper- dardoneband(white)photometryisperformed.Thepolar
atedbyCNESwiththecontributionofAustria,Belgium,Brazil, orbitofthesatelliteallowstoobserve150daysinthelong
ESA,GermanyandSpain. run, and between 20 and 30 days in the short run, both
EPJWebofConferences
inthedirectionofthecenterrespectivelyanticenterofthe
milkyway, whichmakestwo reversalmanoeuvresneces-
saryperyear.
Radial velocity measurements to confirm planet can-
didateswereusuallyperformedwiththefollowinginstru-
ments:
1. HARPSspectrographinLaSilla(3.6mtelescope)
2. SOPHIEspectrographintheObservatoiredeHaute
Provence(1.93mtelescope)
3. CORALIE spectrographon the 1.2swiss telescope in
LaSilla
4. Coude´ echelle spectrograph from the 2 m telescope
Tautenburg(TLS)
5. UVESandFLAMESspectrographsinChile
6. SpectrographsatMcDonaldobservatory
Fig. 1. Normalised and phase-folded lightcurve of the best 34
transitsofCoRoT-1b([5]Fig.1).
2 CoRoT-1b: The first planet discoveredby
CoRoT
AlreadythefirstexoplanetdiscoveredbyCoRoTmeasure-
ments was a surprise concerning its nature (Barge et al.
[5]):itturnedouttohaveaverysmalldensity(0.38gcm−3)1
comparedto all otherplanets foundup to now.The short
period of 1.5 days – the light curve is shown in Fig. 1 –
gaveaverywelldeterminedperiodbecause34successive
transits couldbe used forits computation.AdditionalRV
observation(Fig. 2) were undertakenfrom OHP with the
SOPHIE spectrograph for 9 different positions of the ex-
oplanet and confirmed the planetary nature of the transit
of a planetwith a radiusof 1.49R and a mass of 1.03
Jup
M infrontofaG0Vstar.Laterphotometricobservation
Jup
revealedthesecondaryeclipse,whentheplanetdisappears
behindthediscofthestarwhichwasdiscovereddespitea
veryshallownatureofthesignal(Fig.3).
3 CoRoT-2b: a transitingplanet around an
active G star
Fig.2.RVmeasurementsofCoRoT-1bwithSOPHIE([5]Fig.2).
Out of 78 transits duringthe 150 days of observationsof
CoRoT-2b(Alonso etal. [2]) (Fig. 4) the compositelight
curve for the transit (Fig. 5) was derived after removing
the signal of the star’s rotation and activity, which is due
to large spots on its surface. The respective periods were
between 4.5 and 5 days and showed flux variations of a
fewpercents.ThissecondconfirmedplanetofCoRoTor-
bits a K0V star with a metallicity of [Fe/H]=0 in 1.74
days and has a mass of 3.3 M and a radius of 1.465
Jup
RJup.WiththeuseofverypreciseRVmeasurementswith Fig.3.ThesecondaryeclipseofCoRoT-1b([3],Fig.5).
SOPHIE, HARPS and CORALIE it was possible to de-
termine an inclination of λ = 7.2◦ between the planetary
orbit and the equator of the central star ([7]). The radial
velocityanomalyduringthetransitoftheplanet(Fig.6)–
1 Inthetextalltheparametersaregivenwithouttheerrorbars.
The complete values with the estimated errors are given in the
appendix
NewTechnologiesforProbingtheDiversityofBrownDwarfsandExoplanets
Fig. 4. Normalized flux of CoRoT-2b using 78 transits ([2],
Fig.1).
Fig.6.Phase-foldedRVmeasurementsofCoRoT-2bderivedby
SOPHIE and HARPS showing the Rossiter-McLaughlin effect
duringthetransit([7],Fig.1).
Fig.5.Normalizedandphasefoldedlightcurveof78transitsof
CoRoT-2b([2],Fig.2).
theRossiter-McLaughlineffect2 wasmeasuredupto now
only for 5 transiting exoplanets. This new measurements
showed that even fainter stars (m ≤ 12) transited by a
v
planetcanbeusedtodeterminethiseffectwithtelescopes
ofthe2mclass.
Fig.7.LightcurveofCoRoT-3b([8],Fig.2).
4 CoRoT-3b: the first secureinhabitant of
the brown dwarf desert
During the observations of 152 days from space a series
of34transits(Fig.8)couldbemeasuredforayoungF3V
star with a radiusof1.56M with a periodof 4.26days
Sun
(Fig.7).Theresultswereabigsurprisebecausewithara-
diuscomparabletothatofJupiterthemasscouldbedeter-
minedas21.66M whichclearlydistinguishesthisplanet
Jup
from the normal close-in planets (Deleuil et al. [8]): ei-
ther this is a brown dwarf or member of a new class of
planets(Fig.9). Thedeterminationofthemasswasonly
2 Therotationofastarleadstoalinebroadeninginthespec-
Fig.8.LightcurveofCoRoT-3bfor152days([8],Fig.1).
trabecausebythecomingtowardstheobserverandthemoving
away of different parts of the disc, consequently ablueshift re-
spectively a redshift in the star’s spectrum is observable. Now
whentheplanethostingstarisintransit,ithidespartofthedisc
whichcausestheobservedmeanredshifttovaryandthisredshift possible with RV observations from the ground; in addi-
anomalyswitchesfromnegativetopositive(orviceversa)andof tiontothefourmentionedinstruments(HARPS,SOPHIE,
theformofthisanomalytheinclinationoftheplanets’orbitwith CORALIEandTLS,Fig.10)andmeasurementsfromMc-
respecttotheequatorofthestarcanbedetermined. Donaldobservatory.
EPJWebofConferences
Fig.11.FoldedlightcurveforCoRoT-4b([1],Fig.3).
Fig.9.MassradiusdiagramfortransitingplanetswithCoRoT-3b
inthebrowndwarfdesert([8],Fig.10).
Fig.12. RVmeasurementsof CoRoT-4bwithHARPSandSO-
Fig.10.RVmeasurementsofCoRoT-3b([8],Fig.4.)
PHIE([13],Fig.2).
5 CoRoT-4b: a transitingplanet in a
anoutersynchronizedenvelopeofthestarwithdifferential
synchronousorbit surfacerotation.
The planet itself with a radius of 1.2 R and a mass of
Jup
6 CoRoT-5b:a hot-Jupiter-typeplanet
0.71 M is orbiting the host star with a period of 9.2
Jup
daysona circularorbit.The planetwith its mean density
of0.525gcm−3isintheexpectedlocationofaJupiter-like After an observation time of 112 days with 27 transits –
planetinthemass-radiusdiagrambutbecauseofitsperiod Fig. 13 shows the light curve with a decrease in flux of
of almost ten days lies outside of the other hot Jupiters 1.5% – the analysis led to an orbital period of 4 days,
with significantlysmallerperiodsof P ≤ 5 days(Aigrain a radius of 1.4 R and a mass of 0.47 M (Rauer et
Jup Jup
et al. [1], Moutou et al. [13]). The reduction in luminos- al. [16]). The mean density of 0.217 g cm−3 is very low
ity caused by the planets’ transit (Fig. 11) is in the order compared to other gas giants observed up to now3. This
of1.5%.ThesubsequentlyundertakenRVmeasurements means that the planet shows the largest radius anomaly
(Fig.12) with HARPS and SOPHIE confirmed its plane- foundsofar.Thisrelativelyoldstar(5.5-8.3Gyrs)isaF9V
tarynature.Fromthelightcurve(notshownhere)showing star with the mass of the sun and a slightly larger radius.
6cleartransitsduringthecontinuousobservationofalmost Follow-up observations with SOPHIE and HARPS have
60daysonecanseethatthehoststar(ayoungF0Vstarof been undertaken to derive the RV curve (Fig.14) which
onlyabout1Gyrofage)hasanactivesurfacewithrapidly clearly shows the Rossiter-McLaughlineffect. With addi-
evolvingstarspots.Itwaspossibletoderivearotationpe-
riodofP=8.87days,whichiswithinitserrorbarsconsis- 3 only the planets WASP-1b and WASP-15b
tentwiththeperiodoftheplanet.Inadditiontherecouldbe (http://exoplanet.eu)havesuchlowdensities
NewTechnologiesforProbingtheDiversityofBrownDwarfsandExoplanets
Fig.13.Phase-foldedlightcurveofCoRoT-5b([16],Fig.6).
Fig.15.Phase-foldedlightcurveofCoRoT-6b([9],Fig.4).
Fig. 16. RV measurements of CoRoT-6b with SOPHIE ([9],
Fig.14.RVmeasurementsofHARPSandSOPHIEshowingthe Fig.8).
Rossiter-Laughlin effect of CoRoT-5b during the transit ([16],
Fig.2).
the light curve (Fig. 15) and the RV measurements (Fig.
16)aretakenfromof([9]).
tional HARPS observations it was possible to determine
theverylowmetallicity(ratio[M/H]=−0.25).
8 CoRoT-7b:the firstsuper-Earthwith
7 CoRoT-6b: a transitinghot Jupiter planet
measured radius
in a 8.9d orbit around a low-metallicitystar
ThisplanetdiscoveredbyCoRoTturnedouttobeinaan The most exciting result of CoRoT up to now is the dis-
orbit of P=8.89 with approximately 3 Jupitermasses and covery of a Super-Earth planet with a terrestrial density
a radius15percentlargerthanJupiters’ leadingto a high orbiting extremely close to its host star. The G9V star is
densityof1.94gcm−3 (Fridlundetal.[9]).Itishostedby notolderthan2Gyrsandhasametallicityof0.03(Le´ger
a F9V star with approximatelythe massof the Sunand a et al. [11]). CoRoT-7b turnedoutto be in a circular orbit
surprisinglylowmetallicityof[Fe/H =−0.2].Thecombi- in a distance of only approximately4 times the radius of
nationoftheRVmeasurementswiththephotometricones itshoststarwhichcouldbedeterminedbytheanalysisof
from space – respectively ground-based photometric and its153transits.Theplanets’radiusisdeterminedviapho-
spectroscopic observations – led to the full characterisa- tometric and spectroscopic measurements and turned out
tion of the planet and the star. The respective results for to beslightlysmaller than2timestheEarth’sradius(r =
EPJWebofConferences
Fig.17.Superpositionof153transitsofCoRoT-7b([11],Fig.17).
Fig.18.LocationofCoRoT7-binthemass-radiusdiagram([11],
Fig.20).
1.78 R and a mass of M = 4.8 M ) 4. The mean
Earth Earth
densityof5.6gcm−3iscomparabletotheoneoftheEarth,
consequentlywe can speak of an Earth-like planetwhich
movesinonly0.854daysaroundtherelativelyyoungmain
sequence star which has a rotation period of 23 days. A
second planet (Queloz et al. [15]) turned out to be on a
3.89 days orbitand is probablyalso a Super-Earth( m =
8.4 M ).Itseemsthatbothplanetsaremadeofofrocks
Earth
or water and rockssimilar to our Earth which can be un-
derstoodfromFig.18.
BecauseofthesmallestperiodofCoRoT-7bfoundfor
a planet around another star the temperatures will be ex-
tremely high on its surface. Estimations for the tempera-
turesonthedayside(Schneider[18])leadtoatemperature
of about 2000K depending on the rotation of the planet;
due to the vicinity to the star a bounded rotation is very
probable.Thiswouldmeanthatthesilicatesurfaceconsists
oflavaandtheplanets’atmosphereofevaporatedsilicates.
On the contrary the far side could be in the temperature
rangesuchthatwatercouldbeliquidorevenbepresenton
itssurfaceinformofice.InFig.19thereisasketchofthis
planetwhereboundedrotationbecauseoftheactingtides
ofthestarisassumed.This–atleastsomewhatspeculative
–physicalmodelhasbeendrawnbyJ.Schneider([18])but Fig.19.AphysicalmodelofCoRoT-7b([18]).
it characterizeswhat kindof completelydifferentappear-
ancewemayexpectfromthe’hells’planet.
9 The Mass loss of the CoRoT planets due
With these measurements for CoRoT-7b it has been to proximity to the host stars
proven that the satellite is able to discover such planets
as Super-Earth and even smaller ones. From Fig. 17 one
can see that the very small amplitude transits of δF/F ∼ In a recentstudy(Lammeret al. [10])the thermalescape
3.5·10−4isclearlynotthelimitofdetection. of hydrogenatomsfrom 57 transiting exoplanetswas de-
termined and a modified energy-limited mass loss equa-
tionapplied,whichreproducesthefullhydrodynamicap-
proachofstudies(e.g.[14]).Byapplyingthesamemethod
totheexoplanetsdiscoveredbyCoRoTintegratedoverthe
4 Thesevaluesaretakenfromthesecondpaperonthisplanet life time of the planetary system we obtain for the given
([15]); RV measurements in the first paper ([11]) were used to planetaryandstellarparametersthethermalmasslossrates
excludenonplanetarycompanions. showninTable3.
NewTechnologiesforProbingtheDiversityofBrownDwarfsandExoplanets
Depending on the chosen stellar EUV-related heating observation a confirmation of a planet found around an-
efficiencyηof10%or25%whichcorrespondstothera- otherstarcanbeattested.
tioofthenetlocalgasheatingratetotherateofstellarra- TheplanetsfoundbyCoRoTareofextraordinaryvalue
diativeenergyabsorption,onecanseethatCoRoT-1band fortheextrasolarplanetaryresearchinastronomybecause
CoRoT-5blostduringtheirlife-timeabout1.3%and1.56 ofthecompletecharacterisationoftheplanets.Onecansee
%(η=10%)or3.07%and3.75%(η=25%)oftheirini- thatmostoftheCoRoTplanetsaregiantgasplanets(radii
tialmasses.ThethermalmasslossofCoRoT-2b,CoRoT- between 0.97 ≤ R ≤ 1.49. The largest ones (CoRoT-
Jup
3b,CoRoT-4bandCoRoT-6barelowerandthereforeneg- 1b and 4b) are also very close to the host star having the
ligible. The stronger mass loss effect for CoRoT-1b and shortest periods (1.51 and 1.74 days respectively) which
CoRoT-5barerelatedtothelowerplanetarydensity,orbital is a clear sign of the important role of the star radiation
distanceandstellarparameterssothattheRochelobebe- ontheradiusevolution.CoRoT-4andCoRoT-6hostplan-
comesarelevantfactorinthemasslossevolutionofthese ets which have a synchronizedperiod with respect to the
planets. host stars’ rotation. Concerningthe metallicity it is inter-
RecentlyLeitzingeretal.([12])presentedthermalmass estingtonotethatthreeofthefivehotJupitersdetectedare
loss calculations over evolutionarytime scales to investi- orbiting metalpoor stars, which is in contradictionto the
gatewhetherCoRoT-7bcouldbearemnantofaninitially normalmetallicityrelationsfoundbyRVsearches.Aslast
more massive hydrogen-richgas giant. The thermalmass point it should be emphasized that the domain of planet
loss results of these authors indicate that CoRoT-7b can- masses covered by the CoRoT planets is within a wide
notbearemnantofathermallyevaporatedJupiterlikegas range,namelyfromtheverymassiveCoRoT-3bplanet(with
giant.AscenariothatCoRoT-7bis aremnantofanevap- 21.6 M ) to the telluric planetCoRoT-7b(0.015 M ).
Jup Jup
oratedlowdensity’hotsub-Uranus’or’hotsub-Neptune’ Another new aspect is the discovery of close-in planets
is also veryunlikely butcan notbe completelyexcluded. (CoRoT-7band7c).Thiscanberegardedashintthat–like
Suchanevaporationscenariowouldneed,besideslowini- in our Solar System – planetary systems are ’full’. This
tialdensityoftheplanet,alsoaheatingefficiencyofabout meansthatinbetweentwoplanetsnootherbiggerobjects
25% instead of more realistic 10% and an unlikely short (exceptionsareasteroids)mayexistonstableorbits.
exosphereformationtimeoflessthan50Myr.Fromthese The presentationof the major resultsin thisoverview
simulationsonecanconcludethatCoRoT-7bwasmostlike- is byfar notcomplete– e.g.we did notspeakabouttime
lyneveragasoricegiantwhichhaslostitsentirehydrogen transit variations (TTV) – which have also been detected
envelope,butstarteditsevolutionasa’super-Earth’which insomeofthedataandmaybecausedbyadditionalplan-
couldhavelostathinhydrogenenvelope. etsinthesystem.Onlytheresultsoftheconfirmedplanets
The efficiency of the CoRoT exoplanet mass loss is havebeenpresented5,butthesignalsofmanymoreplanets
connectedtotheRochelobeeffecttogetherwithlowplane- seemtobestillinourdataliketheonesofplanetsaround
tarydensities.Dependingonthestellarluminosityspectral double stars. But they can be confirmed only after diffi-
type,initialplanetarydensity,stellar EUV-relatedheating cult and long analysis combined with observations from
efficiency,orbitaldistance,andtheconnectedRochelobe theground.
effect,onecanexpectthatatorbitaldistances≤0.015AU,
lowdensityhotgasgiantsinorbitsaroundsolartypestars
mayevenevaporatedowntotheircoresize.Therefore,var-
11 Appendix
ioussizeandmasstypeobjectsshouldbediscoveredinthe
nearfuture.
In table 1 the astrophysical parameters of the host stars
arelisted,intable2welistedtheorbitalparametersofthe
detectedplanetsandintable3thephysicalparametersare
10 Conclusions and synopsisof the giventogetherwithanestimationofthemasslossduetothe
results proximitytothestar.Alldataaretakenfromtherespective
publicationsgiveninthetext.
TheobservationsfromspacewiththesatelliteCoRoTtur-
nedouttohaveveryinterestingresultsfortheknowledge
ofthediversityofplanetsandplanetarysystems.Thecon- 12 Acknowledgements
tinuous surveillance of 100000 stars for a period of 150
days is very efficient to detect close by planets (with pe- The LAM team and the Austrian team thanks CNES re-
riods between Venus and Mercury and smaller) and even spectively ASA for fundingthe CoRoT project. The IAC
allowsto’see’smallplanetstransitinginfrontofthestar’s teamacknowledgesthesupportofgrantsoftheEducation
diskwithaverysmalldecreaseinthefluxlikeforCoRoT- and Science Ministry. The German team (TLS and Univ.
7b. But to get absolute planetaryparametersfor the mass Cologne) acknowledges the support of DLR grants. For
and the radius it is necessary to make extensive spectro- readingthemanuscriptandpreparinganappropriateoutlay
scopic measurementsand also to have a goodknowledge ofthepicturesR.D.needstothankA.Bazso´ andV.Eybl.
of the astrophysical parameters of the host star. Only af-
tercarefulanalysisofthelightcurves(contaminationmay 5 Intheappendixweshowthestarparametersandthederived
causea’false’alarm)incombinationwiththoroughground parametersfortheplanetsaspublishedintheoriginalpapers
EPJWebofConferences
Table1.Theastrophysicalparametersofthehoststars Table3.Thephysicalpropertiesoftheplanets
star type M/M age[Gyrs] [Fe/H] planet M/M R/R ̺[gcm−3] Massloss[%]
sun jup jup
CoRoT-1 G0V 0.95 ? -0.3 CoRoT-1b 1.03 1.49 0.38 1.3–10.81
±0.15 ±0.25 ±0.12 ±0.08
CoRoT-2 K0V 0.97 ? 0.0 CoRoT-2b 3.31 1.465 1.31 0.06–0.59
±0.06 ±0.1 ±0.16 ±0.029
CoRoT-3 F3V 1.37 2.0+0.8 -0.02
−0.4 CoRoT-3b 21.66 1.01 26.4 0.0002–0.0017
±0.09 ±0.06
±1.00 ±0.07
CoRoT-4 F0V 1.1+0.03 1.0+1.0 0.0
−0.02 −0.3
±0.15 CoRoT-4b 0.72 1.19 0.525 0.12–1.212
CoRoT-5 F9V 1.0 6.9 -0.25 ±0.08 −+00..0056
±0.02 ±1.4 ±0.06 CoRoT-5b 0.467 1.388 0.217 1.56–12.78
CoRoT-6 F5V 1.055 ? -0.2 +0.067 +0.046
±0.055 ±0.1 CoRoT-6b −20.9.0624 −10.1.06476 1.94 ≤1%
CoRoT-7 G9V 0.93 1.5−+00..38 0.03 ±0.34 ±0.035
±0.03 ±0.06
CoRoT-7b 0.015 0.172 4.23 ?
±0.003 +0.022
−0
Table2.Theorbitalelementsoftheplanets CoRoT-7c 0.026 ? ? ?
±0.003
planet Period[d] a[AU] inc[deg] ecc
CoRoT-1b 1.508956 0.0254 85.1 0
8. Deleuil, M., Deeg, H.J., Alonso, R. et al.: As-
±6e−6 ±0.0004 ±0.5
tron.Astrophys.491(2008)889–897
CoRoT-2b 1.742996 0.0281 87.84 0
9. Fridlund, M., He´brard, G., Alonso, R. et al.: As-
±2e−6 ±0.0009 ±0.1
tron.Astrophys.(inprint)(2009)
CoRoT-3b 4.2568 0.057 85.9 0 10. Lammer, H., P. Odert, M. Leitzinger et al.: As-
±5e−6 ±0.003 ±0.8 tron.Astrophys.506(2009)399–410
CoRoT-4b 9.20205 0.090 90.0 0+0.1 11. Le´ger, A., Rouan, D., Schneider, J. et al.: As-
−0
±37e−5 ±0.001 +0 tron.Astrophys.506(2009)287–302
−0.085
CoRoT-5b 4.037896 0.04947 85.83 0.09 12. Leitzinger,M.,P. Odert,H.Lammeretal.:submitted
±2e−6 +0.00026 +0.99 +0.09 toPlanet.SpaceSci.
−0.00029 −1.38 −0.04
13. Moutou, C., Bruntt, H., Guillot, T. et al.: As-
CoRoT-6b 8.886593 0.0855 89.07 <0.1
±4e−6 ±0.0015 ±0.3 tron.Astrophys.488(2008)L47–L50
14. Penz,T.,Erkaev,N.V.;Kulikov,Yu.N. etal.:Plane-
CoRoT-7b 0.85358 0.0172 80.1 0
taryandSpaceScience56(2008)1260-1272
±2e−5 ±0.0003 ±0.3
15. Queloz, D., Bouchy, F., Moutou, C. et al.: As-
CoRoT-7c 3.698 0.046 ? 0
tron.Astrophys.506(2009)303–319
±0.003
16. Rauer, H., Queloz, D., Csizmadia, Sz. et al.: As-
tron.Astrophys.506,(2009)281–286
17. Schneider, J., Chevreton, M.: Astron.Astrophys. 232
References (1990)251–257
18. SchneiderJ.(CESTmeeting,February2009,Paris)
1. Aigrain,S.,CollierCameron,A.,Ollivier,M.etal.:As-
tron.Astrophys.488(2008)L43–L46
2. Alonso, R., Auvergne, M., Baglin, A.: As-
tron.Astrophys.482(2008)L21–L24
3. Alonso,R.,Alapini,A.,Aigrain,S.:Astron.Astrophys.
506(2009)353–358
4. Barge, P., Baglin, A., Auvergne, M. and the CoRoT
team,inSun,Y.-S.etal,Ferraz-MelloS.andZhou,J.-L.
eds.:Exoplanets,FormationandDynamics,IAUSympo-
sium249(2008)3–16
5. Barge, P., Baglin, A., Auvergne, M. et al.: As-
tron.Astrophys.482(2008)L17–L20
6. Baglin,A.,Aerts,C.,Guillot,T.:Astron.Astrophys.506
(2009)2–572
7. Bouchy, F., Queloz, D., Deleuil, M. et al.: As-
tron.Astrophys.482(2008)L25–L28