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Asteroseismology with the Corot and Kepler Space Missions

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Asteroseismology with the Corot and Kepler Space Missions Asteroseismology with the CoRoT and Kepler space missions ComparisonComparison spacespace versusversus groundground high-precisionhigh-precision spectroscopyspectroscopy versusversus spacespace photometryphotometry SoHO photometry data of the Sun spectroscopy p. 2 Leuven and Nijmegen Universities CNES-ledCNES-led CoRoTCoRoT spacespace missionmission SpaceSpace photometer,photometer, mountedmounted onon 0.27m0.27m mirror,mirror, VmagVmag 55 toto 1616 LaunchedLaunched 2626 DecemberDecember 20062006 Goal:Goal: asteroseismologyasteroseismology andand detectiondetection ofof exoplanetsexoplanets p. 3 Leuven and Nijmegen Universities CoRoTCoRoT focalfocal planeplane Seismology field Exoplanet field highly defocused focused + prism Focal block 10 targets 12000 targets 5.4<V<9 11<V<16 sampling 1 s sampling 512 s 4 CCDs 2000x4000 px 2.6 ° Frame transfer > 100 stars in the Seismo-field > 100000 stars in the Exo-field 1.3 ° p. 4 Leuven and Nijmegen Universities NASANASA KeplerKepler spacespace missionmission SpaceSpace photometer,photometer, mountedmounted onon 0.95m0.95m mirror,mirror, VmagVmag 99 toto 1616 LaunchedLaunched 77 MarchMarch 20092009 Goal:Goal: detectiondetection ofof Earth-likeEarth-like planetsplanets inin habitablehabitable zonezone ofof starsstars p. 5 Leuven and Nijmegen Universities KeplerKepler spacespace missionmission Monitors > 100000 solar-like stars at ultra-high precision Planet discoveries through transit method 10 confirmed so far, 700 candidates Kepler10b has R=1.4 Earth R (NASA PR, Jan.2010) p. 6 Leuven and Nijmegen Universities Kepler©sKepler©s asteroseismology:asteroseismology: why?why? UnderstandingUnderstanding formationformation andand evolutionevolution ofof planetaryplanetary systems:systems: PlanetPlanet sizesize andand composition:composition: wewe wantwant hosthost starstar massesmasses andand radiiradii PlanetPlanet ageage == hosthost starstar ageage ToTo improveimprove drasticallydrastically stellarstellar evolutionevolution modelsmodels acrossacross HRDHRD andand allall fieldsfields inin astrophysicsastrophysics thatthat relyrely onon itit p. 7 Leuven and Nijmegen Universities Solar-like Oscillations in unevolved stars FirstFirst CoRoTCoRoT resultsresults :: AFAF starsstars 6th 7th 8th Michel et al. (2008): lower amplitudes, granulation 3x solar p. 9 Leuven and Nijmegen Universities ExoplanetExoplanet hosthost starstar seismology:seismology: HAT-P-7HAT-P-7 Kepler data (JCD et al. 2010): average density = 0.2712 ± 0.0032 g/cm^3 M=1.520 ± 0.036 Msun , R=1.991 ± 0.018 Rsun age = 2.14 ± 0.26 Gyr Largest limiting factor: unknown convective overshooting in models... p. 10 Leuven and Nijmegen Universities KeplerKepler asteroseismologyasteroseismology Kallinger et al (2010): disentangling of granulation, stellar activity and oscillations IMPORTANT in context of exoplanetary formation and evolution of angular momentum p. 11 Leuven and Nijmegen Universities KeplerKepler ensembleensemble asteroseismologyasteroseismology The power of mixed modes when deducing stellar ages Stellar ages factor 10 better than classical methods (see Soderblom, ARA&A, 2010): Chonology of stellar and planetary systems! p. 12 Leuven and Nijmegen Universities Red-Giant Asteroseismology : from stars to populations FirstFirst CoRoTCoRoT resultsresults :: redred giantsgiants ℓ=0 ℓ=1 ℓ=2 De Ridder et al. (2009): > 100s new exo RG pulsators p. 14 Leuven and Nijmegen Universities FirstFirst CoRoTCoRoT resultsresults :: redred giantsgiants DeDe RidderRidder etet al.al. (2009):(2009): observations in sismo and exo CCDs numerous RG pulsators found in exo data non-radial pulsations!! both short and long mode lifetimes: few to tens of days opens up red part of HRD for asteroseismology p. 15 Leuven and Nijmegen Universities CoRoT:CoRoT: populationpopulation seismologyseismology Miglio et al. (2009): population synthesis combined with asteroseismology in large sample of RG recent starburst or not? No longer restricted to individual stars, but entire populations and probing of the structure and evolution of the Milky Way! p. 16 Leuven and Nijmegen Universities KeplerKepler redred giants:giants: beautiful!!beautiful!! (Q1)(Q1) Red clump red giants Low-luminosity giants on RGB: rare! Granulation Bedding et al. (2010), Hekker et al. (2010), Huber et al. (2010), Kallinger et al. (2010) : much more to come!! (embargoed...) p. 17 Leuven and Nijmegen Universities SeismologySeismology ofof pulsatorspulsators inin EBs:EBs: timing!...timing!... Transit signal Hekker et al. (2010) ingress ingress • RR = 11.8 ± 0.6 Rsun LR = 58 ± 6 Lsun MR = 1.7 ± 0.3 Msun egress egress ⇒ • Eclipse depth = 9% L2 = 5.2 ± 0.7 Lsun thus M2 = 1.44 ± 0.05 Msun • Eclipse time = 1.64 ± 0.01 d, total eclipse Ingress/egress time = 0.276 ± 0.007 d • R ≤ 1.7 ± 0.1 R T = 6700 ± 200 K R2 ≤ 1.7 ± 0.1 Rsun Teff,2 = 6700 ± 200 K p. 18 Leuven and Nijmegen Universities Massive Star Asteroseismology : some unexplainable suprises... Pre-SpacePre-Space resultsresults forfor BB starsstars CompatibleCompatible withwith EBEB && isochroneisochrone fittingfitting Ref. Star Mass (M☼) SpT αov (Hp) ΩR(km/s) Ωcore/Ωenv (1) HD 16582 10.2 ± 0.2 B2IV 0.20±0.10 28(14?) (2) HD 29248 9.2 ± 0.6 B2III 0.10±0.05 6±2 ~5 (3) HD 44743 13.5 ± 0.5 B1III 0.20±0.05 31±5 (4) HD 129929 9.4 ± 0.1 B3V 0.10±0.05 2±1 3.6 (5) HD 157056 8.2 ± 0.3 B2IV 0.44±0.07 29±7 ~1 (1) Aerts et al.al. (2006): 20 d MOST photometry + 1 week spectra (2) Pamyatnykh et al. (2004); Ausseloos et al. (2004): 5 months multisite photometry + spectroscopy (3) Mazumdar et al. (2006): 4 years high-resolution spectroscopy (4) Aerts et al. (2003, 2004); Dupret et al. (2004): 20 years photometry (5) Briquet et al. (2007): 2 years spectroscopy + few months photometry p. 20 Leuven and Nijmegen Universities CoRoTCoRoT datadata ofof aa BetaBeta CepCep starstar HDHD 180642180642 discovereddiscovered fromfrom HIPPARCOSHIPPARCOS (Aerts(Aerts 2000)2000) SpTSpT B1.5II/III,B1.5II/III, dominantdominant nonlinearnonlinear radialradial modemode CoRoTCoRoT 379785379785 datapoints,datapoints, 32sec32sec integration,integration, 156.6156.6 daysdays WorkedWorked inin flux,flux, notnot magnitude;magnitude; linearlinear trendtrend removedremoved p. 21 Leuven and Nijmegen Universities HDHD 180642:180642: LCLC modellingmodelling DominantDominant modesmodes (in(in µµHz):Hz): 63.5056663.50566 (5(5 harmonics),harmonics), 3.462623.46262 (3(3 harmonics),harmonics), 73.20389,73.20389, 97.32853,97.32853, 83.96709,83.96709, 136.70880136.70880 EvolutionaryEvolutionary frequencyfrequency decreasedecrease ofof 0.0270.027 sec/yearsec/year p. 22 Leuven and Nijmegen Universities CoRoTCoRoT datadata ofof aa BetaBeta CepCep starstar f1 f2 f3 f5 f4 f1+f3 p. 23 Leuven and Nijmegen Universities HDHD 180642:180642: LCLC modellingmodelling PeriodogramPeriodogram afterafter prewhiteningprewhitening ofof dominantdominant modemode LightLight gray:gray: smoothedsmoothed overover 0.1/d,0.1/d, dark:dark: overover 2/d2/d SignatureSignature ofof nonlinearnonlinear modemode couplingscouplings occuroccur >> 1919 3-resonance3-resonance freqsfreqs ++ ...... somesome additionaladditional stochastic?stochastic? Star is most evolved of all known Beta Cephei stars, near TAMS Rotational splitting ?; theoretical modelling is ongoing (standard MI methods do not work due to nonlinearity...) p. 24 Leuven and Nijmegen Universities CoRoTCoRoT datadata ofof anan O9VO9V starstar f1 f2 f3 HD 46202, O9V none of detected freqs f5 predictedf4 to be f1+f3 excited... p. 25 Leuven and Nijmegen Universities CoRoTCoRoT datadata ofof aa O8O8 binarybinary f1 f2 f3 HD 46149, an O8V+B Porb=829d, e=0.59 1 2 M =35M¯, M =19M¯ Stochastic oscillations following scaling law of solar-like stars: f4 f1+f3 unknown convection... p. 26 Leuven and Nijmegen Universities Pre-CoRoTPre-CoRoT resultsresults forfor AFAF starsstars αov (Hp) ?? Ω(r) ?? seismic modelling not successful due to lack of mode id. numerous frequency detections from ground networks and Breger et al. (2005) MOST team p. 27 Leuven and Nijmegen Universities Problem:Problem: mergedmerged multipletsmultiplets ℓ=0 Fourier Spectrum ℓ=2 (c/d) Rotation splits each mode in 2ℓ +1 unequidistant components Example shown: simulated 1.8 Msun Delta Scuti star (Goupil et al., 2000) p. 28 Leuven and Nijmegen Universities CoRoTCoRoT datadata ofof aa newnew DeltaDelta SctSct starstar GroundGround basedbased th 9 mag star limitlimit afterafter severalseveral weeksweeks MichelMichel etet al.al. (2009)(2009) p. 29 Leuven and Nijmegen Universities CoRoTCoRoT datadata ofof DeltaDelta SctSct starstar ªConstantº A star of 9th mag MichelMichel etet al.al. (2009):(2009): modellingmodelling ongoingongoing 100s of peaks still significant p. 30 Leuven and Nijmegen Universities Compact Star Asteroseismology with Kepler KeplerKepler CompactCompact PulsatorPulsator SurveySurvey New discoveries among 110 surveyed stars 1. Cataclysmic variables: - Nova like: 2 - AM CVn: 1 2. Compact binaries: - eclipsing sdB+DM: 1 - non-eclipsing beaming sdB+DM: 2 - eclipsing pulsating sdB+DM: 1 - non-eclipsing sdO+dM: 1 - pulsating sdO/B+ F/G/K secondaries: 10 p. 32 Leuven and Nijmegen Universities SomeSome nicenice results:results: sdBsdB ++ DMDM Gravity-mode pulsations in compact binaries Kawaler et al. (2010) p. 33 Leuven and Nijmegen Universities NiceNice result:result: hybridhybrid pulsatorpulsator EBEB Physics of NRP at extreme irradiation? Porb = 0.125765300(21)d, (éstensen et al. 2010) p. 34 Leuven and Nijmegen Universities DiscoveryDiscovery ofof AMAM CVnCVn starstar inin FoVFoV AM CVn nature deduced from spectroscopy
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