exoplanet- asteroseismology synergies bill chaplin, school of physics & astronomy university of...
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Exoplanet-Asteroseismology
Synergies
Bill Chaplin, School of Physics & Astronomy University of Birmingham, UK
EAHS2012, Oxford, 2012 March 15
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Oscillations as clocks: FM stars
Shibahashi & Kurtz (2012), MNRAS, submitted (arXiv:1202.0105)
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Oscillations as clocks: V391 Peg
Silvotti et al. (2007), Nature, 449, 189
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O-C diagram, prominent oscillation frequencies of V391 Peg
Silvotti et al. (2007), Nature, 449, 189
Frequency #1 Frequency #2
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Understanding stellar systems like our own…
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Evolution and properties of stellar systems Precise, accurate fundamental stellar
properties for modelling exoplanet systems: Seismic densities, radii, masses, ages Seismic log(g) for “boot strapping”
spectroscopic analysis
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Internal rotation, stellar angle of inclination:Constraints on dynamical histories of stellar
systems
Evolution and properties of stellar systems
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Intrinsic activity, variability of host stars, influence on local environment: “Sound” stellar activity cyclesDepths of convective envelopes, tests of
stellar dynamos
Evolution and properties of stellar systems
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asteroFLAG Hare and Hounds
Stello, Chaplin et al. 2009, ApJ
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asteroFLAG Hare and Hounds
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Asteroseismic ensemble tests Kepler Input Catalogue
Finds an underestimation bias in KIC radii
Verner et al., 2011, ApJ, 738, L28
KIC – seismic log g (dex) KIC – seismic radii (%)
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Inferences on stellar activity, stellar cycles, activity of the “Sun in time”
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Sun (SOHO/VIRGO)
Kepler: Gtype dwarf
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Sun (SOHO/VIRGO)
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Frequency spectrum of Cyg
Solar-like oscillations
Granulation
Activity
Guzik et al. (2012), in preparation
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Stellar activity suppresses oscillationsInference on magnetic fields and convection
Detected oscillations? noyes
Pro
xy fo
r “s
tella
r ac
tivity
”
Chaplin et al., 2011, ApJ, 732, 5L
Teff (K)
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Broomhall et al., 2009, ApJ, 700, L162
“Sounding” stellar activity cycles: Sun
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Broomhall et al., 2012, ApJ, 420, 1405
Quasi-biennial variationAfter removal of 11-yr cycle signature
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CoRoT reveals a short activity cycle in HD49933
García et al., 2010, Science, 329, 1032
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One example from the seismic Zoo
Oscillation amplitudes
Oscillation frequencies
Light curve
Variation of seismic frequencies and amplitudes
Courtesy Salabert (Elsworth et al., work in progress)
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Inference on distribution:- From frequency shifts of different modes- From frequency asymmetry of components
of non-radial modes
Inference: surface distribution of activity sizes and phases of frequency shifts depend on (l, m)
Chaplin (2011), Proceedings Tenerife Winter School
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Activity distribution: non homogeneous, preferred bands of latitude
Response of modes: depends on (l, m)
Inference: surface distribution of activity sizes and phases of frequency shifts depend on (l, m)
Chaplin (2011), Proceedings Tenerife Winter School
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Effects of near-surface activity on modes Depends on spherical harmonic of mode (l, m)
(1,0) (1,1) (2,0)
(3,0)(2,2)(2,1)
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Chaplin et al. 2007, MNRAS, 377, 17
Spatial dependence of the frequency shifts
Inference on active latitudes
Predicted shifts simple model for
latitudinal distribution
surface activity
Match to observed ratios
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Chaplin et al. 2007, MNRAS, 377, 17
Spatial dependence of the frequency shifts
Inference on active latitudes
Predicted shifts simple model for
latitudinal distribution
surface activity
Match to observed ratios
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Chaplin et al. 2007, MNRAS, 377, 17
Spatial dependence of the frequency shifts
Inference on active latitudes
Predicted shifts simple model for
latitudinal distribution
surface activity
Match to observed ratios
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Chaplin et al. 2007, MNRAS, 377, 17
Spatial dependence of the frequency shifts
Inference on active latitudes
Predicted shifts simple model for
latitudinal distribution
surface activity
Match to observed ratios
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Inference: surface distribution of activity sizes and phases of frequency shifts depend on (l, m)
Chaplin (2011), Proceedings Tenerife Winter School
Sun-as-a-star data
max=40 ± 10 degrees
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Stellar activity squashes mode peaks!
3.0
0.15
= 0.0
1.50.4
See Chaplin et al., 2008, MNRAS, 384, 1668
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Credit: IAC
Asteroseismic analysis
Kepler Objects of Interest
(KOIs)
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Seismology of exoplanet host stars
HAT-P-7 Christensen-Dalsgaard et al. 2010
Kepler-10b Batalha et al. 2011
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Howell et al. (2012), ApJ, 746, 123
Kepler 21b 1.6RE planet orbiting bright F-type sub-giant
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Brightest Kepler exoplanet host star High-precision stellar properties from
asteroseismology: Stellar radius to 2.2% Stellar mass to 4.5% Stellar age to 12%
Planetary radius to 2.4%
Kepler 21b 1.6RE planet orbiting bright F-type sub-giant
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Kepler 22b 2.4RE planet in habitable zone of Sun-like star
Borucki et al. (2012), ApJ, 745, 120
Strong signature of large frequency
separation
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Inclination affects mode visibility
(1,0) (1,1) (2,0)
(3,0)(2,2)(2,1)
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Inclination affects mode visibility
Gizon & Solanki, 2003, ApJ, 589, 1009
m=1 0 +1 m=2 0 +11 +2
l =1 l =2
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Inference on stellar inclination
Height ratios depend on
angle
2 yrs
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1 month Need long datasets
Inference on stellar inclination
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Fin