Measuring Stellar Properties with Asteroseismology and ... · Asteroseismology and Interferometry...
Transcript of Measuring Stellar Properties with Asteroseismology and ... · Asteroseismology and Interferometry...
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Measuring Stellar Properties with Asteroseismology and Interferometry
Tim White Georg-August-Universität Göttingen
Solar-Seminar – Max Planck Instutut für Sonnensystemforschung – 29 April 2014
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Kepler-186f
NASA Ames/SETI Institute/JPL-Caltech
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• Show cover of Science article, transit.
• This planet is interesting because it is in the habitable zone and Earth-sized.
• How do we know it’s Earth-sized?
Science, April 18 2014, Vol 344, Page 277
R*=0.472±0.052 R
Rplanet=1.11±0.14 R
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Planet Validation
Seager & Mallen-Ornélas 2003
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Galaxy Formation
E. L. Wright (UCLA), The COBE Project, DIRBE, NASA
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Source: Ivan Baldry Samland & Gerhard, 2003
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Asteroseismology
Arentoft et al. 2008
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figure by Daniel Huber
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figure by Daniel Huber
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figure by Daniel Huber
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figure by Daniel Huber
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Huber et al. 2011, ApJ, 743, 143
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16 Cyg A
The Sun
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Δν
νmax
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From oscillations to stellar parameters
1) Scaling relations 2) Grid method 3) Detailed modelling
M, R, age
Δν, νmax [Fe/H] log(g)
Teff
ν1,…, νn [Fe/H] log(g) Teff, ...
M, R, age
Difficulty Precision
M, R
Δν νmax Teff
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21
3
/
R
Mν
eff2ac
TR
Mνν max
Ideal gas Adiabatic Oscillations Isothermal Atmosphere
Tassoul (1980) Brown et al. (1991)
1) Scaling relations
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Why care about scaling relations?
21
3
/
R
Mν
eff2ac
TR
Mνν max
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• They tell you
– Density
– Surface gravity
– Radius
– Mass
Without the need for detailed modelling!
Why care about scaling relations?
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From oscillations to stellar parameters
1) Scaling relations 2) Grid method 3) Detailed modelling
M, R, age
Δν, νmax [Fe/H] log(g)
Teff
ν1,…, νn [Fe/H] log(g) Teff, ...
M, R, age
Difficulty Precision
M, R
Δν νmax Teff
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Huber et al. 2011, ApJ, 743, 143
A lot
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From oscillations to stellar parameters
1) Scaling relations 2) Grid method 3) Detailed modelling
M, R, age
Δν, νmax [Fe/H] log(g)
Teff
ν1,…, νn [Fe/H] log(g) Teff, ...
M, R, age
Difficulty Precision
M, R
Δν νmax Teff
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Kepler-21 Howell et al. 2012
Δν = 60.86 ± 0.55 μHz νmax = 1153 ± 32 μHz
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Kepler-36 Carter et al. 2012
Δν = 67.9 ± 1.2 μHz νmax = 1250 ± 44 μHz
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KIC 11772920 From the ensemble in Chaplin et al. 2011
Δν = 158.6± 3.6 μHz νmax = 3800 ±100 μHz
Frequency (μHz)
PSD
(p
pm
2 μ
Hz-1
)
8/LC artifact
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Verifying Transiting Planets
• Can infer stellar density through shape of the transit light curve (Seager & Mallen-Ornélas 2003)
• Asterodensity profiling (e.g. Kipping 2014)
• Does asteroseismic density = transit density?
Asteroseismic density Inferred transit density
(Sliski & Kipping 2014)
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Population Studies: CoRoT Giants
Mass
Frac
tio
n
Miglio et al. 2013
Simulations
Scaling relations Scaling relations
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Population Studies:
Chaplin et al. 2011
Scaling relations Population synthesis modelling
Kepler Dwarfs
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But can we trust the scaling relations?
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Population Studies:
Chaplin et al. 2011
Scaling relations Population synthesis modelling
Kepler Dwarfs
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But can we trust the scaling relations?
Two ways to check:
1.Stellar models
2.Independent observations
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Density
Surface gravity
Mass
Radius
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Models
• Make a grid of stellar models and determine their oscillation frequencies.
• For each model we know M and R.
• For each model we can measure Δν
• Is ?
21
3
/
R
Mν
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White et al. 2011
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White et al. 2011
Mass 0.7 M
2.0 M
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• Observed frequencies are not high enough
• Departures from homology
Why not?
So Δνobs is not equal to
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Mass 0.7 M
2.0 M
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[Fe/H] -0.9 +0.5
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[Fe/H] -0.9 +0.5
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[Fe/H] -0.9 +0.5
Scatter in metallicity
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[Fe/H] -0.9 +0.5
Scatter in mass
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But can we trust the scaling relations?
Two ways to check:
1.Stellar models
2.Independent observations
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Independent Measurements
• Interferometric radii
• Dynamical masses
• Transit densities
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Interferometry Point source
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Interferometry Point source
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Interferometry Point source Resolved disc
Fringe visibility is a function of source size, baseline length, and wavelength
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Visibility
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0.2 mas
0.5 mas 1.5 mas
λ
B
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PAVO at the CHARA Array
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0.2 mas
0.5 mas 1.5 mas
λ
B
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PAVO (visible)
MIRC (infrared)
θLD = 0.753±0.009 mas R = 1.48±0.02 R
White et al. 2013
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Interferometry of Kepler and CoRoT stars
Huber et al. 2012
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Asteroseismology of Kepler and CoRoT stars
Huber et al. 2012
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Density
Surface gravity
Mass
Radius
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Huber et al. 2012
Giants dominated by parallax uncertainties
Measured Radius
From scaling relations
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16 Cyg
16 Cyg A
16 Cyg B
Metcalfe et al. 2012
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θLD = 0.539±0.007 mas R = 1.22±0.02 R
White et al. 2013
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θLD = 0.490±0.006 mas R = 1.12±0.02 R
White et al. 2013
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Huber et al. 2012
Measured Radius
From scaling relations
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White et al. 2013
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PAVO (visible)
MIRC (infrared)
θLD = 0.753±0.009 mas R = 1.48±0.02 R
White et al. 2013
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θ Cyg
Guzik et al. 2011
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Let’s have another look at the Δν scaling relation
using the brightest stars with
independent measurements of mass and radius
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α Cen A R=1.225±0.004 R
(interf. + parallax, Kervella et al. 2003, Söderhjelm 1999)
M=1.105±0.007 M (binary orbit, Pourbaix et al. 2002)
Δν = 105.7±0.3 μHz (Bedding et al. 2004)
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α Cen B R=0.864±0.005 R
(interf. + parallax, Kervella et al. 2003, Söderhjelm 1999)
M=0.934±0.006 M (binary orbit, Pourbaix et al. 2002)
Δν = 161.7±0.2 μHz (Kjeldsen et al. 2005)
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Procyon A R=2.059±0.015 R
(interf. + parallax, Kervella et al. 2004, van Leeuwen 2007)
M=1.461±0.025 M (binary orbit, Girard et al. 2000, Gatewood & Han 2006)
Δν = 55.9±0.3 μHz (Bedding et al. 2010)
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TrES-2 (Kepler-1) ρ=1.105±0.011 ρ
(transit, Southworth, 2011)
Δν = 141.0±1.4 μHz (Huber et al. 2013)
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HAT-P-7 (Kepler-2) ρ=0.2023±0.0024 ρ
(transit, Southworth, 2011)
Δν = 59.2±0.6 μHz (Huber et al. 2013)
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HD 17156
Δν = 83.44±0.15 μHz (Gilliland et al. 2011) 2011) al. et Nutzman (transit, ρ3710 0150
0130.
..
ρ
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16 Cyg A R=1.22±0.02 R
(interf. + parallax, White et al. 2013, van Leeuwen 2007)
M=1.06±0.03 M (H-R diagram, Casagrande et al. 2011)
Δν = 103.5±0.1 μHz (Metcalfe et al. 2012)
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16 Cyg B R=1.12±0.02 R
(interf. + parallax, White et al. 2013, van Leeuwen 2007)
M=1.04±0.04 M (H-R diagram, Casagrande et al. 2011)
Δν = 117.0±0.1 μHz (Metcalfe et al. 2012)
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θ Cyg R=1.49±0.02 R
(interf. + para., White et al. 2013, van Leeuwen 2007)
M=1.39±0.02 M (H-R diagram, Casagrande et al. 2011)
Δν = 84.0±0.4 μHz (Guzik et al. 2011)
Giants?
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Huber et al. 2012
Giants dominated by parallax uncertainties
Measured Radius
From scaling relations
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KIC 8410637
• Giant in an eclipsing binary (Hekker et al. 2010)
– Δν = 4.57 ± 0.03 μHz
• Mass and radius determined by Frandsen et al. 2013
– M = 1.557 ± 0.028 M
– R = 10.74 ± 0.11 R
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KIC 8410637
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What we need:
We need the brightest stars with the best measurements.
• Better parallaxes Gaia
• Asteroseismology of nearby, bright stars K2, SONG, TESS, PLATO
• Interferometry AO system at CHARA
• Dynamical masses