asteroseismology with wfirst - nexscinexsci.caltech.edu/workshop/2017/saganworkshop17_huber.pdf ·...
TRANSCRIPT
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Asteroseismology with WFIRST
Daniel Huber
Institute for Astronomy University of Hawaii
Sagan Workshop August 2017
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Crash Course in Asteroseismology
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Crash Course in Asteroseismology
?
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unnamed author, sometime in 1995
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Radial Order n
surfacecenter
disp
lace
men
t
number of nodes from the surface to the center of the star
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Spherical Degree l
l = 0
total number of nodes on surface of the star
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Spherical Degree l
total number of nodes on surface of the star
l = 0
l = 2
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l = spherical degree (total number of surface nodes)
m = azimuthal order (number of nodes through the rotation axis)
|m| < ll = 2
|m| = 0
Spherical Harmonics Y lm
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l=?, |m|=?
↻
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l=1, |m|=1
↻
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↻
l=?, |m|=?
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↻
l=3, |m|=1
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δSct
roAp
CepSPB
SunDwarfs
Giants
Coherent (“Classical”)
Pulsators
Stochastic (“Solar-like”)
Oscillators
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Oscillations in cool stars are driven by turbulent surface
convection
Mode excitation: stochastic oscillations
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The Sun
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Δν = (2 ∫dr/cs)-1 ∝ (M/R3)1/2sound speed cs
Δν ~ 135 µHz for the Sun
(ω = n π c / L!)
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Ulrich (1986)
Δν = (2 ∫dr/cs)-1 ∝ (M/R3)1/2sound speed cs
δν
δν ∝ ∫dcs/dr (Age & interior
structure)
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νmax
νmax ∝ νac ∝ M R-2 Teff0.5 (gravity)
Δν = (2 ∫dr/cs)-1 ∝ (M/R3)1/2 (density)
ΔνThe Sun
R <~ 5% M <~ 10%
Teff
Δν, νmax
+
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The Space-Photometry Revolution of
Asteroseismology
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pre-2009
Kjeldsen et al. 1995, Frandsen et al. 2002
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CoRoT
De Ridder et al. 2009, Hekker et al. 2009
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Kepler
Hekker et al. 2011, Stello et al. 2013
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Red Clump (He-core burning)
RGB (non He-core
burning)
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The cores of Red Giants: Mixed Modes
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Multiple l=1 modes per order due to coupling with gravity modes trapped in the stellar interior (“mixed modes”)
The cores of Red Giants: Mixed Modesl=1l=1l=1
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non He-core
burning
He-core burning
Mean Density
Mix
ed m
ode
spac
ing
Bedding et al. 2011, Nature
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The Exoplanet - Asteroseismology
Synergy
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(RP/R★)2
M★ & R★
+
RP(<5%
uncertainty!)
Kepler-36Carter et al. 2012
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Huber et al. (2013a)
The Kepler Host Star Sample
All Host StarsHost stars with asteroseismic
detections
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red giant hosting 2 transiting planets
Synergy I: Exoplanet Architectures
10.2d, 6.5R♁
21.4d, 9.8R♁
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~50 individual frequencies
detected
l=1 l=1 l=1
Kepler-56 Asteroseismology
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~50 individual frequencies
detected
mixed l=1 modes are split into triplets by
rotation
l=1 l=1 l=1
Kepler-56 Asteroseismology
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Andrea MiglioUniversity of Birmingham, UK
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~50 individual frequencies
detected
mixed l=1 modes are split into triplets by
rotation
l=1 l=1 l=1
Kepler-56 Asteroseismology
i ~ 45°!
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~50 individual frequencies
detected
mixed l=1 modes are split into triplets by
rotation
l=1 l=1 l=1
Kepler-56 Asteroseismology
i ~ 45°!
↻
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Huber et al. 2013b
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Huber et al. 2013b
confirmed as planet by Otor et al.
2016!
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WFIRST Asteroseismology
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Kepler light curve
Time (Days)
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Kepler light curve
Time (Days)
Time (Days)
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Kepler light curve
Time (Days)
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Kepler light curve
WFIRST Duty Cycle
Time (Days)
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Kepler light curve
WFIRST Duty Cycle
Amplitude (H/Kp) ~ 0.5
Time (Days)
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Kepler light curve
WFIRST Duty Cycle
Amplitude (H/Kp) ~ 0.5
WFIRST photometry
noise
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ΔνKepler
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Δν
ΔνWFIRST
Kepler
Gould et al. (2014)
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Simulated Bulge GiantsH ~ 14.8 mag log(g) ~ 1.8 R ~ 25 R ⦿
H ~ 13.6 mag log(g) ~ 2.5 R ~ 11 R ⦿
H ~ 12.1 mag log(g) ~ 3.0 R ~ 7 R ⦿
Gould et al. (2014)
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Gould et al. (2014)
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~1e6 detections!
Gould et al. (2014)
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Galactic ArcheologyHow old are the galactic bulge &
halo?
How did the thin & thick disc form?
How important is radial migration?
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Galactic Archeology
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K2 Galactic Archeology ProgramStello et al. (2017)
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K2 Galactic Archeology Program
Challenges: - Crowded Field Photometry (4’’ pixels!)- 70 day campaigns limit distance reach
Stello et al. (2017)
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Asteroseismic Distance Reach
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Asteroseismic Distance Reach
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What can WFIRST Asteroseismology do
for Exoplanets?
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Transiting Exoplanet Hosts
simulated WFIRST population (H<15)
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Transiting Exoplanet Hosts
simulated WFIRST population
asteroseismic detections
simulated WFIRST population (H<15)
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Transiting Exoplanet Hosts
simulated WFIRST population
asteroseismic detections
limit for ~1 RJ transit
detectionKepler-56
simulated WFIRST population (H<15)
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Transiting Exoplanet Hosts
simulated WFIRST population
asteroseismic detections
Rotation
Flares(Davenport
2016)
Granulation (“Flicker”)
Bastien et al. (2013)
McQuillan et al. (2013, 2014)
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Asteroseismology & Microlensing
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θ*
Asteroseismology & Microlensing
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Banyai et al. (2013)
Source Star Variability
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Grunblatt et al. (2017)
Source Star Variability
Granulation/Oscillations can be modeled in the time
domain!
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Summary• Asteroseismology is a rapidly growing field in stellar astrophysics: highlights include interior properties of stars and characterization of transiting exoplanets
• What can WFIRST asteroseismology do for exoplanets?
• WFIRST will detect oscillations in ~1e6 giants: strong potential for galactic archeology of the bulge
- Transits: not much overlap; however, powerful for general astrophysics (e.g. rotation, granulation, flares, …)- Microlensing: strong constraints on red-giant source distance, size and variability!
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Better Stars, Better Planets: Exploiting the Stellar - Exoplanet Synergy
(exostar19)
Better stars better planets: exploiting the Stellar - Exoplanet synergy
(exostar19)
April - June 2019, KITP SBACoordinators: Victor Silva Aguirre, Rebekah Dawson, Jim Fuller,
Daniel Huber, Katja PoppenhaegerScience advisor: Josh Winn
April - June 2019, KITP Santa Barbara
Coordinators: Victor Silva Aguirre, Rebekah Dawson, Jim Fuller, Daniel Huber, Katja Poppenhaeger
Science Advisors: Josh Winn & Eric Agol
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WFIRST Photometric Precision
Gould et al. (2014)
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Asteroseismic Distances
Huber et al. (2017)
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Huber et al. (2017)