stellar seismic indices data base (ssi) filer. peralta / r. samadi - stellar seismic indices data...
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 1
Stellar Seismic Indices data base (SSI)
Raphaël PERALTARéza Samadi & Eric Michel
& Kevin Belkacem
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 2
Outline
I. Seismic Indices
II.Stellar Seismic Indices data base, what we plan to do ?
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 3
Some definitions
• Seismic indices give global informations about stars oscillations
• Stellar seismic indices : νmax ,Δ ν ,ΔΠ , ...
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 4
Some definitions
νmax
Frequency of the maximum height in the power spectrum
Cut-off frequencyνc
νmax
νc
Mean large separationΔνΔν = ⟨νl , n+1
−νl , n⟩
• Stellar seismic indices : νmax ,Δ ν ,ΔΠ , ...
ΔΠ = ⟨ pl ,n+1−pl ,n⟩
Mean Period spacingΔΠ
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Canonical scaling relations
Seismic scaling law : Relation between global seismic parameters and fundamental stellar parameters
Mass, Radius, log g, ...νmax ,Δ ν ,ΔΠ , ...
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 6
Canonical scaling relations
● Frequency of the maximum height (Brown 1991)
νmax νc cs
2H p
g
√Teff
M
R2√T eff
● Large separation (Ulrich 1986)
Δ ν ⟨ρ⟩1/2 ( M
R3 )
1/2
● Period spacing
ΔΠ ⟨ρ⟩core
−1/2
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 7
Canonical scaling relations
Δν, νmax + Teff M, R
M
M⊙
≃(νmax
νmax ,⊙ )3
( Δ νΔ ν⊙
)−4
( Teff
T eff ,⊙)
3/2
R
R⊙
≃(νmax
νmax ,⊙)( Δ νΔ ν⊙
)−2
( T eff
T eff ,⊙)
1/2
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 8
● For stellar community :
– e.g. constraint on stellar evolution
● For exoplanets community :
– e.g. better estimates of radii and masses
● For galactic community :
– e.g. masses and radii for a large sample of stars (e.g. Miglio et al. 2009)
Benefits
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 9
Outline
I. Seismic Indices
II.Stellar Seismic Indices data base, what we plan to do ?
![Page 10: Stellar Seismic Indices data base (SSI) fileR. Peralta / R. Samadi - Stellar Seismic Indices data base 11 Are seismic masses and radii accurate ? Typical precision : 15 methods of](https://reader033.vdocuments.site/reader033/viewer/2022041415/5e1ae7460f371472a37617ba/html5/thumbnails/10.jpg)
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Are seismic masses and radii
accurate ?
Scaling relations give us precise determination of M, R
but...
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 11
Are seismic masses and radii
accurate ?
✔ Typical precision : 15 methods of analysis applied by 6 teams on simulated power spectrum (Verner et al. 2011)
● R and M are rather insensitive to uncertainties on ΔTeff
● The precision on νmax the limiting factor
νmax ∼ 5 %
Δν ∼ 1 %
ΔT eff ∼ 100K
Δ M
M∼ 20 %
Δ R
R∼ 8 %}⇒
~ 5%~ 1%
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 12
✔ There are some uncertainties related to the definitions of the seismic parameters
Are seismic masses and radii accurate ?
✔ Can scaling relations be considered as exact relations? (e.g. Belkacem SF2A 2012)
Bedding 2011
Miglio (2012)
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 13
What do we propose ?
● Stellar Seismic Indices (SSI) data base
– νmax, Δν, ∆П...
● « The Seismic plus » portal
– M, R, ...
http://spaceinn.eu/
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 14
What do we need to do ?
● We propose to test and choose one standard method for each seismic parameter
● The « standard » method : a trade off between :
– Automatic
– Robust and fast
– Well documented about algorithm precision and accuracy
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 15
What do we need to do ?
● Example : Autocorrelation method (Roxburgh & Vorontsov 2006 ; Mosser & Appourchaux 2009)HD179079 (LRc09/ID:8111) studied by exoplanet team
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 16
What do we need to do ?
● Example : Autocorrelation method (Roxburgh & Vorontsov 2006 ; Mosser & Appourchaux 2009)HD179079 (LRc09/ID:8111) studied by exoplanet team
● Fourier transform of the filtered power spectrum autocorrelation of the light curve
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What do we need to do ?
FT
● Example : Autocorrelation method (Roxburgh & Vorontsov 2006 ; Mosser & Appourchaux 2009)HD179079 (LRc09/ID:8111) studied by exoplanet team
● Fourier transform of the filtered power spectrum autocorrelation of the light curve
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 18
What do we need to do ?
FT
τ=2
Δ ννmax
● Example : Autocorrelation method (Roxburgh & Vorontsov 2006 ; Mosser & Appourchaux 2009)HD179079 (LRc09/ID:8111) studied by exoplanet team
● Fourier transform of the filtered power spectrum autocorrelation of the light curve
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 19
What do we need to do ?
● Example : Autocorrelation method (Roxburgh & Vorontsov 2006 ; Mosser & Appourchaux 2009)HD179079 (LRc09/ID:8111) studied by exoplanet team
● Results :
Seismic parameters
Δν = 64.95 ± 0.01 µHz
νmax = 1226.6 ± 32.4 µHz
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 20
What do we need to do ?
● Example : Autocorrelation method (Roxburgh & Vorontsov 2006 ; Mosser & Appourchaux 2009)HD179079 (LRc09/ID:8111) studied by exoplanet team
● Results :
Seismic parameters
Δν = 64.95 ± 0.01 µHz
νmax = 1226.6 ± 32.4 µHz
Teff = 5684 ± 100 K (Valenti et al. 2009)
Hence :
M☼ = 1.13 ± 0.05 M⊙
R☼ = 1.71 ± 0.09 R⊙
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What do we need to do ?
● Example : Autocorrelation method (Roxburgh & Vorontsov 2006 ; Mosser & Appourchaux 2009)HD179079 (LRc09/ID:8111) studied by exoplanet team
● Results :
Our values Valenti et al. 2009 M☼ = 1.13 ± 0.05 M⊙ M☼ = 1.15 ± 0.03 M⊙
R☼ = 1.71 ± 0.09 R⊙ R☼ = 1.60 ± 0.09 R⊙
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 22
What do we need to do ?
● Refine scaling relations :
– Theoretical work to understand (and reduce) the dispersion of the scaling relations (e.g. White et al. 2011 ; Belkacem 2012 ; ...)
e.g. Study of metallicity influences
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 23
What do we need to do ?
● Refine scaling relations :
– Theoretical work to understand (and reduce) the dispersion of the scaling relations (e.g. White et al. 2011 ; Belkacem 2012 ; ...)
e.g. Study of metallicity influences
● Test and Calibrate the scaling relations :
– Comparing seismic masses and radii with independent measurements (interferometry and astrometry)
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R. Peralta / R. Samadi - Stellar Seismic Indices data base 24
• CoRoT :
– Red Giants + Sub-Giants ~ 20,000
– Main Sequence ~ 10
• Kepler :
– Red Giants + Sub-Giants ~ 20,000
– Main Sequence ~ 500
• OGLE (optical gravitational lensing experiment) :
– Red Giants ~ 20,000
Set of data
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• 2 missions projects which might provide seismics indices :
– PLATO : its objective is to characterize exoplanets and their host stars in the solar neighbourhood
– SINDICS (Seismic INDICes Survey) : propose the 1st seismic all sky survey of our galactic environnement (idea, submited to CNES prospective).
Future set of data
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Thank you