space- and ground-based asteroseismology · introduction asteroseismology asteroseismology why? lc}...
TRANSCRIPT
Space- and ground-based
asteroseismology
S. Barcelo Forteza, D. Barrado, A. Moya, S. Martın-Ruiz,V. Casanova, A. Garcıa Hernandez.
21 February 2019
Introduction Asteroseismology
Asteroseismology
Why?
LCLV → PSD → ν, A, Γi → νmax → Teff,⋆ → Teff,P
Observed from
1 Ground: CARMENES, SONG
2 Space: CoRoT, Kepler, TESS
Observed and estimated data of CID 546 light curve.
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 1 / 12
Introduction Asteroseismology
Asteroseismology
Why?
LCLV → PSD → ν, A, Γi → νmax → Teff,⋆ → Teff,P
i
How to calculate:
1 Gaussian fit
2 Kallinger et al. (2010):
νmax =∑
Aiνi∑Ai
PSD of the red giant KIC 5701829.
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 2 / 12
Introduction Asteroseismology
Asteroseismology
Why?
LCLV → PSD → ν, A, Γi → νmax → Teff,⋆ → Teff,P
i
Scaling relations
Kjeldsen & Bedding (1995):
νmax ∝ MR−2T−0.5eff
(
Teff,P
Teff,⋆
)2
= R⋆
2a
PSD of the red giant KIC 5701829.
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 3 / 12
Introduction δ Scuti stars
δ Scuti stars
Characteristics:
κ-mechanism (Chevalier 1971; Xiong et al. 2016)
M ∈ [1.5, 2.5] M⊙
Teff ∈ [6000, 9000] K
Ω . ΩC
ν ∈ [60, 930] µHz
Scaling relation?
1 Dziembowski (1997):Teff ∝ νi
2 Kallinger et al. (2010):
νmax =∑
Aiνi∑Ai
Pulsators in the HR diagram (Barcelo Forteza et al., submitted).
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 4 / 12
Introduction δ Scuti stars
δ Scuti stars
Characteristics:
κ-mechanism (Chevalier 1971; Xiong et al. 2016)
M ∈ [1.5, 2.5] M⊙
Teff ∈ [6000, 9000] K
Ω . ΩC
ν ∈ [60, 930] µHz
Scaling relation?
1 Dziembowski (1997):Teff ∝ νi
2 Kallinger et al. (2010):
νmax =∑
Aiνi∑Ai
Excited modes of a δ Scuti model from Dziembowski (1997).
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 4 / 12
Introduction δ Scuti stars
δ Scuti stars
Characteristics:
κ-mechanism (Chevalier 1971; Xiong et al. 2016)
M ∈ [1.5, 2.5] M⊙
Teff ∈ [6000, 9000] K
Ω . ΩC
ν ∈ [60, 930] µHz
Scaling relation?
Teff ∝ νmax
Excited modes of a δ Scuti model from Dziembowski (1997).
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 4 / 12
Introduction Gravity-darkening effect
Gravity-darkening effect
Rotation
geff (i) ≈ g − R(i)Ω2 sin2i
Teff (i) ∝ gβ/4eff
(i) → β ≈ 1 (von Zeipel 1924)
δTeff (i) ≡(
Teff(i)− Teff
)
/Teff
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 5 / 12
Introduction Gravity-darkening effect
Gravity-darkening effect
Rotation
geff (i) ≈ g − R(i)Ω2 sin2i
Teff (i) ∝ gβ/4eff
(i) → β ≈ 1 (von Zeipel 1924)
δTeff (i) ≡(
Teff(i)− Teff
)
/Teff
Ω/ΩC = 0
|δTeff (i)| = 0 %
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 5 / 12
Introduction Gravity-darkening effect
Gravity-darkening effect
Rotation
geff (i) ≈ g − R(i)Ω2 sin2i
Teff (i) ∝ gβ/4eff
(i) → β ≈ 1 (von Zeipel 1924)
δTeff (i) ≡(
Teff(i)− Teff
)
/Teff
Ω/ΩC = 0
|δTeff (i)| = 0 %
Ω/ΩC = 0.7
|δTeff (i)| . 5.9 %
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 5 / 12
Introduction Gravity-darkening effect
Gravity-darkening effect
Rotation
geff (i) ≈ g − R(i)Ω2 sin2i
Teff (i) ∝ gβ/4eff
(i) → β ≈ 1 (von Zeipel 1924)
δTeff (i) ≡(
Teff(i)− Teff
)
/Teff
Ω/ΩC = 0
|δTeff (i)| = 0 %
Ω/ΩC = 0.7
|δTeff (i)| . 5.9 %
Ω/ΩC = 1
|δTeff (i)| . 21.5 %
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 5 / 12
Introduction Gravity-darkening effect
Gravity-darkening effect
i ≈ 90
Ω/ΩC = 0
δTeff (i) = 0 %
Ω/ΩC = 0.7
δTeff (i) ≈ −3.3 %
Ω/ΩC = 1
δTeff (i) ≈ −21.5 %
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 6 / 12
Introduction Gravity-darkening effect
Gravity-darkening effect
i ≈ 0
Ω/ΩC = 0
δTeff (i) = 0 %
Ω/ΩC = 0.7
δTeff (i) ≈ 5.9 %
Ω/ΩC = 1
δTeff (i) ≈ 14.5 %
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 6 / 12
Introduction Gravity-darkening effect
Gravity-darkening effect
i ≈ 55
Ω/ΩC = 0
δTeff (i) = 0 %
Ω/ΩC = 0.7
δTeff (i) ≈ 0 %
Ω/ΩC = 1
δTeff (i) ≈ 0 %
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 6 / 12
Introduction Teff − νmax diagram
Teff − νmax diagram
Barcelo Forteza et al. (2018)
Teff = Teff(1 + δTeff(i))
1 νmax → Teff
2 δTeff(i) → Ω
ΩK, i
Predicted temperatures of over 5000 δ Scuti star models with ∀ νmax,Ω
ΩK, i including the Kepler ETeff ≈ 250 K
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Data & Methods Data sources
Data sources
νmax,Teff
νmax → δSBF pipeline
Barcelo Forteza et al. (2015)
Teff → CATALOGUES
Brown et al. (2011)
Debosscher et al. (2009)
Measured νmax,Teff values of over a thousand δ Scuti stars.
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 8 / 12
Results Linear fit
Method 1: Linear fit
Teff ≈ a · νmax + b
a (K/µHz) 3.56 ± 0.23 σ (%) 6.52b (K) 6840 ± 50 Nin (%) 99R 0.954 Nout (%) 1
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Results Linear fit
Method 1: Linear fit
Teff ≈ a · νmax + b
a (K/µHz) 3.56 ± 0.23 σ (%) 1.08b (K) 6840 ± 50 Nin (%) 98R 0.954 Nout (%) 2
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 9 / 12
Results Known δ Scuti stars
Method 2: Known δ Scuti stars
Teff ,Ω
Ωk, i → Teff
Teff ≈ a · νmax + b
a (K/µHz) 2.5 ± 0.5
b (K) 7090 ± 120∣
∣
∣
Teff−Teff,M
Teff,M
∣
∣
∣. ETeff
Teff
R 0.882
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 10 / 12
Conclusions & Future Work
Conclusions
We suggest a new scaling relation Teff − νmax for δSct
- non dependent of Ω
Ωk, i
- find Teff,P and H.Z.
Future work
Improve Teff − νmax with more data
Improve Teff − νmax with known δ Scuti stars
6= between photometric and spectroscopic data
TESS, CHEOPS
CARMENES
SONG
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 11 / 12
Acknowledgements
Thanks for your attention!
Acknowledgements
J.A. Caballero, E. Solano, C. Rodrıguez-Lopez
S. Barcelo Forteza CARMENES + EXONET 21 February 2019 12 / 12
Acknowledgements
Barcelo Forteza, S., Michel, E., Roca Cortes, T., & Garcıa, R. A.2015, A&A, 579, A133
Barcelo Forteza, S., Roca Cortes, T., & Garcıa, R. A. 2018, A&A,614, A46
Brown, T. M., Latham, D. W., Everett, M. E., & Esquerdo, G. A.2011, AJ, 142, 112
Chevalier, C. 1971, A&A, 14, 24
Debosscher, J., Sarro, L. M., Lopez, M., et al. 2009, A&A, 506, 519
Dziembowski, W. 1997, in IAU Symposium, Vol. 181, Sounding Solarand Stellar Interiors, ed. J. Provost & F.-X. Schmider, 317
Kallinger, T., Mosser, B., Hekker, S., et al. 2010, A&A, 522, A1
Kjeldsen, H. & Bedding, T. R. 1995, A&A, 293, 87
von Zeipel, H. 1924, MNRAS, 84, 684
Xiong, D. R., Deng, L., Zhang, C., & Wang, K. 2016, MNRAS, 457,3163
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