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Inversion of rotation profile for solar-like stars

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jerry
24 diapositives · 460 Views · Aug 10, 2012

Inversion of rotation profile for solar-like stars. Jérémie Lochard. IAS 19/11/04. Rotational splitting: rotation lifts the degeneracy. Rotational splitting:. Rotational splitting:. what we observe. Rotational splitting:. what we observe. what we search. Rotational splitting:.

#anastrophe #chiasmus #inverted #chord #eversion #everting #inverting #reversal
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Inversion of rotation profile for solar-like stars
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  1. Inversion of rotation profile for solar-like stars Jérémie Lochard IAS 19/11/04

  2. Rotational splitting: rotation lifts the degeneracy

  3. Rotational splitting:

  4. Rotational splitting: what we observe

  5. Rotational splitting: what we observe what we search

  6. Rotational splitting: what we observe what we compute from models what we search

  7. Helioseismology Structure and rotation inversion gave strong constraints on solar models

  8. Helioseismology Structure and rotation inversion gave strong constraints on solar models Asteroseismology Restricted mode set: l=0,1,2(,3) (up to a few 1000 for the Sun)

  9. Helioseismology Structure and rotation inversion gave strong constraints on solar models Asteroseismology Restricted mode set: l=0,1,2(,3) (up to a few 1000 for the Sun) Our aim: is rotational inversion possible for some specific solar-like stars ? give selection constraints

  10. Helioseismology Structure and rotation inversion gave strong constraints on solar models Asteroseismology Restricted mode set: l=0,1,2(,3) (up to a few 1000 for the Sun) Our aim: is rotational inversion possible for some specific solar-like stars ? give selection constraints Other stars may show modes with different nature from those observed on the Sun

  11. With evolution g-mode cavity appears at the edge of the convective core

  12. With evolution g-mode cavity appears at the edge of the convective core look for evolved stars (but still on the main sequence)

  13. Eigen-functions and rotational kernels P modes Mixed modes

  14. Mode set selection: Amplitude computation: from the excitation and damping rates Selection threshold: from the COROT specifications mixed modes

  15. Mode set selection: Amplitude computation: from the excitation and damping rates Selection threshold: from the COROT specifications Mode amplitudes increase with mass look for massive stars with outer convective zone mixed modes

  16. Building a trial model to compute the rotational kernels HR diagram constraints: Effectivetemperature and luminosity

  17. Building a trial model to compute the rotational kernels HR diagram constraints: Effective temperature and luminosity Seismic constraints: largeseparation:global constraint (mean density)

  18. Building a trial model to compute the rotational kernels HR diagram constraints: Effective temperature and luminosity Seismic constraints: large separation:global constraint: mean density smallseparation: constraint on the deep interior (evolution stage …)

  19. Inversion inversion Kernels from the initial model forward

  20. Inversion Kernels from the initial model Kernels from the trial model

  21. Inversion Kernels from the initial model Kernels from the trial model Kernels from the trial model and random errors added

  22. Forward check computing the splittings from the recovered rotation profile

  23. Constraints on the rotational inversion for solar-like stars: Mass (modes amplitude) Evolution (mixed modes) Surface velocity (relative precision)

  24. Constraints on the rotational inversion for solar-like stars: Mass (modes amplitude) Evolution (mixed modes) Surface velocity (relative precision) Needs: stellar parameters (Teff, luminosity, surface chemical composition…) long observation periods and low noise level (Corot, Eddington…)