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From Accurate Atomic Data to Elaborate Stellar Modeling

From Accurate Atomic Data to Elaborate Stellar Modeling. Franck Delahaye LUTh (Observatoire de Paris, France) Collaborations : Atomic Physic – Opacity: Claude Zeippen (LUTh) Anil Pradhan (Ohio State) Claudio Mendoza (IVIC) The Opacity/Iron/RmaX Project team

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From Accurate Atomic Data to Elaborate Stellar Modeling

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  1. From Accurate Atomic Data to Elaborate Stellar Modeling Franck Delahaye LUTh (Observatoire de Paris, France) Collaborations: Atomic Physic – Opacity: Claude Zeippen (LUTh) Anil Pradhan (Ohio State) Claudio Mendoza (IVIC) The Opacity/Iron/RmaX Project team Astrophysics – Stellar Physic: Marc Pinsonneault (Ohio State) Georges Alecian (LUTh) Donald Terndrup (Ohio State) Sylvaine Turck-Chièze (CEA) High Accuracy Atomic Physics in Astronomy, August 7 – 9, 2006, ITAMP

  2. Drake et al. 2005 (Nature 436/Chandra) Atomic Physic and Astronomy

  3. Results: Opacities & Accelerations OP Stellar composition Delahaye & Pinsonneault 2006 (ApJ in press) • New opacities OP include inner shell processes. • OP Opacities available for high T -  domains  Stellar interior • Now 2 main sources of opacities: OP and OPAL • Good agreement in  R but important differences in accelerations • Applications → Solar composition, micro-diffusion 1s22s22p6 +h 1s22s22p5nlvalence electron 1s22s22p6 +h1s2s22p6nlinner shell electron Opacities: OP vs OPAL Radiative accelerations: OP vs OPAL ⊙ Badnell et al. 2005 MNRAS 360: 458 Delahaye & Pinsonneault 2005 ApJ 625:563

  4. Solar composition Delahaye & Pinsonneault 2006 (ApJ in press )

  5. Behr et al. 2000 (ApJ 531:L37) Radiative Accelerations & Abundances Anomalies Radiative Acceleration  Gravitational settling 

  6. Radiative Accelerations: OP vs OPAL Comparison OP-OPAL For a given stellar structure which Simulates HB or intermediate mass stars Trend: Z Diff . Delahaye & Pinsonneault 2005 ApJ 625, 563

  7. Detailled comparison between predictions and observations • Disagreement • Stellar wind, mixing • How about uncertainties in micro-diffusion? • Settling↓ Levitation↑. • Error in Acceleration can change amplitude and even sign • AccFe(OP) < AccFe (OPAL) Turcotte et al. 1998 (ApJ 504:559-572)

  8. Age Radiative Acceleration & Stellar interior Surface CZ: Convection Zone Black: CZ   Fe CZ Fe CZ M=1.7M⊙ M=1.5M⊙ centre Radiative Acceleration Gravitational Settling  Fe CZ M=2.5M⊙ Richard et al. 2001 (ApJ 558:377-391)

  9. Future NEEDS: Data and Comparisons Direct → Experiments, other calculations Indirect → Modelling . Context • More observations of high resolution to come (XMM - Chandra - XEUS - ASTROE2 - COROT - MOST – LBT). Atomic Physics • Data for low ionization states of Fe, Co and Ni. • Lasers and opacities: Experiment at ILP (CEA) (Proposal accepted) Astrophysics • Influence of atomic data on stellar modelling. • Development of the new standard of stellar code (including micro-diffusion) Data Bases • Development of codes et services for stellar modelling. • Toward VO standard of the OP/IP databases

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