From Accurate Atomic Data to Elaborate Stellar Modeling

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
Atomic Physic and Astronomy
3
Results Opacities Accelerations OP

• 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? ? 1s22s22p5nl valence
electron 1s22s22p6 h? ? 1s2s22p6nl inner
shell electron
Opacities OP vs OPAL
Radiative accelerations OP vs OPAL
?
Badnell et al. 2005 MNRAS 360 458
Delahaye Pinsonneault 2005 ApJ 625563
4
Solar composition
Delahaye Pinsonneault 2006 (ApJ in press )
5
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) lt AccFe (OPAL)

Turcotte et al. 1998 (ApJ 504559-572)
8
Radiative Acceleration Stellar interior
Surface
CZ Convection Zone
Black CZ ? ? Fe CZ
Fe CZ
M1.7M?
M1.5M?
centre
Radiative Acceleration ? Gravitational Settling
?
Fe CZ
M2.5M?
Richard et al. 2001 (ApJ 558377-391)
9
(No Transcript)