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convergence: ǫ l = 10 −8 Brussels.tex – The PHOENIX Model Atmosphere Package – Peter H. Hauschildt – 21/6/2011 – 16:49 – p.12
Model Construction “Auxiliary” equations: equation of state → (T,P gas ,ρ) relation high temperatures: (hot stars, Supernovae, novae) → need to include many ions low temperatures: (Brown dwarfs, Jupiter-like planets, cool novae) → need to include 100’s of molecules & dust species ACES EOS (Travis Barman), valid above 100 K Brussels.tex – The PHOENIX Model Atmosphere Package – Peter H. Hauschildt – 21/6/2011 – 16:49 – p.13
Page 1 and 2: The PHOENIX Model Atmosphere Packag
Page 3 and 4: Applications PHOENIX v16 is being u
Page 5 and 6: Model Construction Constraint equat
Page 7 and 8: Model Construction Radiative transf
Page 9 and 10: Data size small grid: n x = n y = n
Page 11: Computation of Λ ∗ tri-diagonal
Page 15 and 16: Liquids & Solids Selected liquid/du
Page 17 and 18: Fe NLTE model atoms Brussels.tex -
Page 19 and 20: Computational Problem 1D (serial) C
Page 21 and 22: Results: solar type stars models wo
Page 23 and 24: DRIFT dust mode Helling & Woitke st
Page 25 and 26: DRIFT-PHOENIX models location of co
Page 27 and 28: Application: good fits Witte et al
Page 29 and 30: Application: good fits Witte et al
Page 31 and 32: Irradiation EGP spectra for differe
Page 33 and 34: Results: 3DRT w/ irradiation Brusse
Page 35 and 36: spherical 3D coordinates Brussels.t
Page 37 and 38: PHOENIX 1D vs 3D: 5700K Brussels.te
Page 39 and 40: 3D visualization: hydro model, line
Page 41: Conclusions: The Future better/more

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