Non-LTE ゼミ論文紹介「 The formation of the Hα line in the solar chromosphere 」 ① 20120307 T. Anan.

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Presentation transcript:

non-LTE ゼミ論文紹介「 The formation of the Hα line in the solar chromosphere 」 ① T. Anan

abstruct Radiation-MHD simulation + 3D non-LTE radiative transfer computation => Hα – Statistical equilibrium – Complete frequency redistribution – Non-equilibrium ionization of hydrogen We find – 3D radiative transfer is essential in modeling Hα – Hα opacity is mainly sensitive mass density – Hα core intensity is correlated with the average formation height – The line-core width is a measure of the gas temperature – Fibril-like structure Formation height Simulated results are very similar to observed one without the need for additional microturbilance

RADYN code Hydrodynamics Carlsson & Stein 1992, 1995, 1997, & 2002 Eq. of conservation of mass, momentum, and energy Non-LTE radiative transfer problem including non-equilibrium rate equations – Ionization balance – Equation of state – Partial redistribution of photons in the Ryman lines – Elements & levels H I (5 levels + continuum) Ca II (5 levels + continuum) He I (5 levels + continuum) He II (3 levels + continuum) He III (1 levels + continuum) Lower boundary is just below the photosphere (τ 500nm = 16) – Velocity field derived from MDI (Doppler shift, nm, Ni I, quiet region) Upper boundary is corona at km above the lower boundary Run for more than 1 hour of solar time, and saved output at 10 s intervals => 374 sapshots