The Physics of Chromospheric Plasmas: Proceedings of the Coimbra Solar Physics Meeting Held at the University of Coimbra, Coimbra, Portugal, 9-13 October, 2006Petr Heinzel, Ivan Dorotovič, Robert J. Rutten Astronomical Society of the Pacific, 2007 - 653 ページ |
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... radiative transfer is treated grey ( i.e. frequency - independent ) and under the assumption of local thermody- namic equilibrium ( LTE ) . These are severe assumptions for the upper photo- sphere and the chromosphere above but are ...
... radiative transfer is treated grey ( i.e. frequency - independent ) and under the assumption of local thermody- namic equilibrium ( LTE ) . These are severe assumptions for the upper photo- sphere and the chromosphere above but are ...
103 ページ
... radiation field for hydrogen can be approx- imated by fixed radiative rates in 1D simulations , thus reducing the complex time - dependent radiative transfer to a relatively simple problem of advection of populations with local sources ...
... radiation field for hydrogen can be approx- imated by fixed radiative rates in 1D simulations , thus reducing the complex time - dependent radiative transfer to a relatively simple problem of advection of populations with local sources ...
307 ページ
... radiation emerging from a stochastic multi - component atmosphere such as λ = 0.99 , t1 = 0.5 , t2 = 307 The Physics of Chromospheric Plasmas Radiative Transfer in Prominence Fine Structure as Multi-Component Atmosphere.
... radiation emerging from a stochastic multi - component atmosphere such as λ = 0.99 , t1 = 0.5 , t2 = 307 The Physics of Chromospheric Plasmas Radiative Transfer in Prominence Fine Structure as Multi-Component Atmosphere.
目次
Eightieth Anniversary of Solar Physics at Coimbra | 3 |
Spectroheliographic Observations in Madrid 19121917 | 17 |
Modeling the Solar Chromosphere | 49 |
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2007 Petr Heinzel active region arcsec ASP Conf ASP Conference Series Avrett bipoles bright calculated Carlsson chromosphere cloud model Coimbra computed continuum coronal Czech Republic density Doppler Dorotovič and Robert dynamic electron beam emission energy evolution fibrils field lines Figure filament filter filtergrams flux Fontenla Hanle effect Hansteen heating height instrument intensity inversion ionization Ivan Dorotovič limb line profiles loops magnetic field Meudon mirror motion mottles non-LTE non-thermal observations Observatory obtained optical depth optical thickness panel parameters phase photosphere pixels plage plasma polarization Pontieu prominence quiet Sun radiation radiative transfer RHESSI Rutten Schmieder shows simulations slit Solanki solar activity solar atmosphere solar disk solar flares Solar Phys Solar Prominences source function spatial resolution spectral lines spectrograph spectroheliograms spectrum Stokes structure SUMER sunspot telescope temperature transition region Trujillo Bueno variations velocity vertical wavelength waves Zeeman effect