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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54 ページ
... simulations were performed in 1D and magnetic fields were neglected . To enable a direct comparison with ... simulations of the response of the chromosphere to acous- tic waves show that the Ca II profiles can be explained by ...
... simulations were performed in 1D and magnetic fields were neglected . To enable a direct comparison with ... simulations of the response of the chromosphere to acous- tic waves show that the Ca II profiles can be explained by ...
55 ページ
... simulations . The failure of the simulations to reproduce diagnostics formed in the mid- dle to upper chromosphere gives us information on the energy balance of these regions . The main candidates for an explanation are the absence of ...
... simulations . The failure of the simulations to reproduce diagnostics formed in the mid- dle to upper chromosphere gives us information on the energy balance of these regions . The main candidates for an explanation are the absence of ...
69 ページ
... Simulations 20 20 10 . 000 Bod Figure 3 . 59 50 100 150 200 250 Deceleration [ m s ' ] 300 Adapted from Hansteen et ... simulations , reveals that the simulations reproduce the observed correlation between these parameters , as ...
... Simulations 20 20 10 . 000 Bod Figure 3 . 59 50 100 150 200 250 Deceleration [ m s ' ] 300 Adapted from Hansteen et ... simulations , reveals that the simulations reproduce the observed correlation between these parameters , as ...
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