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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... magnetic field is strong . Reverse granulation is evident in the 170 nm band as is enhanced emission where the magnetic field is strong . Bright emission in the bands formed higher in the chromosphere is a result of both strong magnetic ...
... magnetic field is strong . Reverse granulation is evident in the 170 nm band as is enhanced emission where the magnetic field is strong . Bright emission in the bands formed higher in the chromosphere is a result of both strong magnetic ...
158 ページ
... magnetic field geometry , not on the strength . Figure 2 shows the emergent Q / I and U / I signals at the line core of the Ca II infrared triplet lines for different magnetic field configurations and strengths in the FAL - C model ...
... magnetic field geometry , not on the strength . Figure 2 shows the emergent Q / I and U / I signals at the line core of the Ca II infrared triplet lines for different magnetic field configurations and strengths in the FAL - C model ...
245 ページ
... Magnetic Fields B. Ioshpa , E. Mogilevskii and V. Obridko IZMIRAN , Troitsk , Moscow Region , Russia Abstract . We discuss some results of the study of spatial characteristics of solar magnetic fields . The analysis is based on the magnetic ...
... Magnetic Fields B. Ioshpa , E. Mogilevskii and V. Obridko IZMIRAN , Troitsk , Moscow Region , Russia Abstract . We discuss some results of the study of spatial characteristics of solar magnetic fields . The analysis is based on the magnetic ...
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