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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... approximation simply by setting all photoionization and photoexcitation rates equal to zero . Figure 9 shows the results we obtain for CI - IV . Note that while we may not be using the best available atomic data , we are using the same ...
... approximation simply by setting all photoionization and photoexcitation rates equal to zero . Figure 9 shows the results we obtain for CI - IV . Note that while we may not be using the best available atomic data , we are using the same ...
193 ページ
... approximation . However , when dealing with fast phenomena ( often small ones ) this displacement current plays a role . Using Callebaut's exact solution of the MHD evolution equation , one may verify the approximation by using ...
... approximation . However , when dealing with fast phenomena ( often small ones ) this displacement current plays a role . Using Callebaut's exact solution of the MHD evolution equation , one may verify the approximation by using ...
500 ページ
... approximation for the low chromosphere but is just a first or initial approximation for the upper chromosphere where " re- alistic " 3 - dimensional models with magnetic fields and consistent heating need to still be developed . 2 ...
... approximation for the low chromosphere but is just a first or initial approximation for the upper chromosphere where " re- alistic " 3 - dimensional models with magnetic fields and consistent heating need to still be developed . 2 ...
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