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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... optical depths " procedure for solving the differential cloud model case ... thickness at line center 70 , max , while So , S1 and S2 are functions of 70 ... optical depth , where So is the source function at the middle of the ...
... optical depths " procedure for solving the differential cloud model case ... thickness at line center 70 , max , while So , S1 and S2 are functions of 70 ... optical depth , where So is the source function at the middle of the ...
228 ページ
... optical depth 70 , max and velocity v using a cloud model with variable source function ( see Eq . 6 ) depending only on line - center optical thickness versus the assumed optical thickness . Gaussian noise has also been taken into ...
... optical depth 70 , max and velocity v using a cloud model with variable source function ( see Eq . 6 ) depending only on line - center optical thickness versus the assumed optical thickness . Gaussian noise has also been taken into ...
229 ページ
... optical thickness with an added Gaussian noise ; without noise the results are perfectly reproduced . We see that the differences are now almost negligible for a large range of the assumed optical thickness and the parameters are better ...
... optical thickness with an added Gaussian noise ; without noise the results are perfectly reproduced . We see that the differences are now almost negligible for a large range of the assumed optical thickness and the parameters are better ...
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