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 depth , source function and cloud velocity . 3. Results 3.1 . Lambdameter method The Lambdameter method is used for the derivation of intensity and velocity images for different profile widths . Figure 2 shows the intensity and ...
... optical depth , source function and cloud velocity . 3. Results 3.1 . Lambdameter method The Lambdameter method is used for the derivation of intensity and velocity images for different profile widths . Figure 2 shows the intensity and ...
220 ページ
... optical depths " procedure for solving the differential cloud model case which is described in Sect . 3.5 ( from Mein & Mein ( 1988 ) ) . with the optical depth at the center of the line to taking values between 0 and the total optical ...
... optical depths " procedure for solving the differential cloud model case which is described in Sect . 3.5 ( from Mein & Mein ( 1988 ) ) . with the optical depth at the center of the line to taking values between 0 and the total optical ...
309 ページ
... optical thickness of M elements ( beginning from the first ) . Observing that TNTN - 1 + TN , then we will have the ... depth and a decrease in the number of structures in the line of sight . But in such kind of atmospheres when the internal ...
... optical thickness of M elements ( beginning from the first ) . Observing that TNTN - 1 + TN , then we will have the ... depth and a decrease in the number of structures in the line of sight . But in such kind of atmospheres when the internal ...
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