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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... circular polarization signal of spectral lines seen in emission in prominences like Ha , but particularly in the He D3 line . As we shall see on the next section all these measurements can be disregarded from present knowledge , since ...
... circular polarization signal of spectral lines seen in emission in prominences like Ha , but particularly in the He D3 line . As we shall see on the next section all these measurements can be disregarded from present knowledge , since ...
294 ページ
... polarization will be decreased and the plane of polarization will turn . It is however dangerous to take those ... circular polarization . Because of its origin , such phenomena is often referred to as the alignment - to ...
... polarization will be decreased and the plane of polarization will turn . It is however dangerous to take those ... circular polarization . Because of its origin , such phenomena is often referred to as the alignment - to ...
313 ページ
... circular polarization if the magnetic field lies along the LOS . The Zeeman effect dominates the polarization of the scattered radiation if the splitting among the magnetic sublevels is of the same order of magnitude or larger than the ...
... circular polarization if the magnetic field lies along the LOS . The Zeeman effect dominates the polarization of the scattered radiation if the splitting among the magnetic sublevels is of the same order of magnitude or larger than the ...
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