. . . "Numerical modelling of energetic processes in the solar atmosphere"@en . . "Neuvedeno."@en . "GA205/04/0358" . "Numerick\u00E9 modelov\u00E1n\u00ED energetick\u00FDch proces\u016F ve slune\u010Dn\u00ED atmosf\u00E9\u0159e" . . . "Using methods of numerical modelling, high energy processes in the magnetic plasma loops in the solar atmosphere will be studied. New improved numerical codes recently developed at the Astronomical Institute of Academy of Sciences in Ond\u0159ejov will be combined to self consistently model the problem: 1-D hydrodynamic code will determine the dynamics of solar plasma confined by the magnetic field, test particle code will be used to model the propagation and energy losses of charged high energy particle beams and corresponding heating of the ambient atmosphere and the non-LTE radiative transfer code will be used to calculate the non-LTE radiative losses and hydrogen ionisation in the optically thick photosphere and chromosphere. The radiative losses andelectron densities calculated for actual atmosphere will be then used as source terms for the 1-D hydrodynamic code in each timestep. Expected results of the simulations will be the tune dependent hydrogen line profiles, polarisation of hydrogen lines,"@en . "http://www.isvav.cz/projectDetail.do?rowId=GA205/04/0358"^^ . . . . . "0"^^ . . "P\u0159i \u0159e\u0161en\u00ED grantov\u00E9ho projektu jsme pou\u017E\u00EDvali rozs\u00E1hl\u00E9 numerick\u00E9 simulace k modelov\u00E1n\u00ED n\u011Bkolika aspekt\u016F energetick\u00FDch proces\u016F ve slune\u010Dn\u00ED atmosf\u00E9\u0159e, kter\u00E9 se t\u00FDkaly zejm\u00E9na fyziky slune\u010Dn\u00EDch erupc\u00ED. Synt\u00E9zou n\u011Bkolika po\u010D\u00EDta\u010Dov\u00FDch k\u00F3d\u016F modeluj\u00EDc\u00EDch indivi"@cs . "1"^^ . . "1"^^ . . . "2007-10-16+02:00"^^ . . . "During the workings on the grant project we have used extensive numerical simulations to model several aspects of energetic processes in the solar atmosphere mainly concerning the physics of solar flares. By synthesis of several computer codes, modelling"@en . "33"^^ . . "33"^^ . "S u\u017Eit\u00EDm metod numerick\u00E9ho modelov\u00E1n\u00ED, budou studov\u00E1ny vysokoenergetick\u00E9 procesy v magnetick\u00FDch plazmov\u00FDch smy\u010Dk\u00E1ch ve slune\u010Dn\u00ED atmosf\u00E9\u0159e. K \u0159e\u0161en\u00ED probl\u00E9mu budou pou\u017Eity nov\u00E9, vylep\u0161en\u00E9 numerick\u00E9 k\u00F3dy ned\u00E1vno vyvinut\u00E9 na Astronomick\u00E9m \u00FAstavu AV \u010CR, kter\u00E9 budou spojeny tak, aby self-konzistentn\u011B modelovaly formulovan\u00FD probl\u00E9m: 1-D hydrodynamick\u00FD k\u00F3d bude u\u017Eit k ur\u010Den\u00ED dynamiky slune\u010Dn\u00EDho plazmatu udr\u017Eovan\u00E9ho magnetick\u00FDm polem, test particle k\u00F3d bude modelovat \u0161\u00ED\u0159en\u00ED yysokoenergetick\u00FDch svazk\u016F nabit\u00FDch \u010D\u00E1stic, jeho energetick\u00FDch ztr\u00E1t a odpov\u00EDdaj\u00EDc\u00EDho oh\u0159evu okoln\u00ED slune\u010Dn\u00ED atmosf\u00E9ry a non-LTE k\u00F3d pro p\u0159enos z\u00E1\u0159en\u00ED bude u\u017Eit k v\u00FDpo\u010Dtu z\u00E1\u0159iv\u00FDch ztr\u00E1t a ionizace vod\u00EDku v opticky tlust\u00E9 fotosf\u00E9\u0159e a chromosf\u00E9\u0159e. Z\u00E1\u0159iv\u00E9 ztr\u00E1ty a hustoty elektron\u016F spo\u010Dten\u00E9 pro aktu\u00E1ln\u00ED atmosf\u00E9ru budou potom pou\u017Eity jako zdrojov\u00E9 \u010Dleny pro 1-D hydrodynamick\u00FD k\u00F3d v ka\u017Ed\u00E9m \u010Dasov\u00E9m kroku. O\u010Dek\u00E1van\u00FDmi v\u00FDsledky simulac\u00ED budou \u010Dasov\u011B z\u00E1visl\u00E9 profily vod\u00EDkov\u00FDch \u010Dar, polarizace vod\u00EDkov\u00FDch \u010Dar, rozlo\u017Een\u00ED tvrd\u00E9ho" . . .