"19"^^ . "Using data from\u00A0 the satellite\u00A0 data MDI/SoHO, we studied\u00A0 the flows of matter\u00A0 in the solar photosphere using the method of\u00A0 horizontal motions of\u00A0 the supergranular structures and of\u00A0 direct measurements of Doppler velocities.\u00A0The first method, the acc"@en . "0"^^ . "2007-10-16+02:00"^^ . . . . . . . . "1"^^ . . "Sou\u010Dasn\u00E9 metody dru\u017Eicov\u00FDch pozorov\u00E1n\u00ED Slunce produkuj\u00ED data, kter\u00E1 n\u00E1m dovoluj\u00ED velmi dob\u0159e popsat pohyb hmoty na \u00FArovni slune\u010Dn\u00ED fotosf\u00E9ry po t\u00E9m\u011B\u0159 cel\u00E9m slune\u010Dn\u00EDm disku, v\u010Detn\u011B jeho \u010Dasov\u00E9ho v\u00FDvoje. Pod pohybem hmoty nech\u00E1peme dopplerovsk\u00E1 rychlostn\u00ED pole, ale proud\u00EDc\u00ED plazma, kter\u00FDm jsou fotosf\u00E9rick\u00E9 struktury un\u00E1\u0161eny. Nen\u00ED vylou\u010Deno, \u017Ee n\u011Bkter\u00E9 fotosf\u00E9rick\u00E9 struktury pohyb plazmatu naopak urychluj\u00ED. P\u0159i vykreslov\u00E1n\u00ED t\u011Bchto pohyb\u016F vznikaj\u00ED slo\u017Eit\u00E9 topologick\u00E9 struktury rychlostn\u00EDch pol\u00ED. Na\u0161\u00EDm c\u00EDlemje z\u00EDskat ze standardn\u00EDch dru\u017Eicov\u00FDch dat tyto topologick\u00E9 struktury rychlostn\u00EDch pol\u00ED, popsat jejich vlastnosti, nal\u00E9zt faktory, kter\u00E9 tyto struktury ovliv\u0148uj\u00ED a hledat z\u00E1konitosti, uplat\u0148uj\u00EDc\u00ED se p\u0159i interakci proud\u00EDc\u00EDho plazmatu s oblastmi poza\u010Fov\u00E9ho magnetick\u00E9ho pole, s magnetick\u00FDm a rychlostn\u00EDm polem aktivn\u00EDch oblast\u00ED a skvrn. Z\u00E1rove\u0148 n\u00E1s zaj\u00EDm\u00E1, zda existuje n\u011Bjak\u00E1 souvislost mezi charakteristick\u00FDmi rysy t\u011Bchto struktur a projevy slune\u010Dn\u00ED aktivity a do jak\u00E9 m\u00EDry by pr\u00E1v\u011B tyto pohyby plazmatu," . . "0"^^ . "Velocity Fields in the Solar Photosphere and their Interaction with Magnetic Fields"@en . . . . "GA205/04/2129" . . . "Rychlostn\u00ED pole ve slune\u010Dn\u00ED fotosf\u00E9\u0159e a jejich interakce s magnetick\u00FDmi poli" . . . . . . "Neuvedeno."@en . "http://www.isvav.cz/projectDetail.do?rowId=GA205/04/2129"^^ . . "The contemporary methods of the satellite observations of the Sun produce data which make possible to describe well the mass motion on the level of the solar photosphere over almost the whole solar disk, including its evolution in time. For the mass motion we do not consider the Doppler velocity field, but the flowing plasma, carrying away the photospheric structures. It is not excluded that some photospheric patterns the plasma motion even accelerate. Visualizing these motions we obtain complicatedtopological structures of such velocity fields. Our aim is to get the topological patterns of the velocity fields from standard satellite data, to describe their behaviors, to find various agents influencing them, and to search for regularities dominating during the interaction of the flowing plasma with the background magnetic fields, and with the magnetic and velocity fields of active regions and sunspots. At the same time, we are interested if there exists some relationship between the"@en . "Proud\u011Bn\u00ED hmoty ve slune\u010Dn\u00ED fotosf\u00E9\u0159e jsme studovali na z\u00E1klad\u011B dru\u017Eicov\u00FDch dat MDI/SoHO metodou horizont\u00E1ln\u00EDch pohyb\u016F supergranul\u00E1rn\u00EDch struktur a p\u0159\u00EDm\u00FDm m\u011B\u0159en\u00EDm dopplerovsk\u00FDch rychlost\u00ED. Prvn\u00ED metoda, jej\u00ED\u017E p\u0159esnost je 15 m/s, popisuje zon\u00E1ln\u00ED a meridio"@cs . "19"^^ .