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Regularities in the magnetic field distribution on the Sun in time
Bumba, Václav; Klvaňa, Miroslav
2009 - Czech
Solar background (weak) magnetic fields are very regularly distributed on the solar surface. These regularities change with the range of heliographic latitudes ant they are observable during more than four solar cycles. Sluneční pozaďová (slabá) magnetická pole jsou na povrchu Slunce rozdělena velmi pravidelně. Tyto pravidelnosti se mění s rozsahem heliografických šířek a jsou pozorovatelné v celém rozsahu více než čtyř slunečních cyklů.
Keywords:
solar magnetic fields; activity
Available at various institutes of the ASCR
Regularities in the magnetic field distribution on the Sun in time
Solar background (weak) magnetic fields are very regularly distributed on the solar surface. These regularities change with the range of heliographic latitudes ant they are observable during more than ...
The study of magnetic clouds: expansion and discontinuities
Lynnyk, A.; Vandas, Marek
2009 - English
Magnetic clouds observed during the 1995-2003 years are fitted using force-free cylindrical flux rope models. The cloud parameters yielded by a static model are compared with those obtained from a modified model that includes magnetic cloud expansion.
Keywords:
magnetic field; magnetic cloud; solar wind
Available at various institutes of the ASCR
The study of magnetic clouds: expansion and discontinuities
Magnetic clouds observed during the 1995-2003 years are fitted using force-free cylindrical flux rope models. The cloud parameters yielded by a static model are compared with those obtained from a ...
Displacements of Doppler velocity fields in sunspots
Klvaňa, Miroslav; Bumba, Václav
2009 - Czech
The mean value of Doppler velocity field in magnetized regions shows a sytematic redshift compared to the neighbouring non-magnetic regions in the range 37 – 191 m/s. Changes in the morphology of the Evershed effect are analyzed. Střední hodnota dopplerovského rychlostního pole v oblastech vyplněných magnetickým polem vykazuje systematický rudý posuv vůči sousedním oblastem bez magnetického pole v rozmezí 37 – 191 m/s. Analyzujeme změny v morfologii Evershedova efektu.
Keywords:
solar velocity fields; sunspots
Available at various institutes of the ASCR
Displacements of Doppler velocity fields in sunspots
The mean value of Doppler velocity field in magnetized regions shows a sytematic redshift compared to the neighbouring non-magnetic regions in the range 37 – 191 m/s. Changes in the morphology of the ...
Helioseismology – from oscillations toward the internal structure
Švanda, Michal
2009 - Czech
Solar oscillations make it possible to construct a detailed model od the Sun and to map details of the solar interior. A brief outline of methods of the global and local helioseismology. Sluneční oscilace umožňují konstrukci podrobného modelu Slunce a mapování detailů slunečního nitra. Stručný nástin metod globální a lokální helioseismologie.
Keywords:
solar oscillations; helioseismology
Available at various institutes of the ASCR
Helioseismology – from oscillations toward the internal structure
Solar oscillations make it possible to construct a detailed model od the Sun and to map details of the solar interior. A brief outline of methods of the global and local helioseismology.
Shell-Like Structures in the ISM: Observation Versus Simulations
Sidorin, Vojtěch; Palouš, Jan
2009 - English
The interstellar medium in galaxies is a turbulent environment with a plethora of holes, bubbles and shells. All these shell-like structures are thought to be closely related to the formation, evolution and death of stars. In most cases, they are likely created by the winds of OB stars and supernovae. The material collected along the borders of shells may fragment, become unstable under its own gravity, and create a new generation of stars. This is a variant of triggered star formation referred to as the collect-and-collapse scenario. The aim of our research is to compare numerical simulations of shell-like structures to observations and to search for and investigate regions of triggered star formation in the Milky Way.
Keywords:
shells; ism; triggered star formation
Available at various institutes of the ASCR
Shell-Like Structures in the ISM: Observation Versus Simulations
The interstellar medium in galaxies is a turbulent environment with a plethora of holes, bubbles and shells. All these shell-like structures are thought to be closely related to the formation, ...
Complementary cooperation, the Cardano's world, and the incompletness
Rajchl, Jaroslav
2008 - Czech
The Cardano’s world (CW) is characterized by the well known phrase about the triadicity of all the good and bad! It contains a cubic nonlinearity (NL) as its mainbase, together with the linear, bilinear and quadratic components (i.e. the positive and negative solutions). All these components are fundamental for its dynamical cooperative and relative stability as a system. But, the relation between its quadratic and cubic (NL) is, as has been shown previously, of paradoxical nature (Rajchl 2006), which is the source of dynamical evolution of (CW). It is shown that such a system is incomplete in the sense, that it evolves behind its relative stability state (dimension 3) to the deterministic chaos. Cardanuv svet muže být charakterizován oním dobre známým rcením: „do tretice všeho dobrého i zlého“. Je nelineární (NL) s dimensí 3 a tím i relativne stabilní. Obsahuje v sobe navíc ješte linearitu i kvadratickou nelinearitu (tj. obsahuje ono dobré a zlé jako kladné a záporné), ale i soucinnost komplementárního jako bi-linearitu. Ve vztahu kvadratického a kubického (jak jsme ukázali již loni) je i paradoxní, což zakládá navíc i jeho dynamicnost. Je však, jak se ukazuje (
Keywords:
complementary cooperation; Cardano's world
Available at various institutes of the ASCR
Complementary cooperation, the Cardano's world, and the incompletness
The Cardano’s world (CW) is characterized by the well known phrase about the triadicity of all the good and bad! It contains a cubic nonlinearity (NL) as its mainbase, together with the linear, ...
Comparison of relativistic iron line models
Svoboda, Jiří; Dovčiak, Michal; Goosmann, René; Karas, Vladimír
2008 - English
Analýza profilu široké čáry železa v rentgenových spektrech aktivních galaxií a mikrokvasarů nám umožňuje určit spin černé díry. Porovnávame výsledky pro dva rentgenové zdroje, MCG-6-30-15 a GX 339-4, se širokou čárou železa pomocí současných modelů relativistické čáry v programu XSPEC - LAOR a KYRLINE. The analysis of the broad iron line profile in the X-ray spectra of active galactic nuclei and black hole X-ray binaries allows us to constrain the spin parameter of the black hole. We compare the constraints on the spin value for two X-ray sources, MCG-6-30-15 and GX 339-4, with a broad iron line using present relativistic line models in XSPEC - LAOR and KYRLINE.
Keywords:
accretion; accretion disks; black holes
Available at various institutes of the ASCR
Comparison of relativistic iron line models
Analýza profilu široké čáry železa v rentgenových spektrech aktivních galaxií a mikrokvasarů nám umožňuje určit spin černé díry. Porovnávame výsledky pro dva rentgenové zdroje, MCG-6-30-15 a GX 339-4, ...
Statistical study of the fitting of the magnetic clouds
Lynnyk, A.; Vandas, Marek
2008 - English
Práce je statistickou studií o srovnání modelu expandujícího magnetického oblaku s pozorováními. The paper is a statictical study on comparisons between a model of an expanding magnetic cloud and observations.
Keywords:
magnetic clouds; solar wind; interplanetary magnetic field
Available at various institutes of the ASCR
Statistical study of the fitting of the magnetic clouds
Práce je statistickou studií o srovnání modelu expandujícího magnetického oblaku s pozorováními.
Modelling the polarization dichotomy of active galactic nuclei
Goosmann, René
2007 - English
Prezentuji modelování polarizace záření aktivních galaktických jader v optické a UV oblasti. Při modelování je použit kód Stokes pro Monte Carlo simulace přenosu záření, který selfkonzistentně modeluje polarizaci geometricky komplexního uspořádání aktivního jádra. I present polarization modelling of Active Galactic Nuclei in the optical/UV range. The modelling is conducted using the Monte-Carlo radiative transfer code Stokes, which self-consistently models the polarization signature of a complex model arrangement for an active nucleus.
Keywords:
active galaxies; radiative transfer; polarization
Available at various institutes of the ASCR
Modelling the polarization dichotomy of active galactic nuclei
Prezentuji modelování polarizace záření aktivních galaktických jader v optické a UV oblasti. Při modelování je použit kód Stokes pro Monte Carlo simulace přenosu záření, který selfkonzistentně ...
Magnetic clouds and their expansion
Lynnyk, A.; Vandas, Marek
2007 - English
Analyzovali jsme magnetická oblaka pro roky 1995-1998 s použitím modelu bezsilové magnetické válcové silotrubice, jež může zahrnovat expanzi. Zřetelná expanze oblaků byla zjištěna v 80%.Zahrnutí expanze zlepšuje srovnání modelu s měřeními u 75% z těchto případů. Magnetic clouds for the years 1995-1998 are analyzed using a model of a force-free cylindrical flux rope which may include cloud expansion. Clearly pronounced expansion was found in 80% cases. It was found that including the expansion makes comparison between model and experimental data better in 75% of these cases.
Keywords:
magnetic clouds; solar wind; magnetic field
Available at various institutes of the ASCR
Magnetic clouds and their expansion
Analyzovali jsme magnetická oblaka pro roky 1995-1998 s použitím modelu bezsilové magnetické válcové silotrubice, jež může zahrnovat expanzi. Zřetelná expanze oblaků byla zjištěna v 80%.Zahrnutí ...
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