Flows, Boundaries, InteractionsCristiana Dumitrache, Vasile Mioc, Nedelia A. Popescu Our workshop was divided in two important sections: (1) Sun and Heliosphere; (2) Stars and galaxies. The first section treated solar magnetic structures such as active regions, flares and CMEs, prominences and coronal streamers. Both observational and models works were presented. Flows, boundaries and interfaces were approached in numerical simulations. The second section of the workshop was devoted to stellar studies, extragalactic astronomy and especially cosmology. |
From inside the book
Results 1-3 of 18
Page 87
... curves ( 3 ) and ( 3 ' ) eject asymptotically from UE and tend to infinity ( 3 ) , or conversely ( 3 ' ) . Lastly , curves ( 5 ) and ( 5 ' ) eject from collision and tend to infinity ( 5 ) , or conversely ( 5 ' ) . Some " primed " curves ...
... curves ( 3 ) and ( 3 ' ) eject asymptotically from UE and tend to infinity ( 3 ) , or conversely ( 3 ' ) . Lastly , curves ( 5 ) and ( 5 ' ) eject from collision and tend to infinity ( 5 ) , or conversely ( 5 ' ) . Some " primed " curves ...
Page 89
... curves ( 3 ' ) and ( 2 ) have the same significance as regards trend ; it is the same for the curves ( 3 ) and ( 2 ' ) . The point p still has the look of a saddle , but an unusual one . All orbits that come from / end in it have the ...
... curves ( 3 ' ) and ( 2 ) have the same significance as regards trend ; it is the same for the curves ( 3 ) and ( 2 ' ) . The point p still has the look of a saddle , but an unusual one . All orbits that come from / end in it have the ...
Page 114
... curves p ( r ) , i . e . the one around the streamer axis , has not been completed yet ; therefore , we discuss , here , the lateral sides of these curves , which represent , according to the previous section , the line where the speed ...
... curves p ( r ) , i . e . the one around the streamer axis , has not been completed yet ; therefore , we discuss , here , the lateral sides of these curves , which represent , according to the previous section , the line where the speed ...
Contents
The Origin of Solar Eruptions | 13 |
Eruptive and Compact Flares | 22 |
Analysis of 3D Magnetic Reconnections of Two Active Regions | 31 |
Copyright | |
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Common terms and phrases
2007 American Institute active regions Alfvén analysis arcsecs Astron Astrophys Astrophysics black hole Boundaries calculations Cepheids chromosphere cluster components coronal loops coronal mass ejections cosmological current sheet curves damping length density Doppler Dumitrache dynamics EIT waves ejections emission energy equations equilibrium eruption evolution Ət FRW FIGURE filament flare flows flux rope flux tube frequency galaxy pairs helicity homoclinic orbit images Institute of Physics intensity Interactions edited km/s left panel M. S. Dimitrijević magnetic field magnetic field lines magnetic flux magnetic reconnections magnetogram Mioc modes N. A. Popescu non-standard observed obtained orbits oscillations perturbation phase portraits photometric photospheric plasma poloidal Popescu 2007 American radial velocity ribbons right panel Romanian Academy Rsun simulation SOHO solar corona Solar Phys solar wind spacetime spectral lines speed star Stark broadening Stark widths stellar streamer structure thermal topology UVCS wind model