Magnetic structures in the solar atmosphere
نویسندگان
چکیده
منابع مشابه
Structures in the outer solar atmosphere
The structure and dynamics of the outer solar atmosphere are reviewed with emphasis on the role played by the magnetic field. Contemporary observations that focus on high resolution imaging over a range of temperatures, as well as UV, EUV and hard X-ray spectroscopy, demonstrate the presence of a vast range of temporal and spatial scales, mass motions, and particle energies present. By focussin...
متن کاملMagnetic Coupling in the Quiet Solar Atmosphere
Three kinds of magnetic couplings in the quiet solar atmosphere are highlighted and discussed, all fundamentally connected to the Lorentz force. First the coupling of the convecting and overshooting fluid in the surface layers of the Sun with the magnetic field. Here, the plasma motion provides the dominant force, which shapes the magnetic field and drives the surface dynamo. Progress in the un...
متن کاملMagnetic Transport On The Solar Atmosphere By Turbulent Ambipolar Diffusion
The lower solar atmosphere consists of partially ionized turbulent plasmas harbouring velocity field, magnetic field and current density fluctuations. The correlations amongst these small scale fluctuations give rise to large scale flows and magnetic fields which decisively affect all transport processes. The three fluid system consisting of electrons, ions and neutral particles supports nonide...
متن کاملModels for magnetic heating of the solar atmosphere
Sustaining the hot solar corona requires an energy flux of up to about 10erg cm−2s−1 whose source must be the photospheric motions below. However, the precise way this energy is transferred and damped still remains an open question. Here a review of recent advances in theoretical models for coronal heating, in the light of the fundamental observational results of the last decade, will be
متن کاملThe Solar Atmosphere
Looking at the solar photosphere, we see the top of the convection zone in the form of granulation: Hot gas rising from the solar interior as part of the energy transport process reaches a position where the opacity is no longer sufficient to prevent the escape of radiation. The gas expands, radiates, and cools and in so doing loses its buoyancy and descends. These motions, ultimately driven by...
متن کاملذخیره در منابع من
با ذخیره ی این منبع در منابع من، دسترسی به آن را برای استفاده های بعدی آسان تر کنید
ژورنال
عنوان ژورنال: Bulletin of the Australian Mathematical Society
سال: 1999
ISSN: 0004-9727,1755-1633
DOI: 10.1017/s0004972700032962