Results 161 to 170 of about 11,319 (196)

Circular RNA PTPN4 Contributes to Blood-Brain Barrier Disruption during Early Epileptogenesis. [PDF]

Adv Sci (Weinh)
Yang J, Hu Y, Wang F, Peng X, Qi H, Yao Y, Zhang C, Zhou L, Liang X, Xu K, Zhang C, Zhang A, Chen C, Zeng Y, Zhang C, Gan G, Zhu X.   +16 more
europepmc   +1 more source

The Interplay Between Collisionless Magnetic Reconnection and Turbulence. [PDF]

Space Sci Rev
Stawarz JE, Muñoz PA, Bessho N, Bandyopadhyay R, Nakamura TKM, Eriksson S, Graham DB, Büchner J, Chasapis A, Drake JF, Shay MA, Ergun RE, Hasegawa H, Khotyaintsev YV, Swisdak M, Wilder FD.   +15 more
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Flying through an Eruption-associated Magnetic Reconnection Current Sheet in the Solar Corona

Patel R, Niembro T, Xie X, Seaton D, Badman S, Roy S, Rivera Y, Reeves K, Stenborg G, Hess P, West M, Feller A, Hirzberger J, Suarez DO, Solanki S, Strecker H, Valori G.   +16 more
europepmc   +1 more source

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Coronal loop detection from solar images

Pattern Recognition, 2009
zbMATH Open Web Interface contents unavailable due to conflicting licenses.
Durak, Nurcan, Nasraoui, Olfa, Schmelz, Joan   +2 more
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Solar Coronal Loops and Coronal Heating Models

AIP Conference Proceedings, 2005
Ever since it was realized, some sixty five years ago, that the solar corona is three orders of magnitude hotter than the underlying photosphere, scientists have puzzled over the reason for these extreme conditions. A number of plausible ideas have been put forward, including the dissipation of magnetohydrodynamic (MHD) waves and the dissipation of ...
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Current confinement in solar coronal loops

Solar Physics, 1981
In this paper solar coronal loops are regarded as regions of localized current flows. The main purpose is to investigate the consequences of current confinement rather than to produce a model. The physical and observational basis for this assumption are presented as well as the connection with previous studies on loop structure.
Claudio Chiuderi, Giorgio Einaudi
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Magnetic reconnection in solar coronal loops

Advances in Space Research, 1997
Abstract Simulations of the evolution of kink modes in line-tied coronal loops are presented which demonstrate the occurrence of magnetic reconnection in the non-linear stage of the instability. In loops which do not carry a net axial current (and are confined by a potential purely axial field) the reconnection is limited to the initial current ...
G Einaudi, R Lionello, M Velli
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Coronal Loops in Solar Active Regions

Publications of the Astronomical Society of Australia, 1989
AbstractWe discuss the appearance of solar active regions as seen in EUV line radiation in terms of a system of simple static coronal loop models. The loop models are based on those of Rosner et al. (1978) and may be understood in terms of the scaling laws introduced by these authors. We present here some generalized scaling laws which demonstrate that
C. J. Durrant, S. F. Brown
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Stability of solar coronal loops

Computer Physics Communications, 1990
Abstract The equations of magnetohydrodynamics do not contain an intrinsic length scale determining the size of phenomena. Hence, size only enters through the external geometrical properties of the configurations considered. This is one of the reasons why tokamaks and solar coronal loops may be considered as similar objects.
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Solar and stellar coronal loops

Advances in Space Research, 1991
Abstract X-ray and EUV pictures from space experiments (e.g. SKYLAB ) have revealed that the corona of the Sun consists of a variety of discrete structures - involving a range of timescales - which appear to outline the magnetic field lines emerging from the convection zone below the photosphere.
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