Results 31 to 40 of about 1,619,607 (208)

Comparison of Damping Mechanisms for Transverse Waves in Solar Coronal Loops [PDF]

The Astrophysical Journal, 2017
Abstract We present a method to assess the plausibility of alternative mechanisms to explain the damping of magnetohydrodynamic transverse waves in solar coronal loops. The considered mechanisms are resonant absorption of kink waves in the Alfvén continuum, phase mixing of Alfvén waves, and wave leakage.
María Montes-Solís, Iñigo Arregui
openaire   +2 more sources

Magnetohydrodynamic waves in structured atmospheres [PDF]

, 2012
The effect of structuring, in the form of magnetic or density inhomogeneities, on the magnetohydrodynamic (mhd) waves of an infinite plasma is investigated.
Edwin, Patricia Mary
core   +2 more sources

MHD waves in the solar north polar coronal hole

Astronomische Nachrichten, 2010
AbstractThe effects, hitherto not treated, of the temperature and the number density gradients, both in the parallel and the perpendicular direction to the magnetic field, of O VI ions, on the MHD wave propagation characteristics in the solar North Polar Coronal Hole are investigated.
Devlen, E., Pekunlu, E. R.
openaire   +3 more sources

Radiative damping of standing acoustic waves in solar coronal loops [PDF]

Astronomy & Astrophysics, 2008
Context. A detailed understanding of the physical processes that determine the damping timescales of magneto-acoustic waves is essential to interpret diagnostic results from the application of solar magneto-seismology.\ud Aims. The influence of the transition region and the importance of radiative emission, arising from equilibrium and non-equilibrium ...
Bradshaw, S.J., Erdelyi, R.
openaire   +3 more sources

Photospheric magnetic vortex structures [PDF]

, 2011
Using direct numerical magneto-hydrodynamic (MHD) simulations, we demonstrate the evidence of two physically different types of vortex motions in the solar photosphere.
Shelyag, S., Keenan, Francis, F. P. Keenan, Fedun, V., Mathioudakis, Mihalis, Mathioudakis, M., M. Mathioudakis, Shelyag, Sergiy, Erdélyi, Robert, Keenan, F. P., Erdelyi, R., R. Erdélyi, S. Shelyag, V. Fedun, Fedun, Viktor   +14 more
core   +2 more sources

Slow magnetoacoustic standing waves in a curved solar coronal slab [PDF]

Astronomy & Astrophysics, 2008
Summary: Aims. We consider a model of a two-dimensional solar coronal arcade to explore the effects of a curved magnetic field topology on excitation and attenuation of slow magnetoacoustic standing waves. Methods. The time-dependent ideal magnetohydrodynamic equations are solved numerically to find the spatial and temporal signatures of these waves ...
Ogrodowczyk, R., Murawski, K., Solanki, S.   +2 more
openaire   +4 more sources

MHD turbulence and heating of the open field-line solar corona [PDF]

, 2003
This paper discusses the possibility that heating of the solar corona in open field-line regions emanating from coronal holes is due to a nonlinear cascade, driven by low-frequency or quasi-static magnetohydrodynamic fluctuations.
Dmitruk, Pablo, Milano, L., Matthaeus, William H., Dmitruk, P., Milano, L. J., Matthaeus, W. H., Mullan, D. J., Oughton, Sean, S. Oughton, P. Dmitruk, W. H. Matthaeus, L. Milano, Oughton, S., D. J. Mullan   +13 more
core   +2 more sources

THREE-DIMENSIONAL PROPAGATION OF MAGNETOHYDRODYNAMIC WAVES IN SOLAR CORONAL ARCADES [PDF]

The Astrophysical Journal, 2010
We numerically investigate the excitation and temporal evolution of oscillations in a two-dimensional coronal arcade by including the three-dimensional propagation of perturbations. The time evolution of impulsively generated perturbations is studied by solving the linear, ideal magnetohydrodynamic (MHD) equations in the zero-beta approximation.
Rial, S., Arregui, I., Terradas, J., Oliver, R., Ballester, J. L.   +4 more
openaire   +2 more sources

Coronal Heating & Solar Wind Acceleration by Drift Waves

Journal of Physics: Conference Series, 2015
An alternative approach to the coronal heating problem, based on the theory of drift waves, has been proposed. The drift mode is the only mode that is able to survive the drastically different (collisional/collisionless) extremes in the different layers of the solar atmosphere. As a matter of fact, this mode is over stable, i.e.
Poedts, S., Kanella, Ch, Lapenta, G.
openaire   +1 more source

MHD simulations of coronal heating [PDF]

, 2015
The problem of heating the solar corona requires the conversion of magnetic energy into thermal energy. Presently, there are two promising mechanisms for heating the solar corona: wave heating and nanoflare heating.
Tam, Kuan V.
core   +2 more sources