Results 31 to 40 of about 16,482 (212)
High-frequency waves in the solar coronal plasma [PDF]
Astronomy & Astrophysics, 2006 We derived numerical solutions of a dispersion equation in order to analyze the effect of finite plasma temperature on the highfrequency wave dispersion characteristics in conditions of hot magnetized plasma in the solar corona. Spectra of the high-frequency eigen modes of these plasma were determined in conditions when the electron gyrofrequency is ...
V. G. Ledenev +2 more
openaire +1 more source
The role of torsional Alfven waves in coronal heating [PDF]
, 2009 In the context of coronal heating, among the zoo of MHD waves that exist in the solar atmosphere, Alfven waves receive special attention. Indeed, these waves constitute an attractive heating agent due to their ability to carry over the many different ...
Antiochos +40 more
core +1 more source
Fast magnetohydrodynamic waves in a solar coronal arcade [PDF]
Astronomy & Astrophysics, 2017 Aims. To investigate detailed properties of fast MHD modes of a three-dimensional waveguide for a cylindrical magnetic arcade.\ud \ud Methods. To derive governing equations and dispersion relations for different density profiles and to numerically solve them to obtain\ud discrete eigenvalues for fast modes and the corresponding eigenfunctions.\ud \ud ...
Thackray, H., Jain, R.
openaire +4 more sources
Influence of the Lower Atmosphere on Wave Heating and Evaporation in Solar Coronal Loops
The Astrophysical Journal Letters, 2023 We model a coronal loop as a 3D magnetic cylinder in a realistic solar atmosphere that extends from the chromosphere to the corona. Kink oscillations, believed to be ubiquitous in the solar corona, are launched in the loop.
Mingzhe Guo +5 more
doaj +1 more source
Research progress in coronal magnetic field measurements
地球与行星物理论评, 2022 Different solar atmospheric layers are connected by the magnetic field of the Sun, which is the primary source for various types of solar activity. The magnetic activity of the Sun has a significant impact on the solar-terrestrial environment and human ...
Zihao Yang +6 more
doaj +1 more source
Observational Quantification of the Energy Dissipated by Alfv\'en Waves in a Polar Coronal Hole: Evidence that Waves Drive the Fast Solar Wind [PDF]
, 2013 We present a measurement of the energy carried and dissipated by Alfv\'en waves in a polar coronal hole. Alfv\'en waves have been proposed as the energy source that heats the corona and drives the solar wind.
Hahn, Michael, Savin, Daniel W.
core +1 more source
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. +2 more
openaire +3 more sources
Resonantly Damped Propagating Kink Waves in Longitudinally Stratified Solar Waveguides
, 2011 It has been shown that resonant absorption is a robust physical mechanism to explain the observed damping of magnetohydrodynamic (MHD) kink waves in the solar atmosphere due to naturally occurring plasma inhomogeneity in the direction transverse to the ...
Goossens, Marcel +3 more
core +1 more source
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
The Astrophysical Journal Letters, 2023 We propose that coronal heating in EUV coronal plumes is weaker, not stronger, than in adjacent nonplume coronal magnetic funnels. This expectation stems from (i) the observation that an EUV plume is born as the magnetic flux at the foot of the plume’s ...
Ronald L. Moore +3 more
doaj +1 more source