Results 11 to 20 of about 1,089,572 (146)
An MHD model for solar coronal plumes [PDF]
, 1997 Solar coronal plumes are modelled by solving the steady, ideal, 2-D, magnetohydrodynamic (MHD) equations and assuming azimuthal symmetry around the plume axis. Since magnetic fields are believed to play an essential role in plume formation and structure, a self-consistent method of linearisation of the MHD equations with respect to the magnetic field ...
DEL ZANNA, LUCA, A. HOOD, A. LONGBOTTOM
core +4 more sources
Investigating Alfvénic wave propagation in coronal open-field regions. [PDF]
Nat Commun, 2015 The physical mechanisms behind accelerating solar and stellar winds are a long-standing astrophysical mystery, although recent breakthroughs have come from models invoking the turbulent dissipation of Alfvén waves.
Morton RJ, Tomczyk S, Pinto R.
europepmc +2 more sources
Solar Coronal Plumes and the Fast Solar Wind [PDF]
Journal of Astrophysics and Astronomy, 2015 The spectral profiles of the coronal Ne viii line at 77 nm have different shapes in quiet-Sun regions and coronal holes (CHs). A single Gaussian fit of the line profile provides an adequate approximation in quiet-Sun areas, whereas a strong shoulder on the long-wavelength side is a systematic feature in CHs.
Dwivedi, B., Wilhelm, K.
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Coronal plumes and the expansion of pressure‐balanced structures in the fast solar wind [PDF]
Journal of Geophysical Research: Space Physics, 1999 The expansion of a coronal hole filled with a discrete number of higher density filaments (plumes) in overall pressure balance with the ambient medium is described within the thin flux tube approximation. The resulting solar wind model extends the results of Parker [1964] and Velli et al. [1994] to nonisothermal temperature profiles and includes a flux
Casalbuoni, Sara +3 more
openaire +5 more sources
Effect of structuring on coronal loop oscillations [PDF]
, 2007 In this Thesis the theoretical understanding of oscillations in coronal structures is developed. In particular, coronal loops are modelled as magnetic slabs of plasma.
McEwan, Michael P.
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The Sun's global photospheric and coronal magnetic fields : observations and models [PDF]
, 2012 2012LRSP....9....6M Funding: STFC, the Leverhulme Trust and European Commission’s Seventh Framework Programme (FP7/2007-2013) under the grant agreement SWIFF (project no.
Anthony Yeates +6 more
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Coupling the solar surface and the corona: Coronal rotation, Alfvén wave-driven polar plumes [PDF]
AIP Conference Proceedings, 2013 Solar Wind 13: Proceedings of the Thirteenth International Solar Wind ...
R. F. Pinto +3 more
openaire +4 more sources
3D reconstruction of coronal loops by the principal component analysis [PDF]
, 2013 Knowing the three dimensional structure of plasma filaments in the uppermost part of the solar atmosphere, known as coronal loops, and especially their length, is an important parameter in the wave-based diagnostics of this part of the Sun.
Nisticò, Giuseppe +6 more
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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.
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Observational signatures of waves and flows in the solar corona [PDF]
, 2015 DM acknowledges support of a Royal Society University Research Fellowship and a KU Leuven Research Council senior research fellowship (SF/12/008). The research leading to these results has also received funding from the European Commission Seventh ...
Antolin, Patrick +4 more
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