High cadence, 171 Å, TRACE observations show that outward propagating intensity
disturbances are a common feature in large, quiescent coronal loops. These oscillations are …

The remarkable magnetohydrodynamic stability of solar coronal loops has been attributed
to the anchoring of the ends of loops in the dense photosphere. However, all the previous …

… These loops can be divided into five different types, depending on their temperature,
density and length (see Priest, 1978; Hood and Priest, 1979a). Hood and Priest (1979a) …

… Abstract We present a comprehensive review of MHD wave behaviour in the neighbourhood
of coronal null points: locations where the magnetic field, and hence the local Alfvén speed, …

A theoretical description of slow MHD wave propagation in the solar corona is presented.
Two different damping mechanisms, namely thermal conduction and compressive viscosity, …

Context. The paper is concerned with heating of the solar corona by nanoflares: a superposition
of small transient events in which stored magnetic energy is dissipated by magnetic …

… For more details on wavelet analysis, we refer the reader to De Moortel and Hood (2000)
and references therein. However, we need to note here that the wavelet transform suffers from …

… and Hood 1989). Consider here, however, the magnetic field surface of the tube, and if
the flux (F) and axial twist are given, … For a uniform-twist field, Hood and Priest … AW …

… AW Hood and ER Priest … AW Hood and ER Priest: The Equilibrium of Solar Coronal
Magnetic Loops … For many of the cases that were computed (Hood and Priest, …

… This study is based on the results of De Moortel and Hood (2000) and De Moortel, Hood,
and Ireland (2002). A brief introduction to wavelet analysis and more details on some basic …