Abstract:
With modern imaging and spectral instruments observing in the
visible, EUV, X-ray and radio wavelengths, the detection of
oscillations in the solar outer atmosphere has become a routine
event. These oscillations are considered to be the signatures of a
wave phenomenon and are generally interpreted in terms of
magnetohydrodynamic (MHD) waves. With multi-wavelength observations
from ground and space-based instruments, it has been possible to
detect waves in a number of different wavelengths simultaneously and,
consequently, to study their propagation properties. Observed MHD
waves propagating from the lower solar atmosphere into the higher
regions of the magnetized corona have the potential to provide an
excellent insight into the physical processes at work at the
coupling point between these different regions of the Sun.
High-resolution wave observations combined with forward MHD
modelling can give an unprecedented insight into the connectivity of
the magnetized solar atmosphere, which further provides us with a
realistic chance to reconstruct the structure of the magnetic field in
the solar atmosphere. This type of solar exploration has been termed
atmospheric magneto-seismology. In this review we will summarise some
new trends in the observational study of waves
and oscillations, discussing their origin, and their propagation through the
atmosphere.
In particular, we will focus on waves and oscillations in open ({\it e.g.,}
solar plumes) and closed ({\it e.g.,} loops and prominences) magnetic
structures, where there have been a number of observational
highlights in the last few years. Furthermore, observations of waves in
filament fibrils allied with a better characterization of their
propagating and damping properties, the detection of prominence
oscillations in UV lines, and the renewed interest in
large-amplitude, quickly attenuated, prominence oscillations, caused
by flare or explosive phenomena, will be addressed.
Description:
Solar Physics, Vol. 246, No. 1, pp. 3-29
