Gary Verth
(Sheffield University)
23/06/2016, 14:15
Within the last decade, due to significant improvements in
the spatial and temporal
resolution of chromospheric data, MHD wave studies in this
fascinating region of the
Sun's atmosphere have risen to the forefront of solar
physics research. In this talk
we review the most interesting MHD wave-related discoveries
by space and ground-based
instruments such as Hinode, IRIS, CRISP/SST and...
Shahin Jafarzadeh
(Institute of Theoretical Astrophysics, University of Oslo)
23/06/2016, 14:45
We characterise magnetohydrodynamics (MHD) waves in small magnetic elements and
investigate their propagation in the solar atmosphere by exploiting coordinated
observations with the Swedish 1 m Solar Telescope (SST) and the Interface Region
Imaging Spectrograph (IRIS). We use wavelet transform to analyse (horizontal)
displacement oscillations in magnetic bright points in several passbands...
Munehito Shoda
(The University of Tokyo)
23/06/2016, 16:00
Classically, the solar chromosphere was thought to be a dissipative medium for Alfvén
waves, in that those generated by the convective motions were thought to dissipate
most of their energy there. However, recent high-resolution observations near the
coronal base strongly suggest that the upward Alfvén waves are generated or amplified
in the chromosphere by the large amplitude acoustic...
Tony Arber
(University of Warwick)
23/06/2016, 16:20
By driving Alfven and kink waves into an expanding flux tube we demonstrated that
with a Poynting flux on 2x10^7 erg/s/cm^2 we can reproduce a heating profile broadly
consistent with the mid to upper chromosphere. The heating mechanism is through
ponderomotive coupling of Alfven waves to shock and it is the shocks which dissipate
and heat. These same shocks also produce jets similar to...
Sergiy Shelyag
(Northumbria University)
23/06/2016, 16:40
The most energetic part of the Sun, interior, due to its
plasma parameters is hidden
below the solar surface and invisible to the observer.
Nevertheless, the solar
interior generates the energy and provokes atmospheric
magnetic activity. Despite
great progress in both observational and simulation methods,
the mechanism of energy
transport from the solar convection zone into the...