David Orozco Suárez
(Instituto de Astrofísica de Andalucía)
23/06/2016, 09:00
Spectropolarimetry in the He I 1083nm multiplet offers a
unique opportunity to
observe magnetic fields in the chromosphere. There, the
magnetic fields are expected
to be much lower in intensity than in the photosphere. In
this regard, the
polarization signals of the He I 1083nm multiplet are
sensitive to atomic level
polarization and to the joint action of the Hanle and...
Peter Levens
(University of Glasgow)
23/06/2016, 09:30
Coordinated observations of solar prominences can be a challenge to perform, and even
more so to analyse. During international campaigns in 2014 and 2015 we focused on
studying tornado-like prominences with a combination of space-based satellites (IRIS,
Hinode and SDO) and ground based telescopes (THEMIS, Meudon MSDP). We measured the
magnetic field strength and orientation in these...
Lakshmi Pradeep Chitta
(Max Planck Institute for Solar System Research)
23/06/2016, 09:50
Magnetic reconnection is thought to be responsible for eruptive events on the Sun,
from large-scale CMEs to small-scale events that are barely resolved. The height in
the solar atmosphere where the reconnection takes place may significantly influence
the morphology and appearance of the events. This might be the main distinction
between events such as e.g. Ellerman bombs, IRIS bombs, or...
Maria Loukitcheva
(Max-Planck-Institut fuer Sonnensystemforschung)
23/06/2016, 10:10
Atacama Large Millimeter/Submillimeter Array (ALMA) is opening a new chapter in the
study of the Sun by providing a leap in spatial resolution and sensitivity compared
to currently available millimeter wavelength observations. Using state of the art
radiation MHD simulations of the solar atmosphere we demonstrate the huge potential
of ALMA observations for uncovering the nature of the...
Patrick Antolin
(School of Mathematics and Statistics, University of St Andrews)
23/06/2016, 11:15
The solar atmosphere is permeated with MHD waves of Alfvenic
character. Such waves
are considered important energy carriers through which the
heating and morphology of
the corona may be explained. The highly inhomogeneous
coronal environment,
particularly in solar prominences, ensures the co-existence
of different wave modes
that are expected to be coupled through the robust...
Manuel Luna
(Instituto de Astrofísica de Canarias (IAC))
23/06/2016, 11:45
Large-amplitude oscillations in prominences are among the most spectacular phenomena
of the solar atmosphere. Such an oscillations involve motions with velocities above
20 km/s, and large portions of the filament that move in phase. These are triggered
by energetic disturbances as flares and jets. These oscillations are an excellent
tool to probe the not directly measurable filament...
Huadong Chen
(National Astronomical Observatories, Chinese Academy of Sciences)
23/06/2016, 12:05
Triggering mechanisms of solar eruptions have long been a challenge. A few previous
case studies have indicated that preceding gentle filament merging via magnetic
reconnection may launch following intense eruption, according to the tether-cutting
(TC) model. However, the detailed process of TC reconnection between filaments has
not been exhibited yet. In this work, we report the...
Takafumi Kaneko
(The University of Tokyo)
23/06/2016, 12:25
We show that topological change of coronal magnetic field can trigger radiative
condensation for in-situ prominence formation by 3D MHD simulation including thermal
conduction and optically thin radiative cooling. The multi-wavelength observation by
SDO/AIA (Bergeret al., 2012) has found the process of in-situ prominence formation,
in which the cool dense plasma of prominence came from...