The second meeting will take place from the 2nd-6th July 2018. The schedule is the following.<\/p>\n
Monday 2nd July<\/strong><\/span><\/p>\n Tuesday 3rd<\/strong><\/span><\/p>\n Wednesday 4th<\/strong><\/span><\/p>\n Thursday 5th<\/strong><\/span><\/p>\n Friday 6th<\/strong><\/span><\/p>\n 09:00 Open Discussion<\/p>\n <\/p>\n <\/p>\n <\/p>\n This is the programme for the first meeting, which took place from 27th March to 31st March 2017. Some of the talks are now available as a PDF or ppt.<\/p>\n Monday 27th March<\/strong><\/span> A brief overview of the history of atmospheric seismology, looking at key observations and theoretical models that have helped to develop the field.<\/p>\n 10:30 Break A look towards the future. Over the last few years, insights from SDO, CoMP and chromospheric observatories clearly show that the atmospheric plasma is highly dynamic. Such behaviour is typically neglected in magneto-seismological models and should be a future direction for theory. I discuss recent observations of waves in these highly dynamic plasma environments, highlighting areas with potential for future focus.<\/p>\n 13:00 Lunch<\/p>\n 14:00 Seismology of propagating kink MHD waves in the presence of flow<\/em><\/a> – \u00a0Marcel Goossens<\/span><\/strong><\/p>\n A recent evolution in research on MHD waves of the solar atmosphere is the detection of MHD waves in the presence of flows, see e.g. Morton (2014) and Morton et al.(2015). The present talk discusses ways to include background flows along the magnetic field in a seismological analysis for propagating kink MHD waves.<\/p>\n Seismology of propagating MHD waves in the presence of flows is more complicated than that for propagating MHD waves on a static background. For the latter case there are two observable quantities, i.e. the phase velocity and the damping length of the propagating wave. There are three quantities that we would like to determine by seismology, i.e. the Alfv \u0301en velocity, the density contrast and the quantity that determines the damping. In case of resonant absorption this quantity is the thickness of the non-uniform layer. For MHD waves in the presence of an equilibrium flow there is a forward and a backward propagating wave both with a phase velocity and a damping length. The quantities related to the background that appear in the seismological analysis are the Alfv \u0301en velocity, the density contrast, the velocity of flow, the velocity contrast, and the thickness of the nonuniform layers for density and velocity. In practice there are no accurate observations of all of these quantities.<\/p>\n This talk presents an analytical theory for propagating MHD waves in cylindrical waveg- uides with a flow along the waveguide based on the thin tube (TT) and the thin bound- ary (TB) approximations. The damping is assumed to be due to resonant absorption. The focus is on kink waves that contain transverse motions. Seismological applica- tions of this theory to observations as well as the limitations of the adopted TTTB approximations are discussed.<\/p>\n 16:00 F<\/a>orce-free magnetic fields in coronal seismology<\/a><\/em> – \u00a0Markus Aschwanden<\/span><\/strong><\/p>\n Tuesday\u00a028th March<\/strong><\/span> 10:30 Break Magnetic twist is thought to play an important role in for example,\u00a0coronal loops. One of the effects of twist is to modify the properties of the\u00a0eigenmodes of magnetic tubes. In the linear regime and under the presence of\u00a0twist, standing kink solutions are characterized by a change in polarisation\u00a0of the transverse displacement along the tube. Here we investigate the effect\u00a0of twist on the development of shear instabilities that appear, in the\u00a0nonlinear regime, at the tube boundary. The shear instabilities are produced\u00a0either by the jump in the azimuthal component of the velocity at the edge of\u00a0the sharp boundary between the internal and external part of the tube, or\u00a0either by the phase-mixing process taking place when there is a smooth\u00a0inhomogeneous layer. It is found that twist always delays the appearance of\u00a0the shear instability. This can have some important implications regarding\u00a0observations of transverse kink modes and the instability itself.<\/p>\n 13:00 Lunch We present and discuss the results of recent numerical simulations of coronal plasma disturbed by standing and propagating transverse waves. We will\u00a0show how the presence of these waves has a great influence on the appearance of the coronal plasma in the cross-section (perpendicular to the main magnetic field).\u00a0We will talk about the Kelvin-Helmholtz instability, turbulence, and other phenomena induced by the presence of transverse MHD waves in the solar corona.<\/p>\n Wednesday\u00a029th March<\/strong><\/span> I will discuss the ongoing effort to upgrade the CoMP instrument led by PI Enrico Landi (U Michigan). Upgrades include increased field-of-view, spatial resolution and wavelength range. My talk will focus on increased capabilities in coronal wave observations. The UCoMP will be deployed in the late summer 2017.<\/p>\n 10:30 Break Thursday\u00a030th March<\/strong><\/span> The magnetic nature of the Sun\u2019s tenuous atmosphere naturally supports the plethora of magnetohydrodynamic (MHD) wave activity that has been\u00a0brought to our attention in recent years. Sunspots, with their powerful magnetic fields, naturally provide energy conduits for upwardly propagating MHD wave activity. Previous work has focused on magneto-acoustic waves in the lower atmosphere of sunspots, including the manifestation of wave steepening in the form of umbral flashes (UFs). Here, high-resolution spectral imaging observations, inversion routines and MHD wave theory will be discussed to reveal how the signatures of Alfv\u00e9n wave dissipation is also prevalent within the confines of sunspot atmospheres. Improvements that will be brought about by the next generation of solar telescopes will also be described.<\/p>\n 10:30 Break As was previously found, transverse kink waves are Kelvin-Helmholtz unstable,\u00a0forming so-called TWIKH rolls. In this talk, I will perform forward modelling\u00a0of 3D simulations of coronal loops with TWIKH rolls. These forward models show\u00a0how TWIKH rolls can be observed in the corona. It is clear that these coronal\u00a0loop models are compatible with current observations of coronal loops, such as\u00a0appearing multi-stranded, having broad DEMs and peculiar Doppler shifts.<\/p>\n 13:00 Lunch 16:00 Study of waves from Aditya mission and NLST<\/em> – \u00a0Dipankar Banerjee<\/span><\/strong><\/p>\n Aditya-L1 is India’s first dedicated scientific mission to study the sun.\u00a0<\/span>Aditya-L1 will provide observations of Sun’s Photosphere, Chromosphere (NUV) and corona (Visible and NIR). I will give an overview of the capabilities of the NUV\u00a0full disk imager and also the coronagraph. The instrument specifications will provide new windows to the observation of waves. For wave diagnostic the current status with the existing instruments, its limitations will be\u00a0addressed. \u00a0 \u00a0How these new instruments can enhance our\u00a0understanding will be the point of discussion. I will also discuss on the current status of the National Large Solar Telescope project (NLST) and its high resolution capabilities\u00a0which will enhance our\u00a0<\/span><\/span>understanding on the wave properties.<\/span><\/p>\n Friday\u00a031st March<\/strong><\/span> The second meeting will take place from the 2nd-6th July 2018. The schedule is the following. Monday 2nd July 09:00 Meet & Introduction 09:30 Richard Morton – Magneto-seismology with large-scale statistical samples 10:30 Coffee Break 11:00 Norbet Magyar – Dynamic … Continue reading \n
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\n– Prominence threads and oscillations considering the physical effects of conduction and radiation (2nd)<\/li>\n
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\n09:00 Introduction from ISSI
\n09:30 A\u00a0history of solar atmospheric magnetoseismology<\/em> – \u00a0Gary Verth<\/span><\/strong><\/p>\n
\n11:00 Dynamic magnetoseismology: Pathways & road blocks<\/em><\/a> – \u00a0Richard Morton<\/span><\/strong><\/p>\n
\n09:00\u00a0Phase mixing of kink waves in solar flux tubes<\/em><\/a> – \u00a0Roberto Soler<\/span><\/strong><\/p>\n
\n11:00 Effect of magnetic twist on nonlinear transverse kink oscillations of line-tied magnetic tubes<\/em> – \u00a0Jaume Terradas<\/span><\/strong><\/p>\n
\n14:00 Spicule Dynamics with a 3D Touch<\/em> – \u00a0Rahul Sharma<\/span><\/strong>
\n16:00 How do transverse MHD waves shape the coronal plasma<\/em> – \u00a0Norbert Magyar<\/span><\/strong><\/p>\n
\n09:00 Upgraded Coronal Multi-channel Polarimeter (UCoMP)<\/em> – \u00a0Steve Tomczyk<\/span><\/strong><\/p>\n
\n11:00\u00a0Analysis, Modelling and Seismological Application of Wave Dynamics in Coronal Rain<\/em> – \u00a0Erwin Verwichte<\/span><\/strong>
\n13:00 Lunch
\n14:00 Open discussion<\/p>\n
\n09:00 Alfv\u00e9n Wave Dissipation in the Chromosphere<\/em> – \u00a0David Jess<\/span><\/strong><\/p>\n
\n11:00\u00a0Transverse wave induced Kelvin-Helmholtz (TWIKH) rolls in coronal loops and their observability<\/em> – \u00a0Tom Van Doorsselaere<\/span><\/strong><\/p>\n
\n14:00 Kink oscillations of non-stationary expanding magnetic flux tubes in the presence of flow<\/em> – \u00a0Misha Ruderman<\/span><\/strong><\/p>\n
\n09:00 Open discussion<\/p>\n","protected":false},"excerpt":{"rendered":"