UK-Solar Online Seminar Series

UK-SOSS Zoom Link:
Meeting ID: 953 3817 1418

Time: The UK-SOSS is held once a month on Thursday at 10:00 (UK time). In advance, we have agreed with the ESPOS (European Solar Physics Online Seminar) organisers in advance that UK-SOSS and ESPOS seminars will be not held in the same week.

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Organisers: Marianna Korsos (Aberystwyth University), Chris Nelson (Queen's University Belfast), and Jiajia Liu (Queen's University Belfast)

Next UK-SOSS seminars


Date Speaker
15th October 10:00 (UK time) Prof. Robertus Erdelyi (University of Sheffield)
12th November 10:00 (UK time)  Prof. Silvia Dalla (University of Central Lancashire)
10th December 10:00 (UK time)   Prof. Philippa Browning (University of Manchester) 
21th January 10:00 (UK time) Prof. Valery Nakariakov - University of Warwick

Previous UK-SOSS seminars

Waves and oscillations in the solar atmosphere

Prof. Robertus Erdelyi
University of Sheffield
Date: 10:00 am (UK time), 15th October 2020

Abstract: Satellite and ground-based observations from e.g. SOHO, TRACE, STEREO, Hinode, SDO and IRIS to DST/ROSA, IBIS, CoMP, STT/CRISP have all provided a wealth of evidence of waves and oscillations present in a wide range of spatial and temporal scales of the magnetised solar atmosphere. Our understanding about localised solar structures has been considerably changed in light of these superb spatial and temporal resolution observations. However, MHD waves not only enable us to perform sub-resolution solar magneto-seismology (SMS) but are also potential candidates to carry and damp the observed non-thermal energy in localised MHD waveguides. First, we will briefly outline the basic recent developments in MHD wave theory focussing on linear MHD waves both in symmetric and asymmetric waveguides. This latter may be an important aspect for the fantastic kitty: DKIST. Next, we will concentrate on the role of the most frequently studied wave classes, including the mysterious Alfven, and magneto-acoustic sub-classes of kink and sausage waves. Finally, we will address how solar MHD waves, swirls and solar jet formation may be related. We will argue to unite MHD wave and jet theories and make efforts to develop a common modelling platform with solar applications. An example will be shown where prevalent swirls, in the form of Alfven pulses, propagate upwards through the solar atmosphere dragging with them jets and reach the chromospheric layers. We will argue why this maybe seen as an important step towards understanding better the heating problem of the solar atmosphere.

Probing the Solar Cycle with BiSON: The Solar-Stellar Connection

Prof William Chaplin
University of Birmingham
Date: 10:00 am (UK time), 17th September 2020

Abstract: In this talk I will review how we are utilizing helioseismic observations made by the Birmingham Solar-Oscillations Network (BiSON) to provide unique inferences on the solar activity cycle, using its unprecedented long timebase dataset that is now extending into a fifth cycle. I will also discuss how we are using these data together with asteroseismic data, collected on other Sun-like stars by the NASA Kepler Mission, to provide a broader perspective on stellar activity and dynamo action in main-sequence stars.

Magnetic helicity: decompositions and methods of localization

Prof Mitchell Berger
University of Exeter
Date: 11:00 am, 16th of June, 2020

Abstract: Magnetic helicity is an ideal MHD invariant; it measures geometric and topological properties of a magnetic field. The talk will begin by reviewing helicity and its mathematical properties. It can be decomposed in several ways (for example, self and mutual helicity, Fourier spectra, field line helicity, linking, twist, and writhe). The talk will also review methods of measuring the helicity flux, as well as applications in solar and stellar astrophysics. I will then discuss some new developments in measuring localized concentrations of helicity in a well-defined, gauge invariant manner, using wavelets.

Where do solar eruptions come from?

Prof Anthony Yeates
Durham University
Date: 11:00 am, 19th May 2020

Abstract: An oft-quoted idea in solar physics is that coronal mass ejections are, fundamentally, the Sun's way of shedding the magnetic helicity that is continually generated by its interior flows. In this talk, I will show how models are helping to give us a handle on the build up of magnetic helicity in the corona (the Sun's lower atmosphere): how much is injected, where it collects, and how it is ultimately ejected. This requires time-evolving coronal magnetic field models as well as new tools for analysing the distribution of magnetic helicity.

Probing energy release and transport in explosive events

Prof Sarah Matthews
University College London
Date: 11:00 am, 21st April 2020

Abstract: The magnetic field of the corona stores the energy that is released via magnetic reconnection during solar flares and coronal mass ejections (CMEs). Flares with CMEs are often described by the ‘standard’ eruptive flare (CSHKP) model and this offers a conceptual framework in which to investigate the global characteristics of the energy release and transport in the context of the magnetic field configuration. The low plasma beta environment of the corona means the magnetic field plays a central role in the energy transport, and different magnetic field configurations can lead to a variety of outcomes in terms of the evolution of the energy release, the efficiency of the energy transport mechanisms and the locations where the energy is deposited. Despite the often rather good agreement between observations and the ‘standard’ model, many open questions remain particularly in respect to the triggering of the energy release. In this talk I will discuss how multi-wavelength spectroscopy used in tandem with magnetic field information can help shed light on some of these open questions.

Aspects of MHD Wave Heating in the Complex Solar Atmosphere

Prof Ineke De Moortel
University of St Andrews
Date: 11:00 am, 24th of March 2020

Abstract: In a series of numerical experiments, we investigate the possible role of MHD waves in the energy and mass cycle in the complex solar corona. Using 3D MHD simulations of transverse, Alfvenic waves, we look at the role of chromospheric evaporation, the complexity of the magnetic field and the power spectrum of the wave driver. We focus on the efficiency of the wave-based heating in our models, in particular whether heating provided by the waves can balance coronal losses and whether proposed wave heating mechanisms are in fact self-consistent.

The UK-SOSS is supported by Aberystwyth University and Queen’s University Green Fund