Description
Organisers: Sarah Matthews, Patrick Antolin, Ineke De Moortel
In 2017 the international solar physics community agreed the highest priority science questions for solar physics in the coming decade and the measurements and instruments needed to answer those questions:
o Formation mechanisms of the hot and dynamic outer solar atmosphere
o Mechanisms of large-scale solar eruptions and foundations for predictions
o Mechanisms driving the solar cycle and irradiance variation
The realisation of those recommendations is the combination of two complementary solar space missions: NASA’s MUlti-slit Solar Explorer (MUSE) and JAXA’s multi-agency Solar-C. MUSE (launch 2027) will be a unique multi-slit spectrograph able to provide imaging spectroscopy of the corona at multiple wavelengths up to 100 times faster than current instruments. Solar-C (launched 2028), combines the EUV High-throughput Spectroscopic Telescope (EUVST) and the Solar Spectroscopic Irradiance Monitor (SoSpIM). EUVST will seamlessly and simultaneously observe a range of temperatures spanning more than three orders of magnitude from the chromosphere to the corona, providing unprecedented plasma diagnostic capability, while SoSpIM will provide complementary EUV spectral irradiance measurements. The combination of MUSE and EUVST will revolutionise our ability to probe the multi-scale nature of the physical processes in the corona, from small-scale energy release to large-scale impacts.
Supported by STFC and ESA the UK is both developing the short-wavelength camera for EUVST and helping to develop the science and tools to exploit MUSE, EUVST and SoSpIM. This session will bring together observers, modellers and theoreticians to discuss current work and future directions on all relevant science topics to promote optimum UK science return.
NASA's Multi-slit Solar Explorer (MUSE) mission is a new kind of spectrometer, targeted at spectroscopy of the rapidly evolving phenomena driving heating and dynamics of the solar atmosphere. MUSE is led by the Lockheed Martin Solar and Astrophysics Lab, with international science team involvement, including from the UK. Unlike previous space-based solar spectrometer designs in which a single...
The EUVST spectrograph (EUV High-throughput Spectroscopic Telescope) onboard the upcoming SOLAR-C spacecraft (JAXA), scheduled for launch in the late 2020s, will simultaneously observe a wide temperature range: from the 10,000-Kelvin chromosphere to the million-Kelvin corona, and even to 10 million-Kelvin solar flares, allowing the continuous tracking of plasma and energy transport. The...
An important goal of the Solar-C EUVST spectrometer is to make seamless observations from the chromosphere to the corona. Within its spectral range are potentially hundreds of chromospheric lines from highly excited, Rydberg levels in neutrals. Since the majority of the lines form in LTE the modelling is greatly simplified, and yet their diagnostic potential has largely been untapped in the...
During solar flares, nonthermal heating of the chromosphere induces overpressure, leading to explosive evaporation and consequent condensation to conserve momentum. While this phenomenon has been widely observed via Doppler shifts in various chromospheric and transition region lines, it has yet to be observed in the Si III 1206 Å line (logT≈4.7) which is set to be included in the SOLAR-C/EUVST...
Hinode EIS observations of flares are used to discuss the potential diagnostics
of hot (5-15 MK) plasma for the short wavelength channel of EUVST.
Several lines, rarely or never observed previously, are reported.
Comparisons between theoretical and observed intensities is generally very good, using my recent EIS radiometric calibration. However, discrepancies are present for a few cases,...
Solar flares are the most powerful energy-release processes in the solar system. During the flare, a huge amount of energy is released in a relatively compact space. This can lead to the electron mean free path becoming comparable to the temperature gradient inside the loop and, therefore, to a violation of the local thermal transport approximation. In this case, the commonly used Spitzer-Harm...
Inferring the polarisation state of coronal waves is key to understanding energy flux and dissipation in the outer solar atmosphere. By incorporating the polarisation, seismologists can improve constraints on the velocity amplitude and displacement estimates, leading to more accurate energy flux and deposition rates. We present a novel method to infer the polarisation of standing kink...
