Conveners
Poster Session 5.2
- D. Shaun Bloomfield (Northumbria University)
We report on diagnostics of the off-limb solar corona using coordinated observations of EUV allowed lines together with the coronal forbidden lines. We show that the electron densities obtained from the Fe XIII line ratios observed by both Hinode/EIS and COMP are in good agreement once the photoexcitation and background subtraction are both accounted for. In addition, the Hinode/EIS...
Ellerman Bomb-like brightenings of the hydrogen Balmer line wings in the quiet Sun, also known as quiet Sun Ellerman bombs (QSEBs), are a signature of the fundamental process of magnetic reconnection at the smallest observable scale in the lower solar atmosphere. We analyze high spatial resolution observations (0.″1) obtained with the Swedish 1-m Solar Telescope to explore signatures of QSEBs...
Analysis of the dynamics of the hot coronal plasma is the most promising method
to examine the contribution of wave-like phenomena in the global heating of the solar corona.
We present here a new, state-of-the art instrument for imaging spectroscopy:
the Solar Line Emission Dopplerometer (SLED). It is based on the Multi-channel
Subtractive Double Pass (MSDP) principle, which combines the...
A joint campaign of various space-borne and ground-based observatories, comprising the Hinode-SOT, IRIS, EIS (HOP 381, 10 – 22 October 2019), and the GREGOR Solar Telescope, investigated Quiet Sun regions for inferring the plasma β at photosphere, transition region, and corona. This campaign provided co-spatial and co-temporal observations, which can provide values of the magnetic field,...
Solar flares are generally thought to be the impulsive release of magnetic energy giving rise to a wide range of solar phenomena that influence the heliosphere and in some cases even conditions on Earth. Part of this liberated energy is used for particle acceleration and to heat up the solar plasma. The Spectrometer/Telescope for Imaging X-rays (STIX) instrument onboard the Solar Orbiter...
Condensations are observed in many astrophysical environments. In solar physics, common phenomena are coronal rain and prominences. Coronal rain consists of transient dense blobs that form in magnetic loops and rain down along the magnetic field lines. The prominences are cold, dense structures suspended in the hot, tenuous corona by the magnetic field.
Those structures are formed due to...
