Description
Organisers: Patrick Antolin, Simon Daley-Yates, Jack Jenkins, Sargam Mulay, Christopher Osborne, Aaron W. Peat, Alexander Russell
The Sun offers unique insight and observational applications to the detailed understanding of stellar physics. The Sun serves as both a benchmark and laboratory for stellar processes. High-resolution and novel observations allow for the investigation of magnetic structure, coronal heating, condensations, and solar wind, to name a few. The broader statistical studies of stellar events can assist in the understanding of patterns and extremes of solar phenomena.
Stellar statistics constrain the frequency of, and energy associated with, extreme events. These, in turn, offer insight into coronal energy release mechanisms with applications to solar physics. Flare statistics and prominence formation are of great interest to the solar community as it can assist in the constraint of the formation and properties of these phenomena.
Recent advancements in both simulation and observation are gifting us new insight into and understanding of the aforementioned phenomena. Bridging solar and stellar astrophysics, both theoretical and observational, is essential to the understanding of solar and stellar processes. This session will focus on:
o Linking stellar flare, superflare, and CME statistics to solar coronal energy release mechanisms.
o Studying stellar winds to refine solar wind models and vice versa.
o Exploring solar/stellar prominence and condensation formation and/or ejection mechanisms, and properties.
o Investigating novel trends in coronal heating to resolve solar and stellar physics questions.
This session aims to foster interdisciplinary collaboration, and leverage stellar data to advance solar physics while using solar theories as a framework to understand stellar processes.
The Sun is approaching a transition in magnetic activity that has been observed in many of its siblings. Sun-like stars sustain magnetism by dynamo-action, powered by the interplay of convection and rotation. Stellar magnetic fields enable the heating of their atmospheres to millions of degrees and drive magnetised stellar winds. These winds play a crucial role in the evolution of Sun-like...
Solar flares are explosive releases of magnetic energy stored in the solar corona, driven by magnetic reconnection. These events accelerate particles, generating hard X-ray emissions. However, the energy transfer process remains poorly constrained, with competing theories proposing different acceleration mechanisms, including magnetohydrodynamic (MHD) turbulence. We investigate electron...
With the ongoing peak of the 25th solar cycle, the number of solar flare events is on the rise. This offers the perfect opportunity to study these phenomena in greater detail and understand the production and transport of high energy particles/radiations in interplanetary space. This is fundamentally important for space-weather predictions and protecting in-orbit assets. The multi-wavelength...
Stellar flares cannot be spatially resolved, which means that we have to extract complex three-dimensional behavior from a one-dimensional disk-integrated spectrum. Due to their proximity to Earth, solar flares can serve as a stepping stone for understanding their stellar counterparts, especially when using a Sun-as-a-star instrument in combination with spatially resolved observations. In this...
The study of coronal rain and other cool materials observed in the Sunโs upper atmosphere is becoming increasingly important given their connection to the fundamental mechanisms of coronal heating, flaring and eruption. The widely accepted formation mechanism of the phenomena is through concentrated footpoint heating of coronal loops. This heating leads to a cyclical process known as the...
We explored the impact that Doppler dimming and brightening effects from bulk motions of isolated structures have on the formation of Lyฮฑ, Hฮฑ, and Mgษชษชh line profiles. This study was carried out in the context of solar prominence physics, but will be applicable to different structures and/or in stellar contexts. We compared two regimes in which these effects manifest: when the prominence is...
In the solar atmosphere the catastrophic cooling phenomena known as coronal rain plays an important role in the wider context of coronal heating. Understanding coronal rain can help us put spatial and temporal constraints on the properties of the heating mechanisms. Coronal rain is observed to occur commonly above active regions as "quiescent" coronal rain, as opposed to the flare-driven kind...
