MAGHEAT: understanding energy deposition in the solar chromosphere
The mechanisms that heat the solar chromosphere and corona, and that drive the solar dynamo, arguably remain some of the foremost questions in solar and stellar physics. Here, we focus on the question of how energy is transported...
The mechanisms that heat the solar chromosphere and corona, and that drive the solar dynamo, arguably remain some of the foremost questions in solar and stellar physics. Here, we focus on the question of how energy is transported and released in the solar chromosphere. During the past 20 years, numerical simulations of the chromosphere have been used, with increasing degree of sophistication, to validate various proposed heating mechanisms. These studies have gradually come to recognise that the mechanisms that are likely dominant may be different in different parts of chromospheric fine structures. To make progress, we therefore need constraints from highly resolved observational data.
Recently, I implemented an inversion code that allows estimates of the overall chromospheric heating from spatially and spectrally resolved observational maps. Our results have unveiled very finely structured heating distributions with much larger amplitudes than the hitherto assumed canonical values. But a limitation is that this implementation cannot directly discriminate between the different heating mechanisms that have been proposed.
The goal of MAGHEAT is to identify what mechanisms are heating the chromosphere, characterize the energy flux that is being released into the chromosphere and separate the contribution from each mechanism in active regions and flares. This goal is achievable with the combination of the proposed development of novel non-LTE inversion methods, new hybrid rMHD/particle simulations, and the availability of datasets with unprecedented high spatial resolution, large field-of-view, and high S/N ratio from DKIST, the Sunrise III mission, NASA’s IRIS satellite and updated instrumentation at the Swedish 1-m Solar Telescope. We will use observational data from these facilities to reconstruct new 3D empirical models of the photosphere and chromosphere, which will allow us to identify the mechanisms that are responsible for the energy deposition.ver más
Seleccionando "Aceptar todas las cookies" acepta el uso de cookies para ayudarnos a brindarle una mejor experiencia de usuario y para analizar el uso del sitio web. Al hacer clic en "Ajustar tus preferencias" puede elegir qué cookies permitir. Solo las cookies esenciales son necesarias para el correcto funcionamiento de nuestro sitio web y no se pueden rechazar.
Cookie settings
Nuestro sitio web almacena cuatro tipos de cookies. En cualquier momento puede elegir qué cookies acepta y cuáles rechaza. Puede obtener más información sobre qué son las cookies y qué tipos de cookies almacenamos en nuestra Política de cookies.
Son necesarias por razones técnicas. Sin ellas, este sitio web podría no funcionar correctamente.
Son necesarias para una funcionalidad específica en el sitio web. Sin ellos, algunas características pueden estar deshabilitadas.
Nos permite analizar el uso del sitio web y mejorar la experiencia del visitante.
Nos permite personalizar su experiencia y enviarle contenido y ofertas relevantes, en este sitio web y en otros sitios web.