{"id":2,"date":"2022-06-01T13:12:24","date_gmt":"2022-06-01T13:12:24","guid":{"rendered":"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/?page_id=2"},"modified":"2022-08-11T07:53:40","modified_gmt":"2022-08-11T07:53:40","slug":"home","status":"publish","type":"page","link":"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/","title":{"rendered":"Why an MHS team?"},"content":{"rendered":"\r\n<p>Gaining insight into the magnetic fields and plasma in solar active regions is very\u00a0important for studying various solar activities. So far the main approach to obtaining the\u00a0three-dimensional (3D) magnetic field structure of active regions is to extrapolate the\u00a0magnetic field from magnetograms measured in the photosphere. A basic assumption\u00a0in the past was to completely neglect all plasma effects and to perform the so-called\u00a0force-free field (FFF) extrapolations. A couple of methods (e.g PFSS, linear FFF, nonlinear\u00a0FFF) are available. Among these methods, till now, the NLFFF performed the\u00a0best when compared with observations. While the force-free assumption is well justified\u00a0in the solar corona, it is not the case in the photosphere and chromosphere. New\u00a0approaches that take into account plasma forces (e.g., plasma pressure and gravity)\u00a0developed rapidly in the last decade, for example magnetohydrostatic (MHS) extrapolations.\u00a0It was found that the MHS extrapolation when applied to simple test\u00a0cases performs better than the NLFFF extrapolation in terms of the accuracy of the reconstructed\u00a0magnetic field. To calculate the plasma forces correctly, the MHS extrapolation\u00a0requires a very high-resolution magnetogram (&lt;100 km) which could not be obtained\u00a0regularly in the past. However, such regular measurements of the magnetic field are\u00a0possible with the advent of the Daniel K. Inouye Solar Telescope (DKIST). Moreover,\u00a0the Solar Orbiter (SolO) provides an additional view angle which helps to constrain the\u00a0magnetic field modelling. We, therefore, gathered an <a href=\"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/team-members\">international team<\/a> to focus on the improvement of the MHS modelling with\u00a0unprecedented observations.\u00a0We plan to have two 5-day meetings. The <a href=\"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/meetings\">first meeting<\/a> is expected at the end of 2022\u00a0at ISSI-BJ while the <a href=\"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/meetings\">second meeting<\/a> will be held at ISSI a year after the first meeting.\u00a0Our team will improve the already available magnetic field models which help the solar\u00a0community to better understand activities in the solar atmosphere.<\/p>\r\n","protected":false},"excerpt":{"rendered":"<p>Gaining insight into the magnetic fields and plasma in solar active regions is very\u00a0important for studying various solar activities. So far the main approach to obtaining the\u00a0three-dimensional (3D) magnetic field structure of active regions is to extrapolate the\u00a0magnetic field from magnetograms measured in the photosphere. A basic assumption\u00a0in the past was to completely neglect all [&hellip;]<\/p>\n","protected":false},"author":44,"featured_media":0,"parent":0,"menu_order":0,"comment_status":"closed","ping_status":"closed","template":"","meta":{"footnotes":""},"class_list":["post-2","page","type-page","status-publish","hentry"],"_links":{"self":[{"href":"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/wp-json\/wp\/v2\/pages\/2","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/wp-json\/wp\/v2\/users\/44"}],"replies":[{"embeddable":true,"href":"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/wp-json\/wp\/v2\/comments?post=2"}],"version-history":[{"count":6,"href":"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/wp-json\/wp\/v2\/pages\/2\/revisions"}],"predecessor-version":[{"id":32,"href":"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/wp-json\/wp\/v2\/pages\/2\/revisions\/32"}],"wp:attachment":[{"href":"https:\/\/teams.issibern.ch\/magnetohydrostaticsolaratmosphere\/wp-json\/wp\/v2\/media?parent=2"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}