{"id":2,"date":"2022-08-31T08:25:01","date_gmt":"2022-08-31T08:25:01","guid":{"rendered":"https:\/\/teams.issibern.ch\/magneticfieldactiveregions\/?page_id=2"},"modified":"2022-08-31T09:08:08","modified_gmt":"2022-08-31T09:08:08","slug":"home","status":"publish","type":"page","link":"https:\/\/teams.issibern.ch\/magneticfieldactiveregions\/","title":{"rendered":"Abstract"},"content":{"rendered":"<p><span id=\"page945R_mcid1\" class=\"markedContent\"><span dir=\"ltr\" role=\"presentation\">Sunspots are the hallmark of solar activity. High resolution spectropolarimetry is rapidly progressing<\/span> <span dir=\"ltr\" role=\"presentation\">toward a better physical understanding of small-scale structures in sunspot penumbra and umbra. However, our<\/span> <span dir=\"ltr\" role=\"presentation\">understanding of the magnetic structure of sunspots in the chromosphere and corona is lagging behind. In our<\/span> <span dir=\"ltr\" role=\"presentation\">modeling of magnetic fields in the corona, we still rely on various extrapolation methods, which do not include a<\/span> <span dir=\"ltr\" role=\"presentation\">realistic atmosphere nor are they constrained by the observations. <\/span><\/span><span id=\"page945R_mcid1\" class=\"markedContent\"><span dir=\"ltr\" role=\"presentation\">Our ISSI team will explore different approaches<\/span> <span dir=\"ltr\" role=\"presentation\">to address this deficiency.<\/span><\/span><\/p>\r\n<p><span id=\"page945R_mcid1\" class=\"markedContent\"><span dir=\"ltr\" role=\"presentation\">Nonlinear force-free field reconstructions that employ routinely available full-disk pho<\/span><span dir=\"ltr\" role=\"presentation\">tospheric vector magnetograms as bottom boundary conditions represent the state-of-the-art of coronal magnetic<\/span> <span dir=\"ltr\" role=\"presentation\">field modeling. Such reconstructions, however, are not unique and suffer from an inconsistency between a force-<\/span><span dir=\"ltr\" role=\"presentation\">free coronal magnetic field and non-force-free photospheric boundary condition, from which the coronal recon<\/span><span dir=\"ltr\" role=\"presentation\">struction is performed. Realistic time-dependent MHD models could help greatly, but are not expected to be rou<\/span><span dir=\"ltr\" role=\"presentation\">tinely available any time soon. The use of chromospheric vector magnetograms can aid the coronal part of the<\/span> <span dir=\"ltr\" role=\"presentation\">magnetic model, but does not help to build the magnetic model between the photospheric and chromospheric<\/span>\u00a0 <span dir=\"ltr\" role=\"presentation\">levels.<\/span><\/span><\/p>\r\n<p><span id=\"page945R_mcid1\" class=\"markedContent\"><span dir=\"ltr\" role=\"presentation\">Our ISSI team will use a combination of state-of-the-art modeling with existing and near future high-<\/span><span dir=\"ltr\" role=\"presentation\">resolution observations (e.g. from new DKI 4-meter aperture Solar Telescope, DKIST) to evaluate existing ap<\/span><span dir=\"ltr\" role=\"presentation\">proaches in modeling the chromospheric and coronal magnetic fields and identify key failure points in such mod<\/span><span dir=\"ltr\" role=\"presentation\">eling. The goal is to integrate newly available chromospheric and\/or coronal magnetic field data with the vector<\/span> <span dir=\"ltr\" role=\"presentation\">photospheric magnetograms to improve the magnetic field reconstructions. We will select several well-observed<\/span> <span dir=\"ltr\" role=\"presentation\">active regions, which have both chromospheric and coronal magnetic field diagnostics from optical and radio<\/span> <span dir=\"ltr\" role=\"presentation\">spectropolarimetry, construct their 3D coronal magnetic field models using various complementary techniques,<\/span> <span dir=\"ltr\" role=\"presentation\">and validate these models using the observations. As a result of this effort we will create better constrained models<\/span><span dir=\"ltr\" role=\"presentation\">of the coronal magnetic field, available for public use in the form of data cubes, codes, and scientific publications.<\/span><\/span><\/p>\r\n","protected":false},"excerpt":{"rendered":"<p>Sunspots are the hallmark of solar activity. High resolution spectropolarimetry is rapidly progressing toward a better physical understanding of small-scale structures in sunspot penumbra and umbra. However, our understanding of the magnetic structure of sunspots in the chromosphere and corona is lagging behind. In our modeling of magnetic fields in the corona, we still rely [&hellip;]<\/p>\n","protected":false},"author":59,"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\/magneticfieldactiveregions\/wp-json\/wp\/v2\/pages\/2","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/teams.issibern.ch\/magneticfieldactiveregions\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/teams.issibern.ch\/magneticfieldactiveregions\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/teams.issibern.ch\/magneticfieldactiveregions\/wp-json\/wp\/v2\/users\/59"}],"replies":[{"embeddable":true,"href":"https:\/\/teams.issibern.ch\/magneticfieldactiveregions\/wp-json\/wp\/v2\/comments?post=2"}],"version-history":[{"count":4,"href":"https:\/\/teams.issibern.ch\/magneticfieldactiveregions\/wp-json\/wp\/v2\/pages\/2\/revisions"}],"predecessor-version":[{"id":17,"href":"https:\/\/teams.issibern.ch\/magneticfieldactiveregions\/wp-json\/wp\/v2\/pages\/2\/revisions\/17"}],"wp:attachment":[{"href":"https:\/\/teams.issibern.ch\/magneticfieldactiveregions\/wp-json\/wp\/v2\/media?parent=2"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}