{"id":37,"date":"2019-09-13T13:57:55","date_gmt":"2019-09-13T11:57:55","guid":{"rendered":"http:\/\/spreadfast.astro.bas.bg\/?page_id=37"},"modified":"2019-09-13T13:57:55","modified_gmt":"2019-09-13T11:57:55","slug":"dsa-model","status":"publish","type":"page","link":"https:\/\/spreadfast.astro.bas.bg\/index.php\/about\/dsa-model\/","title":{"rendered":"DSA MODEL"},"content":{"rendered":"<p align=\"JUSTIFY\"><span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\"><span lang=\"en-US\">The system will treat the coronal acceleration of ions with an analytic model based on DSA theory (Kozarev &amp; Schwadron, 2016)<\/span><\/span><\/span><a class=\"sdfootnoteanc\" href=\"#sdfootnote1sym\" name=\"sdfootnote1anc\"><sup>1<\/sup><\/a><span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\"><span lang=\"en-US\">, specifically developed to take as input remote solar observations and data-driven model output from the CASHeW framework. The model solves for the coronal charged particle acceleration by large-scale CME-driven shocks. Our model uses time-dependent estimates of shock speed V<\/span><\/span><\/span><sub><span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\"><span lang=\"en-US\">shock<\/span><\/span><\/span><\/sub><span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\"><span lang=\"en-US\">, density jump ratio r, magnetic field strength <\/span><\/span><\/span><span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\"><span lang=\"en-US\">|<\/span><\/span><\/span><span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\"><span lang=\"en-US\">B<\/span><\/span><\/span><span style=\"font-family: MS Mincho, serif;\"><span style=\"font-size: small;\"><span lang=\"en-US\">\u2223<\/span><\/span><\/span> <span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\"><span lang=\"en-US\">and shock angle q<\/span><\/span><\/span><sub><span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\"><span lang=\"en-US\">BN<\/span><\/span><\/span><\/sub><span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\"><span lang=\"en-US\">, for multiple shock-crossing field lines. The model considers the minimum shock injection speeds. It takes as input a particle distribution function, and provides time-dependent distribution function spectra or fluxes, as output. It has been validated and used for the analysis of several SEP events. This model will be interfaced with the global EPREM particle model, described below.<\/span><\/span><\/span><\/p>\n<div id=\"sdfootnote1\">\n<p lang=\"it-IT\"><a class=\"sdfootnotesym\" href=\"#sdfootnote1anc\" name=\"sdfootnote1sym\">1<\/a><sup><span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\">\u0002<\/span><\/span><\/sup><span style=\"font-family: Arial, serif;\"><span style=\"font-size: small;\"> https:\/\/doi.org\/10.3847\/0004-637X\/831\/2\/120<\/span><\/span><\/p>\n<\/div>\n","protected":false},"excerpt":{"rendered":"<p>The system will treat the coronal acceleration of ions with an analytic model based on DSA theory (Kozarev &amp; Schwadron, 2016)1, specifically developed to take as input remote solar observations and data-driven model output from the CASHeW framework. The model solves for the coronal charged particle acceleration by large-scale CME-driven shocks. Our model uses time-dependent estimates of shock speed Vshock,<\/p>\n<p><a class=\"more-link\" href=\"https:\/\/spreadfast.astro.bas.bg\/index.php\/about\/dsa-model\/\">Read More<\/a><\/p>\n","protected":false},"author":1,"featured_media":0,"parent":21,"menu_order":0,"comment_status":"closed","ping_status":"closed","template":"","meta":{"footnotes":""},"_links":{"self":[{"href":"https:\/\/spreadfast.astro.bas.bg\/index.php\/wp-json\/wp\/v2\/pages\/37"}],"collection":[{"href":"https:\/\/spreadfast.astro.bas.bg\/index.php\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/spreadfast.astro.bas.bg\/index.php\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/spreadfast.astro.bas.bg\/index.php\/wp-json\/wp\/v2\/users\/1"}],"replies":[{"embeddable":true,"href":"https:\/\/spreadfast.astro.bas.bg\/index.php\/wp-json\/wp\/v2\/comments?post=37"}],"version-history":[{"count":1,"href":"https:\/\/spreadfast.astro.bas.bg\/index.php\/wp-json\/wp\/v2\/pages\/37\/revisions"}],"predecessor-version":[{"id":38,"href":"https:\/\/spreadfast.astro.bas.bg\/index.php\/wp-json\/wp\/v2\/pages\/37\/revisions\/38"}],"up":[{"embeddable":true,"href":"https:\/\/spreadfast.astro.bas.bg\/index.php\/wp-json\/wp\/v2\/pages\/21"}],"wp:attachment":[{"href":"https:\/\/spreadfast.astro.bas.bg\/index.php\/wp-json\/wp\/v2\/media?parent=37"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}