{"id":9700,"date":"2018-08-28T20:40:34","date_gmt":"2018-08-28T17:40:34","guid":{"rendered":"http:\/\/www.inasan.ru\/?p=9700"},"modified":"2018-08-28T20:41:55","modified_gmt":"2018-08-28T17:41:55","slug":"seminar_0386","status":"publish","type":"post","link":"http:\/\/www.inasan.ru\/en\/seminar_0386\/","title":{"rendered":"Astrophysical Seminar (30 August  2018, 11:00)"},"content":{"rendered":"<p><b>1) Speaker:<\/b> <em>A. Lazarian (University of Wisconsin-Madison, Madison, USA)<\/em><\/p>\n<p><b>Title:<\/b>\u00a0 &#8220;<em>Studying 3D distribution of magnetic field with velocity gradients&#8221;<\/em><\/p>\n<p><b>Abstract: <br \/>\n<\/b><\/p>\n<p>I shall discuss a radically new way to study magnetic field using velocity gradients. The foundations of this technique are rooted in the theory of turbulent reconnection and MHD turbulence. As a result, turbulent magnetic eddies are aligned with the local direction of magnetic field and the gradients of the velocity fluctuations trace magnetic field. I shall show the application of the technique to the numerical data, HI atomic hydrogen data and 13CO data. I shall demonstrate the 3D maps of galactic magnetic field that are obtained this way and the comparison of the magnetic field data that is obtained with the traditional techniques. Finally, I shall discuss the sister technique that use fluctuations of synchrotron intensity and synchrotron polarization to obtain the complementary information on galactic magnetic fields.<\/p>\n<p>&nbsp;<\/p>\n<p><strong><a href=\"http:\/\/www.inasan.ru\/en\/scientific_activities\/seminars\/inasan_astrophysical_seminar\/\">Sign up for the seminar<\/a><\/strong><\/p>\n<p>&nbsp;<\/p>\n","protected":false},"excerpt":{"rendered":"<p>1) Speaker: A. Lazarian (University of Wisconsin-Madison, Madison, USA) Title:\u00a0 &#8220;Studying 3D distribution of magnetic field with velocity gradients&#8221; Abstract: I shall discuss a radically new way to study magnetic field using velocity gradients. The foundations of this technique are rooted in the theory of turbulent reconnection and MHD turbulence. As a result, turbulent magnetic<\/p>\n<div class=\"read-more\"><a href=\"http:\/\/www.inasan.ru\/en\/seminar_0386\/\">Continue Reading&rsaquo;&rsaquo;<\/a><\/div>\n","protected":false},"author":12,"featured_media":0,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[6,1],"tags":[],"class_list":["post-9700","post","type-post","status-publish","format-standard","hentry","category-seminar","category-uncategorized"],"translation":{"provider":"WPGlobus","version":"3.0.0","language":"en","enabled_languages":["ru","en"],"languages":{"ru":{"title":true,"content":true,"excerpt":false},"en":{"title":true,"content":true,"excerpt":false}}},"_links":{"self":[{"href":"http:\/\/www.inasan.ru\/en\/wp-json\/wp\/v2\/posts\/9700","targetHints":{"allow":["GET"]}}],"collection":[{"href":"http:\/\/www.inasan.ru\/en\/wp-json\/wp\/v2\/posts"}],"about":[{"href":"http:\/\/www.inasan.ru\/en\/wp-json\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"http:\/\/www.inasan.ru\/en\/wp-json\/wp\/v2\/users\/12"}],"replies":[{"embeddable":true,"href":"http:\/\/www.inasan.ru\/en\/wp-json\/wp\/v2\/comments?post=9700"}],"version-history":[{"count":2,"href":"http:\/\/www.inasan.ru\/en\/wp-json\/wp\/v2\/posts\/9700\/revisions"}],"predecessor-version":[{"id":9729,"href":"http:\/\/www.inasan.ru\/en\/wp-json\/wp\/v2\/posts\/9700\/revisions\/9729"}],"wp:attachment":[{"href":"http:\/\/www.inasan.ru\/en\/wp-json\/wp\/v2\/media?parent=9700"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"http:\/\/www.inasan.ru\/en\/wp-json\/wp\/v2\/categories?post=9700"},{"taxonomy":"post_tag","embeddable":true,"href":"http:\/\/www.inasan.ru\/en\/wp-json\/wp\/v2\/tags?post=9700"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}