\u30e1\u30bf\u968e\u5c64\u30c0\u30a4\u30ca\u30df\u30af\u30b9\u30e6\u30cb\u30c3\u30c8\u30bb\u30df\u30ca\u30fc\u3092\u958b\u50ac\u3057\u307e\u3059\u3002\u7686\u69d8\u306e\u3054\u53c2\u52a0\u304a\u5f85\u3061\u3057\u3066\u304a\u308a\u307e\u3059\u3002<\/p>\n\n\n\n
\u3010\u65e5\u6642\u3011<\/span> 2025\u5e746\u670825\u65e5\uff08\u6c34\uff0913:30-15:00<\/p>\n\n\n\n \u3010\u5834\u6240\u3011<\/span> \u6838\u878d\u5408\u79d1\u5b66\u7814\u7a76\u6240 \u7814\u7a76I\u671f\u68df8\u968e801\u4f1a\u8b70\u5ba4\uff0bZoom<\/p>\n\n\n\n \u3010\u8b1b\u6f141\u3011<\/span><\/p>\n\n\n\n Models for Stark broadening in astrophysical and laboratory plasmas<\/strong><\/p>\n\n\n\n Ibtissem Hannachi \uff0f \u5ba2\u54e1\u51c6\u6559\u6388\uff08\u30d0\u30c8\u30a5\u30ca\u7b2c\uff11\u5927\u5b66\uff09<\/strong><\/p>\n<\/blockquote>\n\n\n\n The Stark broadening of hydrogen spectral lines is a key tool for diagnosing both astrophysical and laboratory plasmas. Early models explained this broadening by considering how collisions with charged particles shorten the lifetime of the radiating atom. The Lorentz model successfully described line shapes broadened by electrons and was later extended to include the effect of static ions, forming the standard theory of Stark broadening. While this standard model agrees well with observations in dense arc plasmas, it becomes inaccurate for the lower-density plasmas found in many astrophysical and fusion environments. \u3010\u8b1b\u6f142\u3011<\/span><\/p>\n\n\n\n \u8fd1\u8d64\u5916\u5206\u5149\u3092\u7528\u3044\u305f\u30c0\u30a4\u30d0\u30fc\u30bf\u30d7\u30e9\u30ba\u30de\u8a3a\u65ad \/ Divertor plasma diagnostics using near-infrared spectroscopy<\/strong><\/p>\n\n\n\n \u56db\u7ac8\u6cf0\u4e00 \uff0f \u5ba2\u54e1\u51c6\u6559\u6388\uff08\u4eac\u90fd\u5927\u5b66\uff09<\/strong><\/p>\n<\/blockquote>\n\n\n\n \u8fd1\u8d64\u5916\u57df\u306b\u304a\u3051\u308b\u8f1d\u7dda\u30d7\u30ed\u30d5\u30a1\u30a4\u30eb\u306e\u7cbe\u5bc6\u5206\u5149\u306f\u3001\u8f1d\u7dda\u306b\u542b\u307e\u308c\u308b\u96fb\u78c1\u5834\u3084\u7c92\u5b50\u6e29\u5ea6\u30fb\u6d41\u901f\u306a\u3069\u306e\u60c5\u5831\u3092\u5206\u96e2\u3057\u3066\u53d6\u5f97\u3059\u308b\u305f\u3081\u306e\u6709\u52b9\u306a\u65b9\u6cd5\u3067\u3042\u308b\u3002\u6211\u3005\u306f\u672c\u65b9\u6cd5\u3092\u6d3b\u7528\u3057\u3001\u6838\u878d\u5408\u30d7\u30e9\u30ba\u30de\u306e\u30c0\u30a4\u30d0\u30fc\u30bf\u8a3a\u65ad\u3001\u30d7\u30e9\u30ba\u30de\u6ce2\u52d5\u306b\u8d77\u56e0\u3059\u308b\u4ea4\u6d41\u96fb\u5834\u306e\u8a08\u6e2c\u3001\u96fb\u5b50\u901f\u5ea6\u5206\u5e03\u306e\u7570\u65b9\u6027\u3067\u751f\u3058\u308b\u8f1d\u7dda\u504f\u5149\u306e\u9ad8\u7cbe\u5ea6\u8a08\u6e2c\u306a\u3069\u306b\u53d6\u308a\u7d44\u3093\u3067\u3044\u308b\u3002\u672c\u30bb\u30df\u30ca\u30fc\u3067\u306f\u3001\u30c0\u30a4\u30d0\u30fc\u30bf\u8a3a\u65ad\u306b\u304a\u3051\u308b\u5de5\u5b66\u7684\u8981\u6c42\u3092\u80cc\u666f\u3068\u3057\u3066\u3001\u8fd1\u8d64\u5916\u5206\u5149\u306b\u3088\u3063\u3066\u89b3\u6e2c\u53ef\u80fd\u306a\u7269\u7406\u91cf\u3001\u5b9f\u9a13\u4e0a\u306e\u8ab2\u984c\u306b\u3064\u3044\u3066\u6982\u8aac\u3059\u308b\u3002<\/p>\n\n\n\n High-resolution spectroscopy of emission line profiles in the near-infrared region is an effective method for isolating and extracting physical information included in the spectral lines, such as electromagnetic fields, and particle temperatures and flow velocities. We are utilizing this method to address several research topics, including divertor diagnostics in fusion plasmas, measurement of AC electric fields induced by plasma waves, and high-precision detection of emission line polarization resulting from anisotropic electron velocity distributions. In this seminar, I will talk about an overview of the measurable physical quantities by near-infrared spectroscopy along with experimental challenges in the context of engineering requirements for divertor diagnostics.<\/p>\n<\/blockquote>\n\n\n\n \u3010\u554f\u3044\u5408\u308f\u305b\u3011<\/span> \u203b(at) \u3092@\u306b\u5909\u3048\u3066\u304f\u3060\u3055\u3044\u3002<\/p>\n\n\n\n <\/p>\n","protected":false},"author":2,"featured_media":3336,"menu_order":0,"template":"","meta":{"_acf_changed":false,"footnotes":""},"ppma_author":[340],"class_list":["post-10178","news","type-news","status-publish","has-post-thumbnail","hentry"],"acf":[],"_links":{"self":[{"href":"https:\/\/unit.nifs.ac.jp\/research\/wp-json\/wp\/v2\/news\/10178","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/unit.nifs.ac.jp\/research\/wp-json\/wp\/v2\/news"}],"about":[{"href":"https:\/\/unit.nifs.ac.jp\/research\/wp-json\/wp\/v2\/types\/news"}],"author":[{"embeddable":true,"href":"https:\/\/unit.nifs.ac.jp\/research\/wp-json\/wp\/v2\/users\/2"}],"version-history":[{"count":12,"href":"https:\/\/unit.nifs.ac.jp\/research\/wp-json\/wp\/v2\/news\/10178\/revisions"}],"predecessor-version":[{"id":11423,"href":"https:\/\/unit.nifs.ac.jp\/research\/wp-json\/wp\/v2\/news\/10178\/revisions\/11423"}],"wp:featuredmedia":[{"embeddable":true,"href":"https:\/\/unit.nifs.ac.jp\/research\/wp-json\/wp\/v2\/media\/3336"}],"wp:attachment":[{"href":"https:\/\/unit.nifs.ac.jp\/research\/wp-json\/wp\/v2\/media?parent=10178"}],"wp:term":[{"taxonomy":"author","embeddable":true,"href":"https:\/\/unit.nifs.ac.jp\/research\/wp-json\/wp\/v2\/ppma_author?post=10178"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}\n
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To address these limitations, we present models that incorporate ion dynamics, such as the frequency fluctuation model used in the PPP code, and a plasma simulation coupled with numerical integration of the Schr\u00f6dinger equation for the emitter. These simulation approaches also enable the study of the effects of simultaneous periodic electric fields. We discuss potential spectroscopic diagnostics enabled by these models, with a focus on applications in magnetic fusion devices.<\/p>\n<\/blockquote>\n\n\n\n\n
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\u30e1\u30bf\u968e\u5c64\u30c0\u30a4\u30ca\u30df\u30af\u30b9\u30e6\u30cb\u30c3\u30c8 \u5f8c\u85e4\u57fa\u5fd7\uff08goto.motoshi(at)nifs.ac.jp\uff09<\/p>\n\n\n\n