{"id":3886,"date":"2023-03-06T11:46:35","date_gmt":"2023-03-06T02:46:35","guid":{"rendered":"https:\/\/sci.nao.ac.jp\/main\/?p=3886"},"modified":"2023-03-06T12:17:51","modified_gmt":"2023-03-06T03:17:51","slug":"20230306","status":"publish","type":"post","link":"https:\/\/sci.nao.ac.jp\/main\/highlights\/20230306","title":{"rendered":"Magnetism in High-Mass Stars"},"content":{"rendered":"\n<p>\u5929\u6587\u30b7\u30df\u30e5\u30ec\u30fc\u30b7\u30e7\u30f3\u30d7\u30ed\u30b8\u30a7\u30af\u30c8\u306e\u30b1\u30b9\u30c8\u30d8\u30a4 \u30b8\u30e7\u30eb\u30c8\u3055\u3093\u306e\u7814\u7a76\u6210\u679c\u304c\u767a\u8868\u3055\u308c\u307e\u3057\u305f\u3002<\/p>\n\n\n\n<p>Description:&nbsp;Magnetism is a ubiquitous property of astrophysical plasmas, yet stellar magnetism still remains far from being completely understood. In this review, we describe recent observational and modelling efforts and progress to expand our knowledge of the magnetic properties of high-mass stars. Several mechanisms (magneto-convection, mass-loss quenching, internal angular momentum transport, and magnetic braking) have significant implications for stellar evolution, populations, and end-products. Consequently, it remains an urgent issue to address and resolve open questions related to magnetism in high-mass stars.<\/p>\n\n\n\n<figure class=\"wp-block-image size-large\"><img loading=\"lazy\" decoding=\"async\" width=\"717\" height=\"1024\" src=\"https:\/\/sci.nao.ac.jp\/main\/wp-content\/uploads\/2023\/03\/roadmap-717x1024.png\" alt=\"\" class=\"wp-image-3887\" srcset=\"https:\/\/sci.nao.ac.jp\/main\/wp-content\/uploads\/2023\/03\/roadmap-717x1024.png 717w, https:\/\/sci.nao.ac.jp\/main\/wp-content\/uploads\/2023\/03\/roadmap-210x300.png 210w, https:\/\/sci.nao.ac.jp\/main\/wp-content\/uploads\/2023\/03\/roadmap-768x1096.png 768w, https:\/\/sci.nao.ac.jp\/main\/wp-content\/uploads\/2023\/03\/roadmap-1076x1536.png 1076w, https:\/\/sci.nao.ac.jp\/main\/wp-content\/uploads\/2023\/03\/roadmap-1435x2048.png 1435w, https:\/\/sci.nao.ac.jp\/main\/wp-content\/uploads\/2023\/03\/roadmap-154x220.png 154w, https:\/\/sci.nao.ac.jp\/main\/wp-content\/uploads\/2023\/03\/roadmap.png 1436w\" sizes=\"auto, (max-width: 717px) 100vw, 717px\" \/><figcaption class=\"wp-element-caption\"><strong>Figure 1.&nbsp;<\/strong>Simplified phenomenological picture of magnetic field evolution from early to late stages of stellar evolution for a typical high-mass star. The objects are not to scale. The time evolution proceeds from the molecular cloud phase towards the compact remnants. The black lines indicate magnetic field lines. For stars: Convective burning regions are shown in yellow. Convective non- burning regions are shown in red. Radiative regions are shown in blue. The distinct structure of the pre-supernova Red Supergiant is greatly simplified. See text for the description of the phases, labelled from 1 to 5. (Reference: Keszthelyi, Z. Magnetism in High-Mass Stars. Galaxies 2023, 11, 40. <a href=\"https:\/\/doi.org\/10.3390\/galaxies11020040\">https:\/\/doi.org\/10.3390\/galaxies11020040<\/a>)<\/figcaption><\/figure>\n\n\n\n<p>\u8a73\u3057\u304f\u306f\u3053\u3061\u3089\u306e\u30ea\u30f3\u30af\u3092\u3054\u89a7\u304f\u3060\u3055\u3044\u3002Weblink to the open-access paper:&nbsp;<a href=\"https:\/\/www.mdpi.com\/2075-4434\/11\/2\/40\/htm\">https:\/\/www.mdpi.com\/2075-4434\/11\/2\/40\/htm<\/a><\/p>\n","protected":false},"excerpt":{"rendered":"<p>\u5929\u6587\u30b7\u30df\u30e5\u30ec\u30fc\u30b7\u30e7\u30f3\u30d7\u30ed\u30b8\u30a7\u30af\u30c8\u306e\u30b1\u30b9\u30c8\u30d8\u30a4 \u30b8\u30e7\u30eb\u30c8\u3055\u3093\u306e\u7814\u7a76\u6210\u679c\u304c\u767a\u8868\u3055\u308c\u307e\u3057\u305f\u3002 Description:&nbsp;Magnetism is a ubiquitous property of astrophysi [&hellip;]<\/p>\n","protected":false},"author":45,"featured_media":3887,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"cybocfi_hide_featured_image":"yes","_locale":"ja","_original_post":"https:\/\/sci.nao.ac.jp\/main\/?p=3886","footnotes":""},"categories":[19],"tags":[],"class_list":["post-3886","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-highlights","ja"],"_links":{"self":[{"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/posts\/3886","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/users\/45"}],"replies":[{"embeddable":true,"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/comments?post=3886"}],"version-history":[{"count":5,"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/posts\/3886\/revisions"}],"predecessor-version":[{"id":3898,"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/posts\/3886\/revisions\/3898"}],"wp:featuredmedia":[{"embeddable":true,"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/media\/3887"}],"wp:attachment":[{"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/media?parent=3886"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/categories?post=3886"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/sci.nao.ac.jp\/main\/wp-json\/wp\/v2\/tags?post=3886"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}