{"id":10567,"date":"2021-08-02T14:13:00","date_gmt":"2021-08-02T05:13:00","guid":{"rendered":"https:\/\/www.icrr.u-tokyo.ac.jp\/?post_type=event_researcher&#038;p=10567"},"modified":"2021-10-25T22:13:00","modified_gmt":"2021-10-25T13:13:00","slug":"%e3%83%86%e3%82%b9%e3%83%88","status":"publish","type":"event_researcher","link":"https:\/\/www.icrr.u-tokyo.ac.jp\/en\/event_researcher\/10567\/","title":{"rendered":"PeVatrons and Star Formation Regions : Eduardo de la Fuente Acosta (Universidad de Guadalajara, ICRR)"},"content":{"rendered":"\n<figure class=\"wp-block-table\"><div class=\"js-scrollable\"><table><tbody><tr><td>Number<\/td><td>R3-2<\/td><\/tr><tr><td>&nbsp;Date&amp;Time<\/td><td>&nbsp;15:00-16:30pm, August 2, 2021<\/td><\/tr><tr><td>&nbsp;Place<\/td><td>Zoom: &nbsp;<a href=\"https:\/\/u-tokyo-ac-jp.zoom.us\/j\/81113787920?pwd=cTJzTU1hdzZpcVJHaDRyTVZvV2VCdz09\" target=\"_blank\" rel=\"noreferrer noopener\">https:\/\/u-tokyo-ac-jp.zoom.us\/j\/81113787920?pwd=cTJzTU1hdzZpcVJHaDRyTVZvV2VCdz09<\/a><\/td><\/tr><tr><td>&nbsp;Speaker<\/td><td>Eduardo de la Fuente Acosta<br>Departamento de Fisica, CUCEI, Universidad de Guadalajara, and<br>Institute for Cosmic Ray Research, University of Tokyo<\/td><\/tr><tr><td>&nbsp;Title<\/td><td>&#8220;PeVatrons and Star Formation Regions&#8221;<\/td><\/tr><tr><td>Abstract<\/td><td>After discovering the first PeVatron in the center of the Galaxy by the HESS observatory in 2016, the experiments AS-Tibet, HAWC, and LHAASO joined HESS to open a new window for study in the high energy astrophysics: the PeVatrons. PeVatrons are astronomical objects that can accelerate particles at energies of PeVs, energies impossible to reach yet in man-made accelerators or colliders. Thus, with PeVatrons, it is possible to contribute to the highest energy physics unprecedentedly. Besides, PeVatrons are a hot topic for gamma ray observatories that are currently under development, such as ALPACA, CTA, and SWGO.&nbsp;<br><br>On the other hand, in 2021, HAWC reported the observation of the ultra-high-energy gamma ray emission (&gt;100 TeV) from a stellar superbubble in the Cygnus region, powered by the massive stellar complex Cygnus OB2. Thus, the link between the star formation, observed mainly at radio and IR wavelengths, and the gamma rays at high energy emerge extraordinarily because, before this result, the observed gamma rays in star formation regions were assigned to pulsars. The HAWC result demonstrates without a doubt that massive star formation regions can be considered cosmic-ray accelerators.<br><br>In this talk, I present the status of the HAWC observatory located at Sierra Negra, Puebla, Mexico, its contributions, and its role in the PeVtron era, including a summary of our current knowledge on PeVatrons, focusing on the Cygnus star-forming region.&nbsp;<br><a href=\"https:\/\/www.icrr.u-tokyo.ac.jp\/prwps\/wp-content\/uploads\/ICRR_August_2021.pdf\">Presentation(PDF)<\/a><\/td><\/tr><\/tbody><\/table><\/div><\/figure>\n","protected":false},"featured_media":0,"template":"","tag_year":[],"class_list":["post-10567","event_researcher","type-event_researcher","status-publish","hentry","en-US"],"aioseo_notices":[],"aioseo_head":"\n\t\t<!-- All in One SEO 5.0.2 - aioseo.com -->\n\t<meta name=\"robots\" content=\"max-image-preview:large\" \/>\n\t<link rel=\"canonical\" href=\"https:\/\/www.icrr.u-tokyo.ac.jp\/en\/event_researcher\/10567\/\" \/>\n\t<meta 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