{"id":6986,"date":"2025-06-06T18:39:52","date_gmt":"2025-06-06T16:39:52","guid":{"rendered":"https:\/\/brera.inaf.it\/?post_type=tesi&#038;p=6986"},"modified":"2025-06-09T12:36:52","modified_gmt":"2025-06-09T10:36:52","slug":"x-ray-binaries-master-merate-lc-probing-jet-evolution-in-x-ray-binaries-with-optical-polarimetry-m-c-baglio","status":"publish","type":"tesi","link":"https:\/\/brera.inaf.it\/en\/tesi\/x-ray-binaries-master-merate-lc-probing-jet-evolution-in-x-ray-binaries-with-optical-polarimetry-m-c-baglio\/","title":{"rendered":"\u00a0X-Ray Binaries &#8211; Master &#8211; MERATE (LC) \u2013 Probing Jet Evolution in X-ray Binaries with Optical Polarimetry \u2013 M.C. Baglio."},"content":{"rendered":"\n<div class=\"wp-block-stackable-columns stk-block-columns stk-block stk-4b166ce\" data-block-id=\"4b166ce\"><div class=\"stk-row stk-inner-blocks stk-block-content stk-content-align stk-4b166ce-column\">\n<div class=\"wp-block-stackable-column stk-block-column stk-column stk-block stk-5766870\" data-v=\"4\" data-block-id=\"5766870\"><style>@media screen and (min-width:768px){.stk-5766870{flex:var(--stk-flex-grow,1) 1 33.3% !important}}<\/style><div class=\"stk-column-wrapper stk-block-column__content stk-container stk-5766870-container stk--no-background stk--no-padding\"><div class=\"stk-block-content stk-inner-blocks stk-5766870-inner-blocks\">\n<figure class=\"wp-block-image size-full\"><img loading=\"lazy\" decoding=\"async\" width=\"2048\" height=\"1152\" src=\"https:\/\/brera.inaf.it\/wp-content\/uploads\/2025\/06\/magistrale-baglio.jpg\" alt=\"Immagine rappresentativa tesi Baglio\" class=\"wp-image-6980\"\/><\/figure>\n<\/div><\/div><\/div>\n\n\n\n<div class=\"wp-block-stackable-column stk-block-column stk-column stk-block stk-17cdb6d\" data-v=\"4\" data-block-id=\"17cdb6d\"><style>@media screen and (min-width:768px){.stk-17cdb6d{flex:var(--stk-flex-grow,1) 1 66.7% !important}}<\/style><div class=\"stk-column-wrapper stk-block-column__content stk-container stk-17cdb6d-container stk--no-background stk--no-padding\"><div class=\"stk-block-content stk-inner-blocks stk-17cdb6d-inner-blocks\">\n<h5 class=\"wp-block-heading\"><span style=\"color: #cf2e2e;\" class=\"stk-highlight\">X-ray Binaries<\/span><\/h5>\n\n\n\n<h5 class=\"wp-block-heading\">Master<\/h5>\n\n\n\n<h5 class=\"wp-block-heading\">Site: Merate (LC)<\/h5>\n\n\n\n<h5 class=\"wp-block-heading\">Duration:<\/h5>\n\n\n\n<p>1 year (master)<\/p>\n\n\n\n<h5 class=\"wp-block-heading\">Tutor<\/h5>\n\n\n\n<p>Maria Cristina Baglio<\/p>\n\n\n\n<h5 class=\"wp-block-heading\">Contact<\/h5>\n\n\n\n<p>maria.baglio AT inaf.it<\/p>\n\n\n\n<h5 class=\"wp-block-heading\">Description<\/h5>\n\n\n\n<p><strong><strong><strong>CONTEXT<\/strong><\/strong><\/strong> &#8211; X-ray binaries (systems in which a black hole or neutron star accretes matter from a companion star) undergo outbursts, dramatic increases in luminosity caused by instabilities in the accretion disc. As the outburst evolves, the accretion flow changes structure: in some phases, the inner disc recedes and is replaced by a hot, optically thin, radiatively inefficient flow; in others, the system launches relativistic jets. Both the hot flow and jets produce synchrotron emission, which may contribute to the system\u2019s optical polarization. At the same time, thermal components such as the outer disc can also introduce polarization through scattering. Studying how polarization evolves across different phases provides a unique window into the geometry and physical conditions of these emission regions.<\/p>\n\n\n\n<p><strong><strong>PROPOSED WORK<\/strong><\/strong> &#8211; This thesis will analyze multi-epoch optical polarimetric data acquired with the Very Large Telescope (VLT) for one black hole or neutron star X-ray binaries. Optical and near-infrared photometry from the LCO network and REM telescopes will complement the polarization data, tracing changes in spectral energy distribution and total flux across outburst phases.<\/p>\n\n\n\n<p>The project aims to disentangle the origins of optical polarization, whether from synchrotron emission in jets or hot flows, or from Thomson scattering in the outer accretion disc, and to study how these contributions evolve. Where available, simultaneous radio observations will provide direct insight into jet activity, enabling a full multiwavelength view of inflow\u2013outflow coupling.<\/p>\n\n\n\n<p>This work will help constrain the geometry and physical evolution of accreting systems during outburst, with implications for jet formation and accretion physics.<\/p>\n\n\n\n[<em>Credit image: WEB]<\/em><\/p>\n<\/div><\/div><\/div>\n<\/div><\/div>\n","protected":false},"excerpt":{"rendered":"<p>X-ray Binaries Master Site: Merate (LC) Duration: 1 year (master) Tutor Maria Cristina Baglio Contact maria.baglio AT inaf.it Description CONTEXT &#8211; X-ray binaries (systems in which a black hole or neutron star accretes matter from a companion star) undergo outbursts, dramatic increases in luminosity caused by instabilities in the accretion disc. As the outburst evolves, [&hellip;]<\/p>\n","protected":false},"author":1,"featured_media":6980,"parent":0,"menu_order":0,"comment_status":"open","ping_status":"closed","template":"","format":"standard","meta":{"footnotes":""},"categories":[28,26],"tags":[573,574,368,365,91],"class_list":["post-6986","tesi","type-tesi","status-publish","format-standard","has-post-thumbnail","hentry","category-master-thesis","category-thesis","tag-maria-cristina-baglio-2","tag-optical-polarimetry-2","tag-rem","tag-vlt","tag-x-ray-binaries-en"],"blocksy_meta":[],"featured_image_urls":{"full":["https:\/\/brera.inaf.it\/wp-content\/uploads\/2025\/06\/magistrale-baglio.jpg",2048,1152,false],"thumbnail":["https:\/\/brera.inaf.it\/wp-content\/uploads\/2025\/06\/magistrale-baglio.jpg",150,84,false],"medium":["https:\/\/brera.inaf.it\/wp-content\/uploads\/2025\/06\/magistrale-baglio.jpg",300,169,false],"medium_large":["https:\/\/brera.inaf.it\/wp-content\/uploads\/2025\/06\/magistrale-baglio.jpg",768,432,false],"large":["https:\/\/brera.inaf.it\/wp-content\/uploads\/2025\/06\/magistrale-baglio.jpg",1024,576,false],"1536x1536":["https:\/\/brera.inaf.it\/wp-content\/uploads\/2025\/06\/magistrale-baglio.jpg",1536,864,false],"2048x2048":["https:\/\/brera.inaf.it\/wp-content\/uploads\/2025\/06\/magistrale-baglio.jpg",2048,1152,false]},"post_excerpt_stackable":"<p>X-ray Binaries Master Site: Merate (LC) Duration: 1 year (master) Tutor Maria Cristina Baglio Contact maria.baglio AT inaf.it Description CONTEXT &#8211; X-ray binaries (systems in which a black hole or neutron star accretes matter from a companion star) undergo outbursts, dramatic increases in luminosity caused by instabilities in the accretion disc. As the outburst evolves, the accretion flow changes structure: in some phases, the inner disc recedes and is replaced by a hot, optically thin, radiatively inefficient flow; in others, the system launches relativistic jets. Both the hot flow and jets produce synchrotron emission, which may contribute to the system\u2019s&hellip;<\/p>\n","category_list":"<a href=\"https:\/\/brera.inaf.it\/en\/category\/thesis\/master-thesis\/\" rel=\"category tag\">Master thesis<\/a>, <a href=\"https:\/\/brera.inaf.it\/en\/category\/thesis\/\" rel=\"category tag\">Thesis<\/a>","author_info":{"name":"Maria Rosa Panzera","url":"https:\/\/brera.inaf.it\/en\/author\/maria-rosa-panzera\/"},"comments_num":"0 comments","_links":{"self":[{"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/tesi\/6986","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/tesi"}],"about":[{"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/types\/tesi"}],"author":[{"embeddable":true,"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/users\/1"}],"replies":[{"embeddable":true,"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/comments?post=6986"}],"version-history":[{"count":2,"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/tesi\/6986\/revisions"}],"predecessor-version":[{"id":6990,"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/tesi\/6986\/revisions\/6990"}],"wp:featuredmedia":[{"embeddable":true,"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/media\/6980"}],"wp:attachment":[{"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/media?parent=6986"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/categories?post=6986"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/brera.inaf.it\/en\/wp-json\/wp\/v2\/tags?post=6986"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}