{"id":6629,"date":"2019-06-20T11:40:00","date_gmt":"2019-06-20T09:40:00","guid":{"rendered":"https:\/\/www.ieec.cat\/limitaciones-en-la-transici%c3%b3n-de-fase-de-hadr%c3%b3n-quark-y-propiedades-de-las-estrellas-gemelas-con-gw170817\/"},"modified":"2023-01-17T15:06:50","modified_gmt":"2023-01-17T14:06:50","slug":"limitaciones-en-la-transici%c3%b3n-de-fase-de-hadr%c3%b3n-quark-y-propiedades-de-las-estrellas-gemelas-con-gw170817","status":"publish","type":"post","link":"https:\/\/www.ieec.cat\/es\/limitaciones-en-la-transici%c3%b3n-de-fase-de-hadr%c3%b3n-quark-y-propiedades-de-las-estrellas-gemelas-con-gw170817\/","title":{"rendered":"Limitaciones en la transici\u00f3n de fase de hadr\u00f3n-quark y propiedades de las estrellas gemelas con GW170817"},"content":{"rendered":"<p>[et_pb_section fb_built=\u00bb1&#8243; fullwidth=\u00bbon\u00bb _builder_version=\u00bb4.14.8&#8243; _module_preset=\u00bbdefault\u00bb background_image=\u00bb\/wp-content\/uploads\/2022\/04\/slider-corpo2.jpg\u00bb height=\u00bb114px\u00bb global_colors_info=\u00bb{}\u00bb][\/et_pb_section][et_pb_section fb_built=\u00bb1&#8243; 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global_colors_info=\u00bb{}\u00bb sticky_enabled=\u00bb0&#8243; custom_css_main_element=\u00bbdisplay: inline-block;\u00bb]@ET-DC@eyJkeW5hbWljIjp0cnVlLCJjb250ZW50IjoiY3VzdG9tX21ldGFfZmVjaGFfZXZlbnRvIiwic2V0dGluZ3MiOnsiYmVmb3JlIjoiIiwiYWZ0ZXIiOiIiLCJlbmFibGVfaHRtbCI6Im9mZiJ9fQ==@[\/et_pb_text][et_pb_text _builder_version=\u00bb4.14.8&#8243; _dynamic_attributes=\u00bbcontent\u00bb _module_preset=\u00bbdefault\u00bb custom_margin=\u00bb0px|5px|0px||false|false\u00bb custom_padding=\u00bb0px||0px||false|false\u00bb hover_enabled=\u00bb0&#8243; global_colors_info=\u00bb{}\u00bb sticky_enabled=\u00bb0&#8243; custom_css_main_element=\u00bbdisplay: inline-block;\u00bb]@ET-DC@eyJkeW5hbWljIjp0cnVlLCJjb250ZW50IjoiY3VzdG9tX21ldGFfaG9yYV9ldmVudG8iLCJzZXR0aW5ncyI6eyJiZWZvcmUiOiIiLCJhZnRlciI6IiIsImVuYWJsZV9odG1sIjoib2ZmIn19@[\/et_pb_text][et_pb_text _builder_version=\u00bb4.14.8&#8243; _dynamic_attributes=\u00bbcontent\u00bb _module_preset=\u00bbdefault\u00bb custom_margin=\u00bb0px||0px||false|false\u00bb custom_padding=\u00bb0px||0px||false|false\u00bb hover_enabled=\u00bb0&#8243; global_colors_info=\u00bb{}\u00bb sticky_enabled=\u00bb0&#8243; module_class=\u00bbevent-organizations\u00bb]@ET-DC@eyJkeW5hbWljIjp0cnVlLCJjb250ZW50IjoiY3VzdG9tX21ldGFfb3JnYW5pemFjaW9uZXMiLCJzZXR0aW5ncyI6eyJiZWZvcmUiOiIiLCJhZnRlciI6IiIsImVuYWJsZV9odG1sIjoib2ZmIn19@[\/et_pb_text][et_pb_text _builder_version=\u00bb4.14.8&#8243; _dynamic_attributes=\u00bbcontent\u00bb _module_preset=\u00bbdefault\u00bb custom_margin=\u00bb0px||0px||false|false\u00bb custom_padding=\u00bb0px||0px||false|false\u00bb hover_enabled=\u00bb0&#8243; global_colors_info=\u00bb{}\u00bb sticky_enabled=\u00bb0&#8243;]@ET-DC@eyJkeW5hbWljIjp0cnVlLCJjb250ZW50IjoiY3VzdG9tX21ldGFfbHVnYXJfZXZlbnRvIiwic2V0dGluZ3MiOnsiYmVmb3JlIjoiIiwiYWZ0ZXIiOiIiLCJlbmFibGVfaHRtbCI6Im9mZiJ9fQ==@[\/et_pb_text][\/et_pb_column][\/et_pb_row][\/et_pb_section][et_pb_section fb_built=\u00bb1&#8243; _builder_version=\u00bb4.14.8&#8243; _module_preset=\u00bbdefault\u00bb custom_margin=\u00bb0px||||false|false\u00bb custom_padding=\u00bb0px||||false|false\u00bb top_divider_color=\u00bbRGBA(255,255,255,0)\u00bb top_divider_height=\u00bb0px\u00bb global_colors_info=\u00bb{}\u00bb][et_pb_row _builder_version=\u00bb4.14.8&#8243; _module_preset=\u00bbdefault\u00bb global_colors_info=\u00bb{}\u00bb][et_pb_column type=\u00bb4_4&#8243; _builder_version=\u00bb4.14.8&#8243; _module_preset=\u00bbdefault\u00bb global_colors_info=\u00bb{}\u00bb][et_pb_image src=\u00bbhttps:\/\/www.ieec.cat\/wp-content\/uploads\/2022\/12\/1560845952_04b809b64c90398b5a57401a97989e9b_2019_06_gw170817.png\u00bb alt=\u00bbConstraints on the hadron-quark phase transition and the properties of twin stars with GW170817&#8243; title_text=\u00bbConstraints on the hadron-quark phase transition and the properties of twin stars with GW170817&#8243; _builder_version=\u00bb4.14.8&#8243; _module_preset=\u00bbdefault\u00bb width=\u00bb600px\u00bb module_alignment=\u00bbcenter\u00bb global_colors_info=\u00bb{}\u00bb][\/et_pb_image][et_pb_text _builder_version=\u00bb4.14.8&#8243; _module_preset=\u00bbdefault\u00bb global_colors_info=\u00bb{}\u00bb]Las estrellas h&iacute;bridas son estrellas compactas que consisten en un n&uacute;cleo de quark puro o de materia mixta de hadr&oacute;n-quark y capas externas de materia hadr&oacute;nica (o nuclear). Dependiendo de sus caracter&iacute;sticas, la transici&oacute;n de fase hadr&oacute;n-quark puede conducir a una rama separada estable de masa-radio de estrellas h&iacute;bridas y, por lo tanto, a soluciones de &laquo;estrellas gemelas&raquo;, es decir, estrellas con masas similares y radios diferentes.<\/p>\n<p>Por lo tanto, una prueba de la existencia de estrellas gemelas mediante mediciones experimentales de masas-radios y deformabilidades de mareas puede proporcionar una firma para una transici&oacute;n de fase dentro de las estrellas de neutrones.<\/p>\n<p>En esta charla, mostrar&eacute; que los datos del evento de onda gravitacional GW170817 son compatibles con la existencia de estrellas gemelas y tambi&eacute;n podr&iacute;an interpretarse como la fusi&oacute;n de un sistema binario de estrellas h&iacute;bridas o de una estrella h&iacute;brida con una estrella de neutrones. Adem&aacute;s, combinando las observaciones de 2Msol y la informaci&oacute;n del evento GW170817, establecer&eacute; restricciones sobre los par&aacute;metros que caracterizan la transici&oacute;n de fase, las masas m&aacute;ximas y los radios de las estrellas de 1,4Msol descritas por las ecuaciones de estado que soportan las configuraciones de las estrellas gemelas.[\/et_pb_text][\/et_pb_column][\/et_pb_row][\/et_pb_section]<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Las estrellas h&iacute;bridas son estrellas compactas que consisten en un n&uacute;cleo de quark puro o de materia mixta de hadr&oacute;n-quark y capas externas de materia hadr&oacute;nica (o nuclear). Dependiendo de sus caracter&iacute;sticas, la transici&oacute;n de fase hadr&oacute;n-quark puede conducir a una rama separada estable de masa-radio de estrellas h&iacute;bridas y, por lo tanto, a soluciones [&hellip;]<\/p>\n","protected":false},"author":0,"featured_media":6624,"comment_status":"closed","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"_et_pb_use_builder":"on","_et_pb_old_content":"","_et_gb_content_width":"2880","footnotes":""},"categories":[95,73],"tags":[],"class_list":["post-6629","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-charla","category-eventos"],"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v27.2 - https:\/\/yoast.com\/product\/yoast-seo-wordpress\/ -->\n<title>Limitaciones en la transici\u00f3n de fase de hadr\u00f3n-quark y propiedades de las estrellas gemelas con GW170817 - IEEC<\/title>\n<meta name=\"robots\" content=\"index, follow, max-snippet:-1, max-image-preview:large, max-video-preview:-1\" \/>\n<link rel=\"canonical\" href=\"https:\/\/www.ieec.cat\/es\/limitaciones-en-la-transici%c3%b3n-de-fase-de-hadr%c3%b3n-quark-y-propiedades-de-las-estrellas-gemelas-con-gw170817\/\" \/>\n<meta property=\"og:locale\" content=\"es_ES\" \/>\n<meta property=\"og:type\" content=\"article\" \/>\n<meta property=\"og:title\" content=\"Limitaciones en la transici\u00f3n de fase de hadr\u00f3n-quark y propiedades de las estrellas gemelas con GW170817 - IEEC\" \/>\n<meta property=\"og:description\" content=\"Las estrellas h&iacute;bridas son estrellas compactas que consisten en un n&uacute;cleo de quark puro o de materia mixta de hadr&oacute;n-quark y capas externas de materia hadr&oacute;nica (o nuclear). 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