{"id":101645,"date":"2018-03-11T10:23:33","date_gmt":"2018-03-11T10:23:33","guid":{"rendered":"https:\/\/www.deberes.net\/tesis\/sin-categoria\/the-effect-of-activity-on-the-fundamental-properties-of-low-mass-stars\/"},"modified":"2018-03-11T10:23:33","modified_gmt":"2018-03-11T10:23:33","slug":"the-effect-of-activity-on-the-fundamental-properties-of-low-mass-stars","status":"publish","type":"post","link":"https:\/\/www.deberes.net\/tesis\/barcelona\/the-effect-of-activity-on-the-fundamental-properties-of-low-mass-stars\/","title":{"rendered":"The effect of activity on the fundamental properties of low-mass stars"},"content":{"rendered":"<h2>Tesis doctoral de <strong> Juan  Carlos Morales Peralta <\/strong><\/h2>\n<p>La comparaci\u00f3n entre los modelos de estructura estelar y las observaciones de estrellas de baja masa, indican que los radios y temperaturas efectivas que predicen dichos modelos son aproximadamente un 10% m\u00e1s peque\u00f1os y un 5% m\u00e1s altas, respectivamente, que las observaciones. Las estrellas binarias eclipsantes han demostrado ser una herramienta muy \u00fatil para testear estos modelos ya que permiten obtener las masas y radio de las estrellas con precisiones del orden del 2%. En este trabajo, se han obtenido las propiedades fundamentales de los sistemas binarios cm draconis e im virginis. La comparaci\u00f3n conjunta de estos sistemas, junto con otros con propiedades muy bien determinadas, se ha utilizado para testear los modelos de estructura estelar. Los resultados indican que la actividad magn\u00e9tica presente es estos sistemas es la causante de las diferencias entre los modelos y las observaciones, por su efecto sobre el transporte convectivo en el interior de las estrellas y por la aparici\u00f3n de manchas en su superficie.<\/p>\n<p>&nbsp;<\/p>\n<h3>Datos acad\u00e9micos de la tesis doctoral \u00ab<strong>The effect of activity on the fundamental properties of low-mass stars<\/strong>\u00ab<\/h3>\n<ul>\n<li><strong>T\u00edtulo de la tesis:<\/strong>\u00a0 The effect of activity on the fundamental properties of low-mass stars <\/li>\n<li><strong>Autor:<\/strong>\u00a0 Juan  Carlos Morales Peralta <\/li>\n<li><strong>Universidad:<\/strong>\u00a0 Barcelona<\/li>\n<li><strong>Fecha de lectura de la tesis:<\/strong>\u00a0 14\/06\/2010<\/li>\n<\/ul>\n<p>&nbsp;<\/p>\n<h3>Direcci\u00f3n y tribunal<\/h3>\n<ul>\n<li><strong>Director de la tesis<\/strong>\n<ul>\n<li>Ignasi Ribas Canudas<\/li>\n<\/ul>\n<\/li>\n<li><strong>Tribunal<\/strong>\n<ul>\n<li>Presidente del tribunal: \u00e1lvaro Gim\u00e9nez ca\u00f1ete <\/li>\n<li>thierry Forveille (vocal)<\/li>\n<li>  (vocal)<\/li>\n<li>  (vocal)<\/li>\n<\/ul>\n<\/li>\n<\/ul>\n<p>&nbsp;<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Tesis doctoral de Juan Carlos Morales Peralta La comparaci\u00f3n entre los modelos de estructura estelar y las observaciones de estrellas [&hellip;]<\/p>\n","protected":false},"author":1,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"site-sidebar-layout":"default","site-content-layout":"","ast-site-content-layout":"","site-content-style":"default","site-sidebar-style":"default","ast-global-header-display":"","ast-banner-title-visibility":"","ast-main-header-display":"","ast-hfb-above-header-display":"","ast-hfb-below-header-display":"","ast-hfb-mobile-header-display":"","site-post-title":"","ast-breadcrumbs-content":"","ast-featured-img":"","footer-sml-layout":"","theme-transparent-header-meta":"","adv-header-id-meta":"","stick-header-meta":"","header-above-stick-meta":"","header-main-stick-meta":"","header-below-stick-meta":"","astra-migrate-meta-layouts":"default","ast-page-background-enabled":"default","ast-page-background-meta":{"desktop":{"background-color":"var(--ast-global-color-4)","background-image":"","background-repeat":"repeat","background-position":"center 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