{"id":47843,"date":"2020-06-28T07:55:59","date_gmt":"2020-06-28T07:55:59","guid":{"rendered":"https:\/\/www.deberes.net\/tesis\/sin-categoria\/pulsacion-entre-las-estrellas-delta-scuti-con-bajo-contenido-en-helio\/"},"modified":"2020-06-28T07:55:59","modified_gmt":"2020-06-28T07:55:59","slug":"pulsacion-entre-las-estrellas-delta-scuti-con-bajo-contenido-en-helio","status":"publish","type":"post","link":"https:\/\/www.deberes.net\/tesis\/astronomia-y-astrofisica\/pulsacion-entre-las-estrellas-delta-scuti-con-bajo-contenido-en-helio\/","title":{"rendered":"Pulsacion entre las estrellas delta scuti con bajo contenido en helio"},"content":{"rendered":"<h2>Tesis doctoral de <strong> Manuel Saez Cano <\/strong><\/h2>\n<p>La existencia  en la parte roja de la banda de inestabilidad  de estrellas pulsantes del tipo  delphini que presentan anomalias de abundancia  esta en contradiccion con la teoria de la difusion  que predice la total desaparicion del helio de las capas externas.  proponemos que las envolturas de las estrellas  del no estan completamente desprovistas de helio. Un mecanismo de mezcla parcial podria mantener una abundancia intermedia de he  perimitiendo las sobreabundancias metalicas y restableciendo una abundancia normal de ca.  los modelos de envoltura que hemos calculado con importantes mejoras en la fisica (principalmente en las opacidades) muestran que para un log tc x 3.9 la variabilidad se obtiene para y=0.18 los escasos datos observacionales disponibles apoyan la hipotesis de que todas las  del son variables y que estas giran mas rapidamente que las an clasicas<\/p>\n<p>&nbsp;<\/p>\n<h3>Datos acad\u00e9micos de la tesis doctoral \u00ab<strong>Pulsacion entre las estrellas delta scuti con bajo contenido en helio<\/strong>\u00ab<\/h3>\n<ul>\n<li><strong>T\u00edtulo de la tesis:<\/strong>\u00a0 Pulsacion entre las estrellas delta scuti con bajo contenido en helio <\/li>\n<li><strong>Autor:<\/strong>\u00a0 Manuel Saez Cano <\/li>\n<li><strong>Universidad:<\/strong>\u00a0 Granada<\/li>\n<li><strong>Fecha de lectura de la tesis:<\/strong>\u00a0 01\/01\/1981<\/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>Annie Baglin<\/li>\n<\/ul>\n<\/li>\n<li><strong>Tribunal<\/strong>\n<ul>\n<li>Presidente del tribunal:  De Or\u00fas Navarro Juan  Jos\u00e9 <\/li>\n<li>Jes\u00fas Biel Gaye (vocal)<\/li>\n<li>Francisco Sanchez Martinez (vocal)<\/li>\n<li>Ramon Canal Masgorez (vocal)<\/li>\n<\/ul>\n<\/li>\n<\/ul>\n<p>&nbsp;<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Tesis doctoral de Manuel Saez Cano La existencia en la parte roja de la banda de inestabilidad de estrellas pulsantes [&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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