{"id":85148,"date":"2018-03-10T00:09:33","date_gmt":"2018-03-10T00:09:33","guid":{"rendered":"https:\/\/www.deberes.net\/tesis\/sin-categoria\/formacion-y-evolucion-de-nebulosas-protoplanetarias-el-caso-de-oh231-84-2\/"},"modified":"2018-03-10T00:09:33","modified_gmt":"2018-03-10T00:09:33","slug":"formacion-y-evolucion-de-nebulosas-protoplanetarias-el-caso-de-oh231-84-2","status":"publish","type":"post","link":"https:\/\/www.deberes.net\/tesis\/ciencias-de-la-tierra-y-del-espacio\/formacion-y-evolucion-de-nebulosas-protoplanetarias-el-caso-de-oh231-84-2\/","title":{"rendered":"Formacion y evolucion de nebulosas protoplanetarias: el caso de oh231.8+4.2"},"content":{"rendered":"<h2>Tesis doctoral de <strong> Carmen Sanchez Contreras <\/strong><\/h2>\n<p>Esta tesis doctoral trata el problema de la formaci\u00f3n y evoluci\u00f3n de las nebulosas protoplanetarias(ppne), objetos que est\u00e1n efectuando la transici\u00f3n entre la rama asint\u00f3tica de las gigantes (agb) y la fase de nebulosa planetaria(pn). una parte importante de este trabajo se ha centrado en un objeto particularmente interesante, la ppn oh231.8+4.2. Para esta fuente hemos llevado a cabo un estudio detallado de la din\u00e1mica y propiepades f\u00edsicas y qu\u00edmicas del gas circunestelar de baja y alta excitaci\u00f3n. Dicho estudio se ha basado, por un lado, en observaciones de antena \u00fanica e interferom\u00e9tricas de la emisi\u00f3n de l\u00edneas en el rango de las ondas milim\u00e9tricas de un amplio n\u00famero de especies moleculares(12 co,13co, hco+, sio- t\u00e9rmico y m\u00e1ser-,hcn,hnc,so,so2,etc). estas observaciones, seguidas del apropiado an\u00e1lisis te\u00f3rico,han proporcionado la distribuci\u00f3n espacial de la masa, el momento cin\u00e9tico y las abundancias moleculares a lo largo de oh231.8+4.2. Hemos complementado las observacionesde la componente de baja excitaci\u00f3n de esta fuente con im\u00e1genes en el infrarrojo pr\u00f3ximo de la nebulosa de reflexi\u00f3n. El an\u00e1lisis conjunto de los datos ha permitido extraer importantes conclusiones acerca de cuando se origin\u00f3 y c\u00f3mo transcurre el proceso de interacci\u00f3n de vientos \u00c2\u00bfpost-agb\u00c2\u00bfas\u00ed como sus efectos, determinantes en la subsecuente evoluci\u00f3n hacia la fase de pn. La componente de mayor excitaci\u00f3n de oh231.8+4.2 ha sido estudiada a partir de observaciones en el \u00f3ptico (imagen directa y espectroscop\u00eda de rendija larga de las l\u00edneas nebulares m\u00e1s importantes) que han permitido conocer en detalle la distribuci\u00f3n y cinem\u00e1tica de esta componente as\u00ed como su excitaci\u00f3n. La combinaci\u00f3n de la informaci\u00f3n proporcionada por nuestros datos \u00f3pticos y de la emisi\u00f3n molecular e infrarroja permiten describir la evoluci\u00f3n de este objeto en los \u00faltimos   5000 a\u00f1os.  esta tesis doctoral tambi\u00e9n ha incluido el estudio del po<\/p>\n<p>&nbsp;<\/p>\n<h3>Datos acad\u00e9micos de la tesis doctoral \u00ab<strong>Formacion y evolucion de nebulosas protoplanetarias: el caso de oh231.8+4.2<\/strong>\u00ab<\/h3>\n<ul>\n<li><strong>T\u00edtulo de la tesis:<\/strong>\u00a0 Formacion y evolucion de nebulosas protoplanetarias: el caso de oh231.8+4.2 <\/li>\n<li><strong>Autor:<\/strong>\u00a0 Carmen Sanchez Contreras <\/li>\n<li><strong>Universidad:<\/strong>\u00a0 Complutense de Madrid<\/li>\n<li><strong>Fecha de lectura de la tesis:<\/strong>\u00a0 20\/06\/2000<\/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>Valentin Bujarrabal Fern\u00e1ndez<\/li>\n<\/ul>\n<\/li>\n<li><strong>Tribunal<\/strong>\n<ul>\n<li>Presidente del tribunal: manuel Rego fernandez <\/li>\n<li> Iba\u00f1ez cabanell Jos\u00e9 M\u00aa (vocal)<\/li>\n<li>Jes\u00fas Gomez gonzalez (vocal)<\/li>\n<li>Jes\u00fas Martin-pintado martin (vocal)<\/li>\n<\/ul>\n<\/li>\n<\/ul>\n<p>&nbsp;<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Tesis doctoral de Carmen Sanchez Contreras Esta tesis doctoral trata el problema de la formaci\u00f3n y evoluci\u00f3n de las nebulosas [&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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