{"id":16237,"date":"2017-08-30T09:16:46","date_gmt":"2017-08-30T12:16:46","guid":{"rendered":"http:\/\/www.astrofisicamas.cl\/?p=16237"},"modified":"2023-08-07T19:54:48","modified_gmt":"2023-08-07T19:54:48","slug":"nuestra-investigacion-nacimiento-y-evolucion-de-un-cumulo-estelar-joven","status":"publish","type":"post","link":"https:\/\/astrofisicamas.cl\/en\/nuestra-investigacion-nacimiento-y-evolucion-de-un-cumulo-estelar-joven\/","title":{"rendered":"Nuestra investigaci\u00f3n: Nacimiento y evoluci\u00f3n de un C\u00famulo Estelar Joven"},"content":{"rendered":"<h4><em><strong>Por Michael Kuhn, investigador postdoctoral MAS y del Instituto de F\u00edsica y Astronom\u00eda UV<\/strong><\/em><!--more--><\/h4>\n<p><strong>La formaci\u00f3n de c\u00famulos estelares es fundamental para la astronom\u00eda debido a que la mayor\u00eda de las estrellas se forman en grupos de cientos a miles de estrellas, y m\u00e1s tarde se dispersan.<\/strong> Las condiciones en estos c\u00famulos pueden implicar consecuencias duraderas para las estrellas y sistemas planetarios. Por ejemplo, en c\u00famulos densos, los primeros encuentros cercanos entre estrellas pueden truncar la parte externa de los discos protoplanetarios y, de este modo, limitan el tama\u00f1o de sistemas solares que se pueden formar. <strong>En nuestro propio Sistema Solar, las abundancias qu\u00edmicas de is\u00f3topos radiactivos apuntan a que nuestro Sol estuvo cerca de una explosi\u00f3n de supernova en el c\u00famulo que lo origin\u00f3.<\/strong><\/p>\n<p><strong>Para aprender c\u00f3mo es que los c\u00famulos evolucionan una vez que sus estrellas se han formado, hemos estudiado el c\u00famulo joven cercano NGC 6231.<\/strong> Utilizamos observaciones de diferentes instrumentos \u2013en particular del Observatorio Chandra X-Ray y del <em>survey<\/em> infrarrojo Vista Variables in the V\u00eda L\u00e1ctea (VVV)\u2013 para identificar miembros del c\u00famulo y estimar sus propiedades (por ejemplo, masa estelar y edad estelar). Nuestra primera publicaci\u00f3n cient\u00edfica presenta lo que es, a la fecha, el mejor cat\u00e1logo de estrellas j\u00f3venes en este c\u00famulo (<a href=\"http:\/\/adsabs.harvard.edu\/abs\/2017AJ....154...87K, Kuhn et al., AJ, 2017, 154, 87\">http:\/\/adsabs.harvard.edu\/abs\/2017AJ&#8230;.154&#8230;87K, Kuhn et al., AJ, 2017, 154, 87<\/a>).\u00a0 La imagen 1 muestra la fuerte emisi\u00f3n de rayos X desde las estrellas j\u00f3venes la cual se utiliza como criterio para seleccionar a sus miembros.<\/p>\n<p>La edad de las estrellas de NGC 6231 var\u00eda entre 2 y 7 millones de a\u00f1os, y la formaci\u00f3n de estrellas ya se ha detenido. Encontramos que la luminosidad de rayos X de las estrellas va disminuyendo con la edad. <strong>El c\u00famulo tiene una poblaci\u00f3n total de 5700\u20137500 estrellas, con masas que van desde menos de una d\u00e9cima hasta casi 50 veces la masa del Sol. Las propiedades de los rayos X indican que una gran fracci\u00f3n de las estrellas masivas tienen compa\u00f1eras binarias poco masivas [1].<\/strong><\/p>\n<p>Las observaciones tambi\u00e9n nos permiten establecer restricciones en la evoluci\u00f3n del c\u00famulo (Kuhn et al., AJ 2017, submitted). <strong>Descubrimos que la estructura global del c\u00famulo se ajusta muy bien al perfil de densidad superficial de un \u201celipsoide isot\u00e9rmico\u201d,<\/strong> mientras que otros modelos com\u00fanmente utilizados no coinciden para nada (imagen 2). El modelo isot\u00e9rmico corresponde a un c\u00famulo que est\u00e1 gravitacionalmente ligado, y no a una asociaci\u00f3n de estrellas cuyo futuro es dispersarse. Sin embargo, el c\u00famulo es aproximadamente ~ 10 veces m\u00e1s grande que un c\u00famulo t\u00edpico en su etapa de formaci\u00f3n de estrellas, lo que sugiere que NGC 6231 se ha expandido desde su tama\u00f1o original.<\/p>\n<p>Las relaciones entre la edad, tama\u00f1o y masa del c\u00famulo coinciden con tendencias previamente descubiertas en otras regiones de formaci\u00f3n de estrellas. Las regiones que usamos para comparaci\u00f3n provienen del proyecto MYStIX [2], y son regiones cuyos c\u00famulos probablemente est\u00e1n a\u00fan en etapa de consolidaci\u00f3n por v\u00eda de la fusi\u00f3n jer\u00e1rquica de sub-c\u00famulos [3]. La imagen 3 muestra el tama\u00f1o vs la masa para NGC 6231 (punto azul), para los c\u00famulos y sub-c\u00famulos del MYStIX (puntos negros), y para c\u00famulos en regiones \u201c<em>starburst\u201d<\/em> de formaci\u00f3n estelar muy activa (puntos rojos) [4]. El NGC 6231 se encuentra en la misma tendencia que los c\u00famulos\u00a0 del MYStIX, lo que sugiere que el NGC 6231 puede ser la etapa final del proceso de fusi\u00f3n jer\u00e1rquica. Por el contrario, las regiones <em>starburst<\/em> m\u00e1s extremas en la V\u00eda L\u00e1ctea y en galaxias cercanas podr\u00edan formarse de diferentes maneras.<\/p>\n<p>Para m\u00e1s informaci\u00f3n, se puede visitar el sitio web del MYStIX en:\u00a0<a href=\"http:\/\/astro.psu.edu\/mystix\">http:\/\/astro.psu.edu\/mystix\u00a0<\/a><\/p>\n<p>[1] Kuhn et al., AJ, 2017, 154, 87<\/p>\n<p>[2] Feigelson et al., ApJS, 2013, 209, 26<\/p>\n<p>[3] Kuhn et al., ApJ, 2015, 812, 131<\/p>\n<p>[4] Portegies Zwart et al., ARA&amp;A, 48, 431<\/p>\n<figure id=\"attachment_16239\" aria-describedby=\"caption-attachment-16239\" style=\"width: 300px\" class=\"wp-caption aligncenter\"><a href=\"http:\/\/www.astrofisicamas.cl\/wp-content\/uploads\/2017\/08\/2017_08_23_MKuhns1.jpg\"><img loading=\"lazy\" decoding=\"async\" class=\"wp-image-16239 size-medium\" src=\"http:\/\/www.astrofisicamas.cl\/wp-content\/uploads\/2017\/08\/2017_08_23_MKuhns1-300x300.jpg\" alt=\"\" width=\"300\" height=\"300\" \/><\/a><figcaption id=\"caption-attachment-16239\" class=\"wp-caption-text\">Figura 1<\/figcaption><\/figure>\n<figure id=\"attachment_16238\" aria-describedby=\"caption-attachment-16238\" style=\"width: 300px\" class=\"wp-caption aligncenter\"><a href=\"http:\/\/www.astrofisicamas.cl\/wp-content\/uploads\/2017\/08\/2017_08_23_MKuhns2.jpg\"><img loading=\"lazy\" decoding=\"async\" class=\"wp-image-16238 size-medium\" src=\"http:\/\/www.astrofisicamas.cl\/wp-content\/uploads\/2017\/08\/2017_08_23_MKuhns2-300x155.jpg\" alt=\"\" width=\"300\" height=\"155\" \/><\/a><figcaption id=\"caption-attachment-16238\" class=\"wp-caption-text\">Figura 2<\/figcaption><\/figure>\n<figure id=\"attachment_16242\" aria-describedby=\"caption-attachment-16242\" style=\"width: 300px\" class=\"wp-caption aligncenter\"><a href=\"http:\/\/www.astrofisicamas.cl\/wp-content\/uploads\/2017\/08\/2017_08_23_MKuhns3.jpg\"><img loading=\"lazy\" decoding=\"async\" class=\"wp-image-16242 size-medium\" src=\"http:\/\/www.astrofisicamas.cl\/wp-content\/uploads\/2017\/08\/2017_08_23_MKuhns3-300x267.jpg\" alt=\"\" width=\"300\" height=\"267\" \/><\/a><figcaption id=\"caption-attachment-16242\" class=\"wp-caption-text\">Figura 3<\/figcaption><\/figure>","protected":false},"excerpt":{"rendered":"<p>Por Michael Kuhn, investigador postdoctoral MAS y del Instituto de F\u00edsica y Astronom\u00eda UV<\/p>","protected":false},"author":3,"featured_media":29249,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"_coblocks_attr":"","_coblocks_dimensions":"","_coblocks_responsive_height":"","_coblocks_accordion_ie_support":"","_eb_attr":"","footnotes":""},"categories":[59],"tags":[],"class_list":["post-16237","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-columnas"],"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v27.2 - 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