{"id":16915,"date":"2017-12-28T11:49:06","date_gmt":"2017-12-28T14:49:06","guid":{"rendered":"http:\/\/www.astrofisicamas.cl\/?p=16915"},"modified":"2023-08-04T22:44:15","modified_gmt":"2023-08-04T22:44:15","slug":"la-peculiar-anticorrelacion-del-cumulo-globular-del-bulbo-ngc-6440","status":"publish","type":"post","link":"https:\/\/astrofisicamas.cl\/en\/la-peculiar-anticorrelacion-del-cumulo-globular-del-bulbo-ngc-6440\/","title":{"rendered":"Nuestra Investigaci\u00f3n: La peculiar anticorrelaci\u00f3n del cumulo globular del bulbo NGC 6440"},"content":{"rendered":"<h4><em><strong>Por Francesco Mauro, investigador Instituto Milenio de Astrof\u00edsica y del Instituto de Astronom\u00eda de la Universidad Cat\u00f3lica del Norte\u00a0<\/strong><\/em><\/h4>\n<p><!--more--><\/p>\n<p><strong>Los c\u00famulos estelares son un conjunto de estrellas nacidas a dentro de la misma nube molecular, enormes complejos de gas fr\u00edo que existen dentro de las galaxias.<\/strong> <strong>La gravedad mutua las mantiene unidas a medida que envejecen, formando un claro sistema aislado.<\/strong> Existen dos tipos de c\u00famulos estelares: los c\u00famulos abiertos y los globulares. Los c\u00famulos globulares son t\u00edpicamente m\u00e1s viejos y m\u00e1s compactos. <strong>Los c\u00famulos globulares gal\u00e1cticos tienen aproximadamente la misma edad de la V\u00eda L\u00e1ctea, por esta raz\u00f3n son usados para estudiar su formaci\u00f3n y evoluci\u00f3n.<\/strong><\/p>\n<p><strong>Los astr\u00f3nomos podemos medir el brillo intr\u00ednseco de las estrellas en una cierta longitud de onda (y lo llamamos \u201cluminosidad\u201d). Tambi\u00e9n llamamos \u201ccolor\u201d a la diferencia entre la luminosidad en dos longitudes de onda diferentes <\/strong>(la raz\u00f3n es simple: una estrella azul ser\u00e1 m\u00e1s luminosa en la parte azul del espectro que en la roja, y viceversa). El gr\u00e1fico de la luminosidad de las estrellas versus su color es una poderosa herramienta de an\u00e1lisis que llamamos \u201c<strong>diagrama color-luminosidad\u201d<\/strong> (o diagrama color-magnitud si se usan magnitudes en vez de luminosidades). Cuando graficamos este diagrama para los miembros de un c\u00famulo globular, el gr\u00e1fico queda caracterizado por grupos de \u201cl\u00edneas\u201d muy caracter\u00edsticos. Las dos partes m\u00e1s brillantes son la rama de las gigantes rojas (estrellas que han agotado el hidr\u00f3geno en su carozo central y se preparan para quemar el helio), y la rama horizontal (estrellas que ya est\u00e1n quemando el helio en sus carozos centrales).<\/p>\n<p><strong>NGC6440 es un interesante c\u00famulo globular situado en la parte interior del bulbo gal\u00e1ctico<\/strong>. Muestra dos ramas horizontales con luminosidades ligeramente diferentes. <strong>Esta es una caracter\u00edstica inusual presente solo en este y otros dos c\u00famulos globulares gal\u00e1cticos.<\/strong> La doble rama horizontal podr\u00eda deberse a que las estrellas del c\u00famulo tienen una composici\u00f3n qu\u00edmica ligeramente diferente, lo que podr\u00eda deberse a su vez a ligeras inhomogeneidades en la nube molecular de la que se origin\u00f3 el c\u00famulo.<\/p>\n<p><strong>Para probar esta hip\u00f3tesis, seleccionamos siete estrellas de la rama de las gigantes rojas a fin de determinar con precisi\u00f3n sus composiciones qu\u00edmicas v\u00eda el an\u00e1lisis de sus espectros. Esper\u00e1bamos poder obtener informaci\u00f3n que nos permitiera entender mejor algunos detalles del entorno original de las estrellas y el proceso de formaci\u00f3n del c\u00famulo.<\/strong><\/p>\n<p>Encontramos valores uniformes de composici\u00f3n qu\u00edmica en los elementos del grupo del hierro (esto es: hierro y otros elementos qu\u00edmicos con n\u00famero at\u00f3mico parecido). Es decir, no hay variabilidad en contenido de elementos del grupo de hierro dentro del c\u00famulo. S\u00ed encontramos heterogeneidades en la abundancia qu\u00edmica de sodio y aluminio, y no encontramos la t\u00edpica anticorrelaci\u00f3n entre sodio y ox\u00edgeno, o aluminio y manganeso, que existe en los c\u00famulos globulares de nuestra galaxia. Tambi\u00e9n, la abundancia de aquellos elementos qu\u00edmicos cuyos n\u00facleos se forman uniendo n\u00facleos de helio es similar a la de las estrellas del bulbo gal\u00e1ctico, y mayor a la que suelen mostrar c\u00famulos globulares similares.<\/p>\n<p><strong>La composici\u00f3n qu\u00edmica global es semejante a la de las estrellas del bulbo gal\u00e1ctico, lo que sugiere que el c\u00famulo se form\u00f3 a la par de ellas.<\/strong> La abundancia de sodio, aluminio, manganeso y elementos del grupo de hierro est\u00e1 determinada por las explosiones de distintos tipos de supernovas en la nube molecular originaria. El patr\u00f3n abundancias qu\u00edmicas que descubrimos, que muestra peque\u00f1as diferencias dentro de una gen\u00e9rica similaridad, sugiere que <strong>NGC6440 se form\u00f3 muy al comienzo de la historia del bulbo gal\u00e1ctico en una zona de la nube molecular donde hab\u00edan explotado muchas supernovas.<\/strong><\/p>\n<figure id=\"attachment_16918\" aria-describedby=\"caption-attachment-16918\" style=\"width: 508px\" class=\"wp-caption aligncenter\"><a href=\"http:\/\/www.astrofisicamas.cl\/wp-content\/uploads\/2017\/12\/2017_12_28_FMauro_2.jpg\" rel=\"attachment wp-att-16918\"><img loading=\"lazy\" decoding=\"async\" class=\"wp-image-16918 size-full\" src=\"http:\/\/www.astrofisicamas.cl\/wp-content\/uploads\/2017\/12\/2017_12_28_FMauro_2.jpg\" alt=\"\" width=\"508\" height=\"500\" \/><\/a><figcaption id=\"caption-attachment-16918\" class=\"wp-caption-text\">Diagrama color-magnitud de NGC 6440 usando datos del proyecto VVV. Las estrellas seleccionadas para el an\u00e1lisis espectrosc\u00f3pico est\u00e1n marcadas con c\u00edrculos azules.<\/figcaption><\/figure>","protected":false},"excerpt":{"rendered":"<p>Por Francesco Mauro, investigador Instituto Milenio de Astrof\u00edsica y del Instituto de Astronom\u00eda de la Universidad Cat\u00f3lica del Norte\u00a0<\/p>","protected":false},"author":3,"featured_media":29196,"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":[59,1],"tags":[],"class_list":["post-16915","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-columnas","category-uncategorized"],"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v27.2 - https:\/\/yoast.com\/product\/yoast-seo-wordpress\/ -->\n<title>Nuestra Investigaci\u00f3n: La peculiar anticorrelaci\u00f3n del cumulo globular del bulbo NGC 6440 - 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