{"id":1726,"date":"2017-12-14T10:37:21","date_gmt":"2017-12-14T13:37:21","guid":{"rendered":"https:\/\/iate.oac.uncor.edu\/?p=1726"},"modified":"2017-12-14T10:37:21","modified_gmt":"2017-12-14T13:37:21","slug":"migracion-planetaria-y-el-origen-de-las-poblaciones-exoplanetarias-cerca-de-las-resonancias-32-y-21","status":"publish","type":"post","link":"https:\/\/iate.oac.uncor.edu\/en\/2017\/12\/14\/migracion-planetaria-y-el-origen-de-las-poblaciones-exoplanetarias-cerca-de-las-resonancias-32-y-21\/","title":{"rendered":"Migraci\u00f3n planetaria y el origen de las poblaciones exoplanetarias cerca de las resonancias 3:2 y 2:1"},"content":{"rendered":"
\n

X. S. Ramos<\/span>1<\/sup>,2<\/sup>, C. Charalambous<\/span>1<\/sup>, P. Ben\u00edtez-Llambay<\/span>1<\/sup>,2<\/sup> and C. Beaug\u00e9<\/span>1<\/sup><\/p>\n<\/div>\n

1<\/sup> Instituto de Astronom\u00eda Te\u00f3rica y Experimental, Observatorio Astron\u00f3mico, Universidad Nacional de C\u00f3rdoba, Laprida 854, X5000BGR, C\u00f3rdoba, Argentina
\ne-mail: xramos@oac.unc.edu.ar
\n2<\/sup> Niels Bohr International Academy, The Niels Bohr Institute, Blegdamsvej 17, 2100 Copenhagen \u00d8, Denmark<\/p>\n

Resumen<\/strong><\/p>\n

En este trabajo\u00a0(2017A&A…602A.101R<\/a>) presentamos un estudio anal\u00edtico y num\u00e9rico de la migraci\u00f3n orbital y la captura en resonancia de sistemas con dos planetas ficticios, con masas en el rango de las s\u00faper-Tierras, experimentando migraci\u00f3n de Tipo-I. Encontramos que, dependiendo del \u00edndice de forma del disco y la proximidad a la estrella central, el valor promedio de la raz\u00f3n de per\u00edodos, P2\/P1, entre ambos planetas muestra una desviaci\u00f3n importante respecto del valor nominal de la resonancia estudiada. Para planetas atrapados en la conmensurabilidad 2:1, esta desviaci\u00f3n puede alcanzar valores del orden de 0.1 para per\u00edodos orbitales de 1 d\u00eda, mientras que los sistemas en la resonancia de movimientos medios (RMM) 3:2 muestran desviaciones menores para todo valor de semieje mayor.<\/p>\n

\n

\"\"<\/p>\n

Estas propiedades est\u00e1n en buen acuerdo con la distribuci\u00f3n observada de exoplanetas casi resonantes, independientemente del m\u00e9todo con que fueron detectados. Mostramos que los sistemas en RMM 2:1 alejados de su estrella, como HD 82943 y HR 8799, se caracterizan por desviaciones muy peque\u00f1as de la resonancia nominal, mientras que valores mayores t\u00edpicamente corresponden a sistemas planetarios descubiertos por Kepler, con per\u00edodos orbitales de pocos d\u00edas. Contrariamente, aquellos sistemas en la vecindad de la resonancia 3:2 muestran poco apartamiento, sin dependencia significativa con la distancia orbital. En conclusi\u00f3n, nuestros resultados indican que la distribuci\u00f3n de sistemas planetarios Kepler alrededor de las RMMs 3:2 y 2:1 son consistentes con configuraciones resonantes obtenidas como consecuencia de una migraci\u00f3n suave en un disco laminar acampanado, y no se requieren fuerzas externas para describir la configuraci\u00f3n observada, ni su dependencia con la conmensurabilidad o la distancia a la estrella central.<\/p>\n

Abstract<\/strong><\/p>\n

We present an analytical and numerical study of the orbital migration and resonance capture of fictitious two-planet systems with masses in the super-Earth range undergoing Type-I migration. We find that, depending on the flare index and proximity to the central star, the average value of the period ratio, P2 \/P1, between both planets may show a significant deviation with respect to the nominal value. For planets trapped in the 2:1 commensurability, offsets may reach values on the order of 0.1 for orbital periods on the order of 1 day, while systems in the 3:2 mean-motion resonance (MMR) show much smaller offsets for all values of the semimajor axis.<\/p>\n

These properties are in good agreement with the observed distribution of near-resonant exoplanets, independent of their detection method. We show that 2:1-resonant systems far from the star, such as HD 82943 and HR 8799, are characterized by very small resonant offsets, while higher values are typical of systems discovered by Kepler with orbital periods approximately a few days. Conversely, planetary systems in the vicinity of the 3:2 MMR show little offset with no significant dependence on the orbital distance. In conclusion, our results indicate that the distribution of Kepler planetary systems around the 2:1 and 3:2 MMR are consistent with resonant configurations obtained as a consequence of a smooth migration in a laminar flared disk, and no external forces are required to induce the observed offset or its dependence with the commensurability or orbital distance from the star.<\/p>\n

 <\/p>","protected":false},"excerpt":{"rendered":"

X. S. Ramos1,2, C. Charalambous1, P. Ben\u00edtez-Llambay1,2 and C. Beaug\u00e91 1 Instituto de Astronom\u00eda Te\u00f3rica y Experimental, Observatorio Astron\u00f3mico, Universidad Nacional de C\u00f3rdoba, Laprida 854, X5000BGR, C\u00f3rdoba, Argentina e-mail: xramos@oac.unc.edu.ar 2 Niels Bohr International Academy, The Niels Bohr Institute, Blegdamsvej 17, 2100 Copenhagen \u00d8, Denmark Resumen En este trabajo\u00a0(2017A&A…602A.101R) presentamos…<\/p>","protected":false},"author":1,"featured_media":592,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[3],"tags":[],"class_list":["post-1726","post","type-post","status-publish","format-standard","has-post-thumbnail","hentry","category-novedades"],"_links":{"self":[{"href":"https:\/\/iate.oac.uncor.edu\/en\/wp-json\/wp\/v2\/posts\/1726","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/iate.oac.uncor.edu\/en\/wp-json\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/iate.oac.uncor.edu\/en\/wp-json\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/iate.oac.uncor.edu\/en\/wp-json\/wp\/v2\/users\/1"}],"replies":[{"embeddable":true,"href":"https:\/\/iate.oac.uncor.edu\/en\/wp-json\/wp\/v2\/comments?post=1726"}],"version-history":[{"count":0,"href":"https:\/\/iate.oac.uncor.edu\/en\/wp-json\/wp\/v2\/posts\/1726\/revisions"}],"wp:featuredmedia":[{"embeddable":true,"href":"https:\/\/iate.oac.uncor.edu\/en\/wp-json\/wp\/v2\/media\/592"}],"wp:attachment":[{"href":"https:\/\/iate.oac.uncor.edu\/en\/wp-json\/wp\/v2\/media?parent=1726"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/iate.oac.uncor.edu\/en\/wp-json\/wp\/v2\/categories?post=1726"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/iate.oac.uncor.edu\/en\/wp-json\/wp\/v2\/tags?post=1726"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}