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Estrellas Evolucionadas Con Planetas: Abundancias Qu´Imicasy Propiedades Planetarias

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Estrellas Evolucionadas Con Planetas: Abundancias Qu´Imicasy Propiedades Planetarias Estrellas evolucionadas con planetas: abundancias qu´ımicasy propiedades planetarias por Jorge Emiliano Jofr´e Presentado ante la Facultad de Matem´atica,Astronom´ıay F´ısicacomo parte de los requerimientos para obtener el t´ıtulo de Doctor en Astronom´ıade la UNIVERSIDAD NACIONAL DE CORDOBA´ Marzo de 2015 c FaMAF - UNC - 2015 Director: Dr. Pablo J. D. Mauas Co-Directora: Dra. Mercedes G´omez ii Estrellas evolucionadas con planetas: abundancias qu´ımicasy propiedades planetarias por Jorge Emiliano Jofr´ese distribuye bajo una Licencia Creative Commons Atribu- ci´on-NoComercial-SinDerivadas 2.5 Argentina. A mis padres iv \... si quieres lanzar una caja al Sol, tienes que hacerlo t´umismo." {Hermes Conrad Futurama (temporada 5, capıtulo´ 10)0 0\The Farnsworth Parabox" (2003); creado por Matt Groening & David X. Cohen, escrito por Bill Odenkirk. vi vii ´Indice general Resumen XI Abstract XVII Introducci´on 1 1. Planetas extrasolares y estrellas hu´espedes 9 1.1. Definici´onde planetas y exoplanetas . .9 1.2. M´etodos de detecci´on. 11 1.2.1. Perturbaci´ondin´amicade la estrella: velocidad radial, astrometr´ıa y timing ............................... 13 M´etodo Doppler de velocidad radial . 13 Posici´onastrom´etrica. 16 Timing ............................... 18 1.2.2. Imagen directa . 19 1.2.3. Tr´ansitosplanetarios . 20 1.2.4. TTV: Transit Timing Variations ................. 22 1.2.5. Microlentes gravitacionales . 24 1.3. Propiedades de los planetas detectados por VR . 24 1.3.1. Frecuencia de planetas gigantes . 25 1.3.2. Distribuci´onde masa . 26 1.3.3. Distribuci´onde per´ıodo . 26 1.3.4. Relaci´onmasa-per´ıodo . 29 1.3.5. Excentricidades orbitales . 29 1.4. Propiedades de las estrellas hu´espedes . 32 1.4.1. Metalicidad de las estrellas hu´espedes . 32 Origen de la correlaci´onplaneta-metalidad . 34 1.5. Estrellas evolucionadas con planetas . 38 1.5.1. Subgigantes . 41 1.5.2. Gigantes . 42 1.5.3. Propiedades de los planetas alrededor de estrellas evolucionadas 44 Semieje mayor . 44 viii ´INDICE GENERAL Masa planetaria . 46 1.6. Formaci´on planetaria . 47 1.6.1. Modelo de acreci´onde n´ucleo . 47 1.6.2. Inestabilidad gravitacional . 49 1.7. Objetivos generales de esta tesis . 51 2. Muestra, observaciones y reducci´onde datos 53 2.1. Selecci´onde la muestra . 53 2.2. Observaciones y descripci´ondel instrumental . 55 2.2.1. HARPS . 56 2.2.2. SOPHIE . 56 2.2.3. FEROS . 57 2.2.4. ELODIE . 57 2.2.5. EBASIM . 58 2.3. Reducci´onde las observaciones . 58 2.3.1. Espectros EBASIM . 58 2.3.2. Espectros de bases de datos . 62 3. Par´ametrosestelares 65 3.1. Par´ametrosfotosf´ericosfundamentales . 65 3.1.1. Comparaci´oncon otros estudios . 68 3.2. Par´ametrosfotom´etricos y f´ısicos . 77 3.3. Componentes de velocidad espacial . 87 3.4. Rotaci´onestelar . 93 4. Metalicidad de las estrellas evolucionadas 97 4.1. Antecedentes y objetivos . 97 4.2. Distribuciones de Metalicidad . 98 4.2.1. Estrellas gigantes . 98 4.2.2. Estrellas subgigantes . 102 4.2.3. Gigantes vs. subgigantes . 102 4.3. [Fe/H] en funci´onde la Teff ........................ 105 4.4. Conclusiones . 107 5. Otros elementos 109 5.1. Introducci´on. 109 5.1.1. Objetivos . 112 5.2. Obtenci´onde las abundancias qu´ımicas . 112 5.2.1. Errores en las abundancias qu´ımicas . 129 5.2.2. Comparaci´oncon otros estudios . 129 5.3. Distribuciones de [X/H] . 132 5.4. Los cocientes [X/Fe] . 135 ´INDICE GENERAL ix 5.4.1. B´usquedade diferencias en el plano [X/Fe]{[Fe/H] . 139 5.5. Conclusiones . 144 6. Propiedades planetarias 149 6.1. Introducci´on. 149 6.1.1. Objetivos . 151 6.2. Par´ametrosplanetarios y abundancias qu´ımicas . 151 6.3. Sistemas multi-planeta y metalicidad estelar . 154 6.4. Distancia orbital . 155 6.5. Masa Planetaria . 159 6.6. Excentricidad orbital . 165 6.7. Conclusiones . 168 7. Litio 171 7.1. Introducci´on. 171 7.1.1. Estudios previos de abundancias de litio en estrellas con planetas 174 7.1.2. Objetivos del trabajo . 178 7.2. Muestra . 178 7.3. An´alisis:S´ıntesis espectral . 178 7.3.1. Correcciones NLTE . 186 7.3.2. An´alisisde errores . 187 7.4. Chequeos de consistencia . 188 7.4.1. Mediciones realizadas con distintos espectr´ografos . 188 7.4.2. Comparaci´oncon valores obtenidos por otros autores . 189 7.5. Resultados generales . 191 7.6. Discusi´on:litio en estrellas con y sin planetas . 196 7.6.1. Subgigantes . 196 A(Li) en funci´onde los par´ametrosestelares . 196 Distribuci´onde A(Li) en las subgigantes con y sin planetas . 199 7.6.2. Gigantes . 202 A(Li) en funci´onde los par´ametrosestelares . 202 Distribuci´onde A(Li) en las gigantes con y sin planetas . 204 7.7. A(Li) vs. par´ametrosplanetarios . 207 7.8. Conclusiones . 209 Conclusiones finales y perspectivas futuras 213 Ap´endices 221 A. Evoluci´onpost-secuencia principal 221 Bibliograf´ıa 231 x ´INDICE GENERAL ´Indice de Figuras 251 ´Indice de Tablas 261 Agradecimientos 265 xi Resumen Desde 1992 se ha confirmado la detecci´onde m´asde 1500 planetas extrasolares, marcando una revoluci´onen la astronom´ıamoderna. A partir del an´alisisuniforme de grandes muestras es posible estudiar la relaci´onentre los par´ametrosplanetarios y las caracter´ısticasde sus estrellas hu´espedes, lo que puede proveer informaci´onmuy importante para los modelos de formaci´ony evoluci´onplanetaria. Por ejemplo, actual- mente es un hecho casi indiscutido que las estrellas de secuencia principal que albergan planetas gigantes son, en promedio, m´asricas en metales que aqu´ellassin planetas detectados. Esto se conoce usualmente como la correlaci´onplaneta-metalicidad. Los relevamientos de b´usquedade planetas alrededor de estrellas evolucionadas per- miten estudiar la frecuencia de planetas alrededor de estrellas m´asmasivas. Los resul- tados de estos programas de b´usquedacombinados con aqu´ellosque buscan planetas en estrellas de masa baja, indican que la frecuencia de planetas aumenta con la masa estelar, sugiriendo que este par´ametrotambi´entiene un papel preponderante en la for- maci´onde planetas gigantes. De los casi 500 planetas detectados por velocidad radial hasta la fecha, aproximadamente 120 orbitan alrededor de estrellas evolucionadas (es- trellas subgigantes y gigantes). Esto ha permitido investigar tambi´ensi la correlaci´on planeta-metalicidad encontrada para las estrellas de secuencia principal se mantiene para aqu´ellasevolucionadas. Los pocos estudios que han analizado la metalicidad de las subgigantes coinciden en que se mantiene la tendencia encontrada en las estrellas de secuencia principal. Sin embargo, en el caso de las estrellas gigantes, los resulta- dos han sido m´asdispares o controvertidos. M´asa´un,el estudio de las abundancias qu´ımicasde otros elementos, adem´asdel hierro, y la exploraci´onde sus relaciones con las propiedades planetarias cuenta con varios antecedentes en estrellas de secuencia principal con planetas, pero se ha realizado s´oloocasionalmente en estrellas evolu- cionadas con planetas. Este tipo de estudio puede proveer informaci´onvaliosa acerca de los elementos que podr´ıantener un papel importante en el proceso de formaci´on planetaria. Adem´asde la bien establecida correlaci´onplaneta-metalicidad, se ha debatido otra posible correlaci´onentre la presencia de planetas y las propiedades de las estrellas hu´espedes. Varios estudios sugieren que las estrellas de secuencia principal que alber- xii RESUMEN gan planetas tienen una abundancia de litio significativamente menor en comparaci´on con aqu´ellassin planetas detectados. Sin embargo, este tipo de an´alisistiene pocos antecedentes en el caso de estrellas evolucionadas. As´ı,en este trabajo presentamos par´ametrosestelares fundamentales (temperatura efectiva, gravedad superficial, metalicidad y velocidad de microturbulencia), par´ame- tros f´ısicos(masa, edad, radio, luminosidad), velocidades de rotaci´onproyectada, veloci- dades radiales, componentes de velocidad espacial Gal´acticay abundancias qu´ımicas de 14 elementos para una muestra de 86 estrellas evolucionadas con planetas (56 gigantes y 30 subgigantes) y para una muestra de control de 137 estrellas sin planetas detecta- dos (101 gigantes y 36 subgigantes). La muestra de estrellas evolucionadas con planetas constituye una de las m´asgrandes analizadas de manera uniforme hasta el momento. El an´alisisse hizo a partir de espectros echelle de alta resoluci´ony relaci´onse~nal-ruido, tomados con los espectr´ografosHARPS, FEROS, SOPHIE, ELODIE y EBASIM. Los objetivos principales de la primera parte del trabajo consistieron en: I) investigar difer- encias qu´ımicasentre estrellas evolucionadas con y sin planetas detectados; II) explorar potenciales diferencias entre las propiedades de planetas alrededor de estrellas gigantes y subgigantes; y III) buscar posibles correlaciones entre las propiedades planetarias (f´ısicasy orbitales) y las abundancias qu´ımicas de sus estrellas hu´espedes. Los par´ametrosfundamentales se determinaron de manera homog´eneausando el programa FUNDPAR a partir de los anchos equivalentes de l´ıneasde hierro requiriendo equilibrio de ionizaci´ony excitaci´on,y la independencia entre las abundancias y los anchos equivalentes. Las abundancias qu´ımicasde 14 elementos (Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Zn y Ba) se obtuvieron a partir de la medici´onde anchos equivalentes de una serie de l´ıneas no solapadas, utilizando el c´odigoMOOG. Las velocidades rotacionales se computaron a partir de los anchos a mitad de profundidad de una serie de l´ıneasaisladas de hierro. En acuerdo con estudios previos, encontramos que las estrellas subgigantes con pla- netas son, en promedio, m´asricas en metales que aqu´ellassin planetas por ∼0.16 dex. Por el contrario, la distribuci´onde metalicidad de las estrellas gigantes con planetas est´acentrada en metalicidades ligeramente subsolares y no muestra un exceso respecto a la distribuci´onde metalicidad de las gigantes sin planetas.
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