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Análise Da Composiç˜Ao Qu´Imica Das Gêmeas Solares HIP 100963, HD

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Análise Da Composiç˜Ao Qu´Imica Das Gêmeas Solares HIP 100963, HD Universidade de S~aoPaulo Instituto de Astronomia, Geof´ısicae Ci^enciasAtmosf´ericas Departamento de Astronomia Jhon Yana Galarza An´alise da composi¸c~aoqu´ımicadas g^emeas solares HIP 100963, HD 45184 e a descoberta da g^emeasolar Inti 1 S~aoPaulo 2016 Jhon Yana Galarza An´alise da composi¸c~aoqu´ımicadas g^emeas solares HIP 100963, HD 45184 e a descoberta da g^emeasolar Inti 1 Disserta¸c~aoapresentada ao Departamento de Astronomia do Instituto de Astronomia, Geof´ısica e Ci^enciasAtmosf´ericasda Universidade de S~aoPaulo como requisito parcial para a ob- ten¸c~aodo t´ıtulode Mestre em Ci^encias. Vers~aoCorrigida. O original encontra- se dispon´ıvel na Unidade Area´ de Concentra¸c~ao:Astronomia Orientador: Prof. Dr. Jorge Mel´endez S~aoPaulo 2016 Dedico este trabalho `aminha professora, orientadora e amiga Mar´ıaLuisa Aguilar Hurtado, quem foi a primeira astro^noma do Peru. Agradecimentos A` minha querida fam´ılia: Aurelio Yana, Ines Galarza e Luis Yana Galarza, pelo seu apoio, assist^enciae carinho ao longo dos anos sem os quais a realiza¸c~aodesta disserta¸c~ao teria sido imposs´ıvel. A` minha noiva Cecilia Toledo, pela companhia de todos os dias, pelo apoio nos momen- tos mais dif´ıceise tamb´empelos bons momentos que ajudaram ao sucesso deste trabalho. Ao meu orientador Dr. Jorge Mel´endez,pela orienta¸c~ao,paci^encia,prestatividade e as in´umerasoportunidades que me deu, permitindo a minha forma¸c~aocient´ıfica. Aos meus colegas do grupo SAMPA: Leonardo dos Santos, Mar´ıliaCarlos, Henrique Reggiani, Lorenzo Spina e Marcelo Tucci, pelas importantes discuss~oesastrof´ısicasque contribu´ıramao desenvolvimento desta disserta¸c~ao. Ao meu colega de sala Rafael Campos, pela ajuda nas corre¸c~oesdeste trabalho. Tamb´em aos meus colegas do IAG por propiciarem um ambiente instigante `apesquisa. Aos professores cuja ajuda foi indispens´avel para enriquecer meus conhecimentos. Agrade¸co em especial `aDra. Silvia Rossi pela prestatividade. A` CNPq pela concess~aoda bolsa de mestrado. Esta tese/disserta¸c~aofoi escrita em LATEX com a classe IAGTESE, para teses e disserta¸c~oesdo IAG. \O universo n~aofoi feito `amedida do ser humano, mas tampouco lhe ´eadverso: ´e-lhe indiferente." Carl Sagan \Ser jovem e n~aoser revolucion´ario´euma contradi¸c~aogen´etica." Ernesto Guevara de la Serna, o "Che Guevara" Resumo O objetivo deste trabalho ´erealizar uma an´alisediferencial detalhada linha a linha para verificar se 2MASS J23263267-0239363 (nomeada de Inti 1) ´euma g^emeasolar. Tamb´em investigar a origem do padr~aode abund^anciasde HIP 100963, a correla¸c~aode l´ıtioe idade, os elementos vol´ateis e refrat´arios, e os elementos pesados atrav´esdos processos -s e -r. Os espectros das estrelas Inti 1, HD 45184, HIP 100963 e o Sol (empregando luz refle- tida nos asteroides Vesta e Iris) foram obtidos usando o espectr´ografoHIRES do telesc´opio Keck I, atingindo uma alta resolu¸c~ao e raz~aode sinal-ruido. Medi manualmente as lar- guras equivalentes (EWs) das linhas do ferro para determinar os par^ametrosatmosf´ericos atrav´esdo equil´ıbrioespectrosc´opico diferencial. A temperatura efetiva e a gravidade su- perficial tamb´emforam obtidas empregando calibra¸c~oesfotom´etricase usando o m´etodo trigonom´etrico.Determinei a composi¸c~aoqu´ımicados elementos vol´ateis,refrat´ariose de captura de n^eutrons.Desenvolvi o c´odigo terra para reproduzir os padr~oesde abund^ancias observados em HD 45184 e Inti 1. As idades foram obtidas usando is´ocronas(usando q2), a rela¸c~ao[Y/Mg], e atividade estelar (apenas para HIP 100963). Conclui que a estrela Inti 1 ´euma g^emea solar fraca e tem um padr~aode abund^ancias similar ao do Sol. HD 45184 mostra um padr~aosimilar `asg^emeassolares pr´oximas,isto ´e,ricas em elementos refrat´ariosem rela¸c~aoaos vol´ateis.Confirmou-se que HIP 100963 ´e uma g^emeasolar e demonstrei que seu padr~aode abund^ancias´esolar depois de corrigir por GCE; isto poderia significar que HIP 100963 e Inti 1 poderiam ter formado planetas rochosos. HIP 100963 mostra enriquecimento de elementos dos processos -s e -r, sugerindo que os elementos de captura de n^eutronss~aoricos em estrelas jovens. Da mesma forma que com outras g^emeassolares, HIP 100963 apresenta uma deple¸c~aode l´ıtioque ´ecausada pela evolu¸c~aoestelar, e sua abund^anciade l´ıtiosegue a correla¸c~aol´ıtioe idade. Abstract The aim of this work is to perform a detailed line-by-line differential analysis to verify whether 2MASS J23263267-0239363 (designated as Inti 1) is indeed a solar twin. I also investigate the origin of the abundance pattern of HIP 100963, the Li-age correlation, the volatile and refractory elements, and the heavy elements from the s- and r-processes. The spectra of the stars Inti 1, HD 45184, HIP 100963 and the Sun (using reflected light from the asteroids Vesta and Iris) were obtained employing the HIRES spectrograph on the Keck I telescope, reaching a high-resolution and high signal-to-noise ratio. I measu- red by hand the equivalent widths (EWs) of iron lines to determine the stellar parameters through the differential spectroscopic equilibrium. The effective temperature and surface gravity were also obtained by using photometric calibrations and through the trigonome- tric technique. I determined the composition of volatile, refractory, and neutron-capture elements. I developed the code terra to reproduce the abundance patterns observed in HD 45184 and Inti 1. The age and mass were obtained using isochrones (using q2), the [Y/Mg] ratio, and stellar activity (only for HIP 100963). I conclude that the star Inti 1 is a faint solar twin and has an abundance pattern similar to the Sun. HD 45184 shows an pattern similar to nearby solar twins, meaning enhanced in refractory relative to volatile elements. I confirmed that HIP 100963 is a solar twin and demonstrate that its abundance pattern is about solar after corrections for GCE; this could mean that HIP 10063 and Inti 1 may have formed rocky planets. HIP 100963 present enrichment in s- and r-process elements, suggesting that neutron capture elements are enhanced in young stars. Like in other solar twins, HIP 100963 shows a depletion in lithium that is caused by stellar evolution, and its lithium abundance follows the Li-age correlation. Lista de Figuras 1.1 Amostra das 88 g^emeassolares de Ram´ırezet al. (2014) em fun¸c~aoda tem- peratura efetiva. A linha pontilhada representa `atemperatura solar. 30 1.2 Diferen¸cas∆[X/Fe] (Sol - <g^emeassolares>) entre a composi¸c~aoqu´ımica do Sol e g^emeassolares vs. n´umeroat^omico(painel esquerdo) e temperatura de condensa¸c~ao(painel direito) (Mel´endez et al., 2009). 32 1.3 Painel esquerdo: a m´ediado padr~aode abund^anciasde 22 g^emeassolares em fun¸c~aoda temperatura de condensa¸c~ao.Painel direito: a inclina¸c~ao da m´ediado padr~aode abund^ancias dos elementos refrat´ariose a m´ediadas abund^anciasdos elementos vol´ateisem fun¸c~aodos par^ametrosatmosf´ericos. Cr´editosdas imagens: Ram´ırezet al. (2009). 33 1.4 A m´ediado padr~aode abund^anciasqu´ımicasdas amostras estudadas por Ram´ırezet al. (2010). Notar que nesta figura s~aomostrados apenas os tra- balhos onde os par^ametrosestelares foram determinados usando os espectros (equil´ıbrioespectrosc´opico). 33 1.5 Diferen¸casem abund^ancias qu´ımicasno Sol, observadas em latitudes altas e no equador solar. Fonte: Kiselman et al. (2011). 34 1.6 Diferen¸casentre as abund^anciasdo Sol obtidas com o asteroide Juno e Ceres (painel esquerdo), como tamb´emde Ceres e Vesta (painel direito). Cr´editos das imagem: Mel´endezet al. (2012) e Bedell et al. (2014). 36 1.7 Raz~aode abund^anciasentre a m´ediadas g^emeassolares em rela¸c~aoao Sol (linha vermelha) e as abund^anciasdo Sistema Solar polu´ıdas por estrelas AGB, supernovas e hipernovas. Cr´editosda imagem: Mel´endezet al. (2012). 37 1.8 Diferen¸caentre as abund^anciasqu´ımicasde 16 Cyg A e 16 Cyg B. A linha pontilhada ´ea m´ediados elementos vol´ateise a linha s´olida´eo padr~aodos elementos refrat´arios.A linha vermelha tracejada e pontilhada ´ea m´ediado padr~aode abund^anciasdas g^emeassolares. Fonte: Tucci Maia et al. (2014). 38 1.9 Imagem da estrela jovem TW Hydrae e seu disco protoplanet´ariorealizado pelo ALMA. Os espa¸cosvazios indicam que existe forma¸c~aoplanet´ariano sistema. Fonte: ESO e Andrews et al. (2016). 40 1.10 Distribui¸c~aode temperaturas na nebulosa solar. Fonte: Freedman e Kauf- mann (2005). 41 1.11 As abund^anciaselementais da fotosfera solar (Asplund et al., 2009) vs. a composi¸c~aoqu´ımicados condritos CI (Lodders et al., 2009). 42 1.12 Abund^ancia dos primeiros 41 elementos qu´ımicos presentes na fotosfera solar (Asplund et al., 2009). 43 1.13 Composi¸c~aoda fotosfera solar adicionando 4 massas terrestres de material tipo terra (painel superior), de tipo condr´ıticoCM (painel do meio) e uma mistura de material terrestre e condr´ıtico(painel inferior). A linha repre- senta o ajuste das 11 g^emeassolares analisadas por Mel´endezet al. (2009). Imagem tirada de Chambers (2010). 44 2.1 Abund^anciasdiferenciais da g^emeasolar HIP 100963 estimadas usando os modelos de atmosfera de Castelli e Kurucz (2004) e de Gustafsson et al. (2008), em fun¸c~aodo n´umeroat^omico(Z). 51 2.2 Esquema ilustrativo da defini¸c~aode largura equivalente. Imagem tirada e modificada de Rutten (2003). 53 2.3 Ilustra¸c~aogr´aficade uma curva de crescimento mostrando seus tr^esregimes (linha fraca, saturada e forte).
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