Made available in DSpace on 2015-03-03T15:15:27Z (GMT). No. of bitstreams: 1 CaioFTC_DISSERT.pdf: 1416691 bytes, checksum: 65196f540a2e74d7cb641ab2966c1db0 (MD5) Previous issue date: 2011-08-12 / Coordena??o de Aperfei?oamento de Pessoal de N?vel Superior / In the present study we compute the atmospheric parameters (Teff , log g and vmic, [Fe/H]) and chemical abundance of 16 ions (Fe I, Fe II, O I, Si I, Na I, Mg I, Al I, Ca I, Ti I, Co I, Ni I, Rb I, Zr I, Ba II, La II and Cr I) for 16 solar-like stars with masses between 0:8 and 1:2 Mfi aproximatedly, including 10 planet-host stars detected by the CoRoT Space Mission. For this study, we use data from the ESO public archive: (i) high resolution spectra (R 47000) from the UVES spectrograph on the VLT/UT2-ESO (for 7 stars, covering the wavelength range 3450-4515 ? and 5500-9400 ?) and (ii) high resolution spectra from HARPS spectrograph on the La Silla-ESO 3.60 m telescope (for 9 stars, covering the wavelength range 4200-6865 ?). Our spectral analysis is based on MARCS models of atmosphere and Turbospectrum spectroscopic tools. On the base of the computed parameters, the referred abundances appears to follow the same behavior of the solar curve abundances. Further, one observes a signifficant correlation between the abundance ratio [m/Fe] and condensation temperature (Tc) of refractory elements (Tc > 900 K). The behavior of the projected rotational velocity (v sin i) versus the computed abundances [m/Fe] is also analyzed, presenting no clear trends. This study oers additional constraints to trace the evolutive history of solar-like stars with planets, including the search for chemical dierences between stars with and without transit planets and anomalies in the studied abundances / No presente estudo, n?s determinamos os par?metros atmosf?ricos (Teff , log g, vmic e [Fe/H]) e as abund?ncias qu?micas de 16 ?ons (Fe I, Fe II, O I, Si I, Na I, Mg I, Al I, Ca I, Ti I, Co I, Ni I, Rb I, Zr I, Ba II, La II e Cr I) para 16 estrelas solares, com massas entre 0:8 e 1:2 M , aproximadamente, incluindo 10 estrelas com planetas detectados pelo telesc?pio espacial CoRoT. Para este estudo, foram usados dados do arquivo p?blico do ESO: (i) espectros de alta resolu??o (R 47000) do espectr?grafo UVES localizado no VLT/UT2- ESO (para 7 estrelas, cobrindo o dom?nio espectral de 3450-4515 ? e 5500-9400 ?) e (ii) espectros de alta resolu??o obtidos com o espectr?grafo HARPS localizado no telesc?pio de 3,60 m, em La Silla-ESO (para 9 estrelas, cobrindo a faixa de 4200-6865 ?). Nossa an?lise espectral ? baseada nos modelos de atmosfera MARCS e nas ferramentas espectrosc?picas do Turbospectrum. Com base nos par?metros obtidos, as abund?ncias referidas parecem seguir tend?ncia semelhante ? curva de abund?ncias solares. Adicionalmente, observa-se uma correla??o signi cativa entre a abund?ncia relativa [m/H] e a temperatura de condensa??o (Tc) dos elementos refrat?rios (Tc > 900 K). O comportamento da velocidade rotacional projetada (v sin i) em fun??o das abund?ncias obtidas tamb?m ? analisada, n?o apresentando correla??es claras. Este estudo oferece v?nculos adicionais para o tra?ado da hist?ria evolutiva de estrelas solares com planetas, incluindo a busca por diferen?as qu?micas entre estrelas com e sem planetas em tr?nsito, e por anomalias nas abund?ncias estudadas