@MastersThesis{Oliveira:2016:CaSiTr,
author = "Oliveira, Aysses do Carmo",
title = "Caracteriza{\c{c}}{\~a}o de um sistema triplo eclipsante entre
as vari{\'a}veis do levantamento OGLE",
school = "Instituto Nacional de Pesquisas Espaciais (INPE)",
year = "2016",
address = "S{\~a}o Jos{\'e} dos Campos",
month = "2016-05-18",
keywords = "sistemas triplos, sistemas triplos eclipsante, bin{\'a}rias
eclipsantes, caracteriza{\c{c}}{\~a}o, triple systems, triple
eclipsing systems, eclipsing binary, characterization.",
abstract = "Este trabalho apresenta um estudo detalhado de um candidato a
sistema triplo eclipsante descoberto entre as vari{\'a}veis do
levantamento OGLE (Optical Gravitational Lensing Experiment). O
sistema eclipsante BUL-SC33 4277 tem caracter{\'{\i}}sticas de
uma bin{\'a}ria separada, com eclipses de 0,3 mag de profundidade
na banda I\$_{c}\$, recorrentes a cada 3,355 dias. Sobrepostos a
essa curva de luz ocorrem eclipses de 0,06 mag de profundidade,
com per{\'{\i}}odo de 0,517 dias. O mesmo comportamento aparece
nos dados do levantamento MACHO. Fotometria e espectroscopia
obtidas no Observat{\'o}rio do Pico dos Dias (OPD/LNA) tanto no
vis{\'{\i}}vel quanto no infravermelho pr{\'o}ximo, imagens no
infravermelho obtidas no telesc{\'o}pio SOAR e um conjunto de
medidas fotom{\'e}tricas na banca K\$_{s}\$ do VVV,
complementam o conjunto de dados utilizado. As
observa{\c{c}}{\~o}es espectrosc{\'o}picas foram utilizadas
para definir o tipo espectral do sistema e restringir sua
temperatura efetiva. A fotometria nas bandas B, V, R\$_{c}\$,
I\$_{c}\$, J, H, e K\$_{s}\$ permitem determinar a
distribui{\c{c}}{\~a}o espectral de energia, que junto com as
medidas fotom{\'e}tricas, estabelece o avermelhamento
interestelar do objeto. As curvas de luz, tanto da bin{\'a}ria
separada quanto da configura{\c{c}}{\~a}o com o objeto de baixa
massa foram modeladas com o c{\'o}digo Wilson-Devinney que
fornece uma estimativa das temperaturas, potenciais, raz{\~a}o de
massas e inclina{\c{c}}{\~a}o orbital. A bin{\'a}ria de 3,355
dias consiste de dois objetos da sequ{\^e}ncia principal cujo
tipo espectral combinado {\'e} F8, com massas e dimens{\~o}es
bem pr{\'o}ximas {\`a}s de uma estrela de 1 M\$\odot\$ . A
inclina{\c{c}}{\~a}o orbital {\'e} 84,53\$^{o}\$. O objeto de
baixa massa possui uma raz{\~a}o de massas de apenas 0,03, o que
implica massa tenha de cerca de 30 M\$_{4}\$. H{\'a}
evid{\^e}ncias de que o per{\'{\i}}odo orbital da bin{\'a}rias
AC possa ser vari{\'a}vel. As caracter{\'{\i}}sticas de
BUL-SC33 4277 tornam-o um sistema ideal para o estudo
din{\^a}mico de sistemas triplos. ABSTRACT: This work presents a
detailed study of a candidate to be a triple stellar system where
all components show eclipses. The system, called BUL-SC33 4277,
was found among the variable or candidates to variable stars from
the OGLE (Optical Gravitational Lensing Experiment) survey.
BUL-SC33 4277 as characteristics of a wide binary, with eclipses
0.3 mag deep in the l\$_{c}\$ band recurring at a 3.355 d
period. Superimposed to this light curve there are eclipses 0.06
mag deep which recur at a 0.517 d period. Both eclipses are also
seen in the MACHO survey in the B and R bands. Photometric and
spectroscopic data were collected at Observat{\'o}rio do Pico dos
Dias (OPD/LNA) in the visible and infrared. Imaging from the SOAR
telescope in the infrared and data from the VVV in the K\$_{s}\$
band complement our data. The spectroscopic data aim to define the
spectral type of the system and to constraint the effective
temperature of the components. Photometry in the B, V,
R\$_{c}\$, I\$_{c}\$ a, J, H, e K\$_{s}\$ bands allows us to
explore the spectral energy distribution on a wide range of
wavelengths. Together with characteristics of the spectral lines
present in the spectrum it is useful to estimate the interstellar
reddening in the line-of-sight to this object. The light curves,
both of the wide binary and of the configuration involving a low
mass object were modeled with the Wilson-Devinney code, providing
us with an estimate of the temperatures, gravitational potentials,
mass ratios and inclination. The 3.355 d binary consists of two
objects in the main sequence, with combined spectral type F8 and
masses and radii similar to those of a 1 M\$\odot\$ star. The
orbital inclination is 84.53\$^{o}\$. The low mass object has a
mass ratio of only \$\sim\$0.03, implying a mass of
\$\sim\$30 M\$_{4}\$. There are evidences that the orbital
period of the AC binary is changing with time. The characteristics
of BUL-SC33 4277 make it ideal for future studies of the dynamic
and radiative interactions in triple systems.",
committee = "Rodrigues, Cl{\'a}udia Vilega (presidente) and Jablonski,
Francisco Jos{\'e} (orientador) and D'Amico, Flavio and Almeida,
Leonardo Andrade de",
copyholder = "SID/SCD",
englishtitle = "Characterization of a triple eclipsing system among the variables
of the OGLE survey",
language = "pt",
pages = "105",
ibi = "8JMKD3MGP3W34P/3LKU5B2",
url = "http://urlib.net/ibi/8JMKD3MGP3W34P/3LKU5B2",
targetfile = "publicacao.pdf",
urlaccessdate = "27 abr. 2024"
}