@MastersThesis{Santos:2014:SiNu,
author = "Santos, Luiz Henrique Guimar{\~a}es dos",
title = "Estudo da intera{\c{c}}{\~a}o entre o disco protoplanet{\'a}rio
e os planetas: simula{\c{c}}{\~o}es num{\'e}ricas",
school = "Instituto Nacional de Pesquisas Espaciais (INPE)",
year = "2014",
address = "S{\~a}o Jos{\'e} dos Campos",
month = "2014-04-15",
keywords = "exoplanetas, simula{\c{c}}{\~o}es num{\'e}ricas, disco
protoplanet{\'a}rio, forma{\c{c}}{\~a}o planet{\'a}ria,
exoplanets, numerical simulations, protoplanetary disk, planetary
formation.",
abstract = "Entender a intera{\c{c}}{\~a}o de planetas ainda embebidos no
disco protoplanet{\'a}rio {\'e} crucial para conhecermos o
processo de forma{\c{c}}{\~a}o de planetas, inclusive do Sistema
Solar. Para tanto precisamos compreender as
caracter{\'{\i}}sticas dos exoplanetas descobertos nas
{\'u}ltimas duas d{\'e}cadas, seus m{\'e}todos de
detec{\c{c}}{\~a}o e a estat{\'{\i}}stica destes planetas.
Este trabalho apresenta um estudo te{\'o}rico mais aprofundado
sobre as caracter{\'{\i}}sticas do disco protoplanet{\'a}rio e
os torques que surgem sobre o planeta em sua intera{\c{c}}{\~a}o
com o disco e os consequentes tipos de migra{\c{c}}{\~a}o
orbital que podem ocorrer. Para verificar a teoria, realizamos
simula{\c{c}}{\~o}es num{\'e}ricas utilizando o c{\'o}digo
hidrodin{\^a}mico FARGO. Foram feitas seis s{\'e}ries de
simula{\c{c}}{\~o}es com planetas de quatro massas distintas
(tipo Terra, Super-Terra, Netuno e J{\'u}piter) inseridos no
disco gasoso e com diferentes configura{\c{c}}{\~o}es de
inicializa{\c{c}}{\~a}o. Buscando observar as
caracter{\'{\i}}sticas f{\'{\i}}sicas da intera{\c{c}}{\~a}o
disco-planeta estimamos a velocidade de migra{\c{c}}{\~a}o para
diferentes perfis radiais de densidade superficial do disco. Como
resultado marcante destas simula{\c{c}}{\~o}es encontramos a
r{\'a}pida taxa de varia{\c{c}}{\~a}o radial dos planetas e uma
massa limite na forma{\c{c}}{\~a}o dentro do disco, equivalente
a aproximadamente 10 M\$_{Jup}\$, ap{\'o}s o qual o planeta cai
rapidamente sobre sua estrela hospedeira. Al{\'e}m disto, para
aumentar o tempo de exist{\^e}ncia do planeta dentro do disco,
analisamos o comportamento da migra{\c{c}}{\~a}o na
presen{\c{c}}a de saltos no perfil radial de densidade
superficial do disco, verificando o seu travamento e um
cen{\'a}rio que possibilitaria ao planeta se formar antes da
dissipa{\c{c}}{\~a}o total do disco de acres{\c{c}}{\~a}o.
Considerando os resultados das simula{\c{c}}{\~o}es e suas
limita{\c{c}}{\~o}es, discutimos os poss{\'{\i}}veis
cen{\'a}rios finais de sistemas planet{\'a}rios. Verificamos a
possibilidade de um planeta gigante estimular o aparecimento
destes saltos radiais de densidade e que a varia{\c{c}}{\~a}o
radial da borda deste salto levaria o planeta em seus limites,
podendo definir a sua {\'o}rbita final. ABSTRACT: To understand
the interaction of planets still embedded in protoplanetary disks
is crucial to the process of planet formation, including that of
our own Solar System. For this purpose, we need to know the
characteristics of exoplanets discovered in the last two decades,
their detection methods, and statistics of these planets. This
work presents a theoretical study more depth on the
characteristics of the protoplanetary disk is needed as well as
that of the torques that act on the planet in their interaction,
and the resulting types of orbital migration that can occur. To
verify the theory, we performed numerical simulations using the
hydrodynamic code FARGO. Six series of simulations with planets of
four different masses (Earth, Super-Earth, Neptune, and Jupiter
types) embedded in a gaseous disk were done with different initial
setups. A study of the physical characteristics of disc-planet
interaction was made by estimating the migration velocity for
different radial profiles of the disk surface density. As a result
of these simulations we find the rapid rate of radial variation of
planets and a mass limit the formation within the disk, equivalent
to approximately 10 M\$_{Jup}\$, after which the planet falls
quickly on its host star. Furthermore, to increase the lifetime of
the planet within the disk, anaIyzed the migration behavior in the
presence of jumps in the radial density profile surface of the
disk, checking your lock and a scenario that would allow the
planet is formed before the complete dissipation of the accretion
disk. Considering the simulation results and its limitations, we
discussed the possible final scenarios of planetary systems. We
checked the possibility of a giant planet stimulate the appearance
of these jumps radial density and radial variation of the edge of
this planet would jump at their Iimits and can define its final
orbit.",
committee = "Jablonski, Francisco Jos{\'e} (presidente) and Valio, Adriana
Benetti Marques (orientadora) and Winter, Othon Cabo and Martioli,
{\'E}der",
englishtitle = "Study of the interaction between the protoplanetary disk and the
planets: numerical simulations",
language = "pt",
ibi = "8JMKD3MGP5W34M/3GF4HGP",
url = "http://urlib.net/ibi/8JMKD3MGP5W34M/3GF4HGP",
targetfile = "publicacao.pdf",
urlaccessdate = "04 maio 2024"
}