Resultado da Pesquisa

10.1007/s40314-015-0270-z

DOI

ISSN

2238-3603

Código do Detentor

isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S

Chave de Citação

CarvalhoMorPraMouWin:2016:AnOrEv

Autor

1 Carvalho, J. P. S.
2 Moraes, R. V. de
3 Prado, Antonio Fernando Bertachini de Almeida
4 Mourão, D. C.
5 Winter, O. C.

Identificador de Curriculo

1
2
3 8JMKD3MGP5W/3C9JGJA

Grupo

1
2
3 DMC-ETE-INPE-MCTI-GOV-BR

Afiliação

1 Universidade Federal do Recôcavo da Bahia (UFRB)
2 Universidade Federal de São Paulo (UNIFESP)
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 Universidade Estadual Paulista (UNESP)
5 Universidade Estadual Paulista (UNESP)

Endereço de e-Mail do Autor

1
2
3 antonio.prado@inpe.br

Título

Analysis of the orbital evolution of exoplanets

Revista

Computational & Applied Mathematics

Ano

2016

Volume

Número

Mês

Oct.

Palavras-Chave

Astrodynamics, Planetary systems, Stellar dynamics, Exoplanets and third-body perturbation.

Resumo

An exoplanet, or extrasolar planet, is a planet that does not orbit the Sun, but is around a different star, stellar remnant, or brown dwarf. Up to now, about 1900 exoplanets were discovered. To better understand the dynamics of these exoplanets, a study with respect to possible collisions of the planet with the central star is shown here. We present an expanded model in a small parameter that takes into account up to the fifth order to analyze the effect of this potential in the orbital elements of the extrasolar planet. Numerical simulations were also performed using the N-body simulations, using the software Mercury, to compare the results with the ones obtained by the analytical model. The numerical simulations are presented in two stages: one considering the celestial bodies as point masses and the other one taking into account their dimensions. This analysis showed that the planet collided with the central star in the moment of the first inversion for orbits with high inclinations in various situations. The results of the simulations of the equations developed in this study are consistent with the N-body numerical simulations. We analyze also the flip of the inclination taking into account the coupling of the perturbations of the third body, effect due to the precession of periastron and the tide effect. In general, we find that such perturbations combined delay the time of first inversion, but do not keep the planet in a prograde or retrograde orbit.

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847-863

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journal article

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WEBSCI; PORTALCAPES; SCOPUS.

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2184 KiB

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Carvallho_Analysis.pdf

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Data de Acesso

19 out. 2020

Tipo da Referência

Journal Article

Identificador

8JMKD3MGP3W34P/3L59TC8

Repositório

sid.inpe.br/mtc-m21b/2016/02.05.15.37 (acesso restrito)

Metadados

sid.inpe.br/mtc-m21b/2016/02.05.15.37.25

Site

10.1007/s10569-015-9650-3

DOI

Rótulo

self-archiving-INPE-MCTI-GOV-BR

ISSN

0923-2958

Código do Detentor

isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S

Chave de Citação

CarvalhoMouMorPraWin:2016:SwPrRe

Autor

1 Carvalho, Jean P. S.
2 Mourão, D. C.
3 Moraes, Rodolpho Vilhena de
4 Prado, Antonio Fernando Bertachini de Almeida
5 Winter, O. C.

Identificador de Curriculo

1
2
3
4 8JMKD3MGP5W/3C9JGJA

Grupo

1
2
3
4 DMC-ETE-INPE-MCTI-GOV-BR

Afiliação

1 Universidade Federal do Recôcavo da Bahia (UFRB)
2 Universidade Estadual Paulista (UNESP)
3 Universidade Federal de São Paulo (UNIFESP)
4 Instituto Nacional de Pesquisas Espaciais (INPE)
5 Universidade Estadual Paulista (UNESP)

Endereço de e-Mail do Autor

1 jeanfeg@gmail.com
2 decmou@yahoo.com.br
3 rodolpho.vilhena@gmail.com
4 antonio.prado@inpe.br
5 ocwinter@gmail.com

Título

Exoplanets in binary star systems: on the switch from prograde to retrograde orbits

Revista

Celestial Mechanics & Dynamical Astronomy

Ano

2016

Volume

124

Número

Mês

Jan.

Palavras-Chave

Three-body problem, Orbital perturbation, Exoplanets, Flip of inclination, Lidov-Kozai mechanism.

Resumo

The eccentric Kozai-Lidov mechanism, based on the secular theory, has been proposed as a mechanism that plays an important role in producing orbits that switch from prograde to retrograde. In the present work we study the secular dynamics of a triple system composed of a Sun-like central star and a Jupiter-like planet, which are under the gravitational influence of another perturbing star (brown dwarf). The perturbation potential is developed in closed form up to the fifth order in a small parameter (), where is the semimajor axis of the extrasolar planet and is the semimajor axis of the perturbing star. To eliminate the short-period terms of the perturbation potential, the double-average method is applied. In this work we do not eliminate the nodes, a standard method in the literature, before deriving the equations of motion. The main goal is to study the effects of the higher-order terms of the expansion of the perturbing force due to the third body in the orbital evolution of the planet. In particular, we investigate the inclination and the shape (eccentricity) of these orbits. We show the importance of the higher-order terms in changing the inversion times of the flip, i.e., the times where the inclination of the inner planet flips from prograde to retrograde trajectories. We also show the dependence of the first flip with respect to the semimajor axis and eccentricity of the orbit of the planet. The general conclusion is that the analytical model increases its accuracy with the inclusion of higher-order terms. We also performed full numerical integrations using the Bulirsch-Stoer method available in the Mercury package for comparison with the analytical model. The results obtained with the equations developed in this work are in accordance with direct numerical simulations.

Páginas

73-96

Idioma

Tipo de Trabalho

journal article

Tipo Secundário

PRE PI

Divulgação

WEBSCI; PORTALCAPES; SCOPUS.

Area

ETES

Nota Secundária

A2_ENGENHARIAS_III B1_INTERDISCIPLINAR B1_ASTRONOMIA_/_FÍSICA B2_MATEMÁTICA_/_PROBABILIDADE_E_ESTATÍSTICA B3_ENSINO B3_CIÊNCIA_DA_COMPUTAÇÃO

Tamanho

4735 KiB

Número de Arquivos

Arquivo Alvo

carvalho.pdf

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2016:02.05.15.39.35 sid.inpe.br/mtc-m21b/2013/09.26.14.25.20 administrator

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Data de Acesso

19 out. 2020

Tipo da Referência

Journal Article

Identificador

8JMKD3MGP3W34P/3LFG2E8

Repositório

sid.inpe.br/mtc-m21b/2016/04.08.13.04 (acesso restrito)

Metadados

sid.inpe.br/mtc-m21b/2016/04.08.13.04.44

Site

10.1016/j.icarus.2016.02.043

DOI

ISSN

0019-1035

Código do Detentor

isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S

Chave de Citação

DeiennoGomWalMorNes:2016:GrTaMo

Autor

1 Deienno, Rogério
2 Gomes, R. S.
3 Walsh, K. J.
4 Morbidelli, A.
5 Nesvorný, D.

Grupo

1 DMC-ETE-INPE-MCTI-GOV-BR

Afiliação

1 Instituto Nacional de Pesquisas Espaciais (INPE)
2 Observatório Nacional (ON)
3 Southwest Space Research Institute
4 Université Côte d'Azur
5 Southwest Space Research Institute

Endereço de e-Mail do Autor

1 rogerio.deienno@inpe.br

Título

Is the Grand Tack model compatible with the orbital distribution of main belt asteroids?

Revista

Icarus

Ano

2016

Volume

272

Mês

July

Palavras-Chave

Asteroids, dynamics, Origin, Solar System, Planetary dynamics, Planets, migration.

Resumo

The Asteroid Belt is characterized by the radial mixing of bodies with different physical properties, a very low mass compared to Minimum Mass Solar Nebula expectations and has an excited orbital distribution, with eccentricities and inclinations covering the entire range of values allowed by the constraints of dynamical stability. Models of the evolution of the Asteroid Belt show that the origin of its structure is strongly linked to the process of terrestrial planet formation. The Grand Tack model presents a possible solution to the conundrum of reconciling the small mass of Mars with the properties of the Asteroid Belt, including the mass depletion, radial mixing and orbital excitation. However, while the inclination distribution produced in the Grand Tack model is in good agreement with the one observed, the eccentricity distribution is skewed towards values larger than those found today. Here, we evaluate the evolution of the orbital properties of the Asteroid Belt from the end of the Grand Tack model (at the end of the gas nebula phase when planets emerge from the dispersing gas disk), throughout the subsequent evolution of the Solar System including an instability of the Giant Planets approximately 400 Myr later. Before the instability, the terrestrial planets were modeled on dynamically cold orbits with Jupiter and Saturn locked in a 3:2 mean motion resonance. The model continues for an additional 4.1 Gyr after the giant planet instability. Our results show that the eccentricity distribution obtained in the Grand Tack model evolves towards one very similar to that currently observed, and the semimajor axis distribution does the same. The inclination distribution remains nearly unchanged with a slight preference for depletion at low inclination; this leads to the conclusion that the inclination distribution at the end of the Grand Tack is a bit over-excited. Also, we constrain the primordial eccentricities of Jupiter and Saturn, which have a major influence on the dynamical evolution of the Asteroid Belt and its final orbital structure.

Páginas

114-124

Idioma

Tipo de Trabalho

journal article

Tipo Secundário

PRE PI

Divulgação

WEBSCI; PORTALCAPES; SCOPUS.

Area

ETES

Nota Secundária

A1_GEOCIÊNCIAS A2_ASTRONOMIA_/_FÍSICA

Tamanho

2733 KiB

Número de Arquivos

Arquivo Alvo

Deienno_is the grand.pdf

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Data de Acesso

19 out. 2020

Tipo da Referência

Journal Article

Identificador

8JMKD3MGP3W34P/3MRK398

Repositório

sid.inpe.br/mtc-m21b/2016/11.22.19.40 (acesso restrito)

Metadados

sid.inpe.br/mtc-m21b/2016/11.22.19.40.29

Site

10.1007/s10569-016-9699-7

DOI

ISSN

0923-2958

Código do Detentor

isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S

Chave de Citação

DeiennoMergPradSmir:2016:SaDeVi

Autor

1 Deienno, Rogério
2 Merguizo Sanchez, Diogo
3 Prado, Antonio Fernando Bertachini de Almeida
4 Smirnov, Georgi

Identificador de Curriculo

1
2
3 8JMKD3MGP5W/3C9JGJA

Grupo

1 DMC-ETE-INPE-MCTI-GOV-BR
2 DMC-ETE-INPE-MCTI-GOV-BR
3 DMC-ETE-INPE-MCTI-GOV-BR

Afiliação

1 Instituto Nacional de Pesquisas Espaciais (INPE)
2 Instituto Nacional de Pesquisas Espaciais (INPE)
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 University of Minho

Endereço de e-Mail do Autor

1 rogerio.deienno@inpe.br
2 diogo.sanchez@inpe.br
3 antonio.prado@inpe.br

Título

Satellite de-orbiting via controlled solar radiation pressure

Revista

Celestial Mechanics and Dynamical Astronomy

Ano

2016

Volume

126

Número

Mês

Nov.

Palavras-Chave

Astrodynamics, Orbital maneuvers, Satellite de-orbiting, Solar radiation pressure.

Resumo

The goal of the present research was to study the use of solar radiation pressure to place a satellite in an orbit that makes it to re-enter the atmosphere of the Earth. This phase of the mission is usual, since the orbital space around the Earth is crowded and all satellites have to be discarded after the end of their lifetimes. The technique proposed here is based on a device that can increase and decrease the area-to-mass ratio of the satellite when it is intended to reduce its altitude until a re-entry point is reached. Equations that predict the evolution of the eccentricity and semi-major axis of the orbit of the satellite are derived and can be used to allow the evaluation of the time required for the decay of the satellite. Numerical simulations are made, and they show the time required for the decay as a function of the area-to-mass ratio and the evolution of the most important orbital elements. The results show maps that indicate regions of fast decays as a function of the area-to-mass ratio and the initial inclination of the orbit of the satellite. They also confirmed the applicability of the equations derived here. The numerical results showed the role played by the evection and the Sun-synchronous resonances in the de-orbiting time.

Páginas

433-459

Idioma

Tipo de Trabalho

journal article

Tipo Secundário

PRE PI

Divulgação

WEBSCI; PORTALCAPES.

Area

ETES

Nota Secundária

A2_ENGENHARIAS_III B1_INTERDISCIPLINAR B1_ASTRONOMIA_/_FÍSICA B2_MATEMÁTICA_/_PROBABILIDADE_E_ESTATÍSTICA B3_ENSINO B3_CIÊNCIA_DA_COMPUTAÇÃO

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1055 KiB

Número de Arquivos

Arquivo Alvo

Deienno_satellite.pdf

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Data de Acesso

19 out. 2020

Tipo da Referência

Journal Article

Identificador

8JMKD3MGP3W34P/3MPQHTP

Repositório

sid.inpe.br/mtc-m21b/2016/11.11.18.44 (acesso restrito)

Metadados

sid.inpe.br/mtc-m21b/2016/11.11.18.44.36

Site

10.1007/s40314-015-0264-x

DOI

Rótulo

self-archiving-INPE-MCTI-GOV-BR

ISSN

2238-3603

Código do Detentor

isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S

Chave de Citação

GomesOlivPradSanc:2016:ClApCl

Autor

1 Gomes, Vivian Martins
2 Oliveira, Geraldo M. C.
3 Prado, Antonio Fernando Bertachini de Almeida
4 Sanchez, Diogo Merguizo

Identificador de Curriculo

1
2
3 8JMKD3MGP5W/3C9JGJA

Grupo

1
2
3 DMC-ETE-INPE-MCTI-GOV-BR
4 CMC-ETES-SPG-INPE-MCTI-GOV-BR

Afiliação

1 Universidade Estadual Paulista (UNESP)
2 Centro Federal para Educação Tecnológica de Minas Gerais (CEFET-MG)
3 Instituto Nacional de Pesquisas Espaciais (INPE)
4 Instituto Nacional de Pesquisas Espaciais (INPE)

Endereço de e-Mail do Autor

1 vivianmartinsgomes@gmail.com
2
3 antonio.prado@inpe.br
4 diogo.sanchez@inpe.br

Título

Close approach of a cloud of particles around an oblate planet

Revista

Computational & Applied Mathematics

Ano

2016

Volume

Número

Mês

Oct.

Palavras-Chave

Astrodynamics, Close approaches, Orbital maneuver, Oblate planet.

Resumo

The goal of the present paper is to study close approaches of a cloud of particles with an oblate planet, which means that there is a term in the gravitational potential of the planet. This cloud of particles is assumed to be created during the passage of a spacecraft by the periapsis of its orbit, by an explosion or any other disruptive event. The system is formed by two large bodies (Sun and planet), assumed to be in circular orbits around the center of mass of the system, and the cloud of particles. The particles that belong to the cloud make a close approach to the flat planet and then they are dispersed by the gravitational force of the planet. The motion is governed by the equations of motion given by the planar restricted circular three-body problem plus the effects of the oblateness of the planet. Jupiter is used for numerical simulations. The results show the differences between the behavior of the cloud after the passage, considering or not the effects of the oblateness of the planet. The results show that the oblateness of the planet is equivalent to an increase in the mass of the planet.

Páginas

663-673

Idioma

Tipo de Trabalho

journal article

Tipo Secundário

PRE PI

Divulgação

WEBSCI; PORTALCAPES; SCOPUS.

Area

ETES

Tamanho

4442 KiB

Número de Arquivos

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gomes_close.pdf

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Data de Acesso

19 out. 2020