| 1. Identificação | ||||
| Tipo de Referência | Artigo em Revista Científica (Journal Article) | |||
| Site | mtc-m21b.sid.inpe.br | |||
| Código do Detentor | isadg {BR SPINPE} ibi 8JMKD3MGPCW/3DT298S | |||
| Identificador | 8JMKD3MGP3W34P/3LFG2E8 | |||
| Repositório | sid.inpe.br/mtc-m21b/2016/04.08.13.04 (acesso restrito) | |||
| Última Atualização | 2016:04.08.13.06.17 (UTC) administrator | |||
| Repositório de Metadados | sid.inpe.br/mtc-m21b/2016/04.08.13.04.44 | |||
| Última Atualização dos Metadados | 2021:02.11.18.12.33 (UTC) administrator | |||
| DOI | 10.1016/j.icarus.2016.02.043 | |||
| ISSN | 0019-1035 | |||
| Chave de Citação | DeiennoGomWalMorNes:2016:GrTaMo | |||
| Título | Is the Grand Tack model compatible with the orbital distribution of main belt asteroids?  | |||
| Ano | 2016 | |||
| Mês | July | |||
| Data de Acesso | 08 maio 2024 | |||
| Tipo de Trabalho | journal article | |||
| Tipo Secundário | PRE PI | |||
| Número de Arquivos | 1 | |||
| Tamanho | 2733 KiB | |||
| 2. Contextualização | ||||
| 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 | |||
| Revista | Icarus | |||
| Volume | 272 | |||
| Páginas | 114-124 | |||
| Nota Secundária | A1_GEOCIÊNCIAS A2_ASTRONOMIA_/_FÍSICA | |||
| Histórico (UTC) | 2016-04-08 13:04:44 :: simone -> administrator :: 2021-02-11 18:12:33 :: administrator -> simone :: 2016 | |||
| 3. Conteúdo e estrutura | ||||
| É a matriz ou uma cópia? | é a matriz | |||
| Estágio do Conteúdo | concluido | |||
| Transferível | 1 | |||
| Tipo do Conteúdo | External Contribution | |||
| Tipo de Versão | publisher | |||
| 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. | |||
| Área | ETES | |||
| Arranjo | urlib.net > BDMCI > Fonds > Produção anterior à 2021 > DIDMC > Is the Grand... | |||
| Conteúdo da Pasta doc | acessar | |||
| Conteúdo da Pasta source | não têm arquivos | |||
| Conteúdo da Pasta agreement |
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| 4. Condições de acesso e uso | ||||
| Idioma | en | |||
| Arquivo Alvo | Deienno_is the grand.pdf | |||
| Grupo de Usuários | simone | |||
| Grupo de Leitores | administrator simone | |||
| Visibilidade | shown | |||
| Política de Arquivamento | denypublisher denyfinaldraft24 | |||
| Permissão de Leitura | deny from all and allow from 150.163 | |||
| Permissão de Atualização | não transferida | |||
| 5. Fontes relacionadas | ||||
| Repositório Espelho | urlib.net/www/2011/03.29.20.55 | |||
| Unidades Imediatamente Superiores | 8JMKD3MGPCW/446AF4B | |||
| Lista de Itens Citando | sid.inpe.br/bibdigital/2021/02.11.18.06 6 | |||
| Divulgação | WEBSCI; PORTALCAPES; SCOPUS. | |||
| Acervo Hospedeiro | sid.inpe.br/mtc-m21b/2013/09.26.14.25.20 | |||
| 6. Notas | ||||
| Campos Vazios | alternatejournal archivist callnumber copyholder copyright creatorhistory descriptionlevel e-mailaddress format isbn label lineage mark nextedition notes number orcid parameterlist parentrepositories previousedition previouslowerunit progress project resumeid rightsholder schedulinginformation secondarydate secondarykey session shorttitle sponsor subject tertiarymark tertiarytype url | |||
| 7. Controle da descrição | ||||
| e-Mail (login) | simone | |||
| atualizar | ||||