Detalhes bibliográficos
| Ano de defesa: |
2018 |
| Autor(a) principal: |
Carolina Gribel de Vasconcelos Ferreira |
| Orientador(a): |
Oswaldo Duarte Miranda,
José Williams dos Santos Vilas Boas |
| Banca de defesa: |
Diego Antônio Falceta Gonçalves |
| Tipo de documento: |
Tese
|
| Tipo de acesso: |
Acesso aberto |
| Idioma: |
eng |
| Instituição de defesa: |
Instituto Nacional de Pesquisas Espaciais (INPE)
|
| Programa de Pós-Graduação: |
Programa de Pós-Graduação do INPE em Astrofísica
|
| Departamento: |
Não Informado pela instituição
|
| País: |
BR
|
| Link de acesso: |
http://urlib.net/sid.inpe.br/mtc-m21b/2018/02.05.17.02
|
Resumo: |
We present a model that unifies the cosmic star formation rate (CSFR), obtained through the hierarchical structure formation scenario, with the (Galactic) local star formation rate (SFR). It is possible to use the SFR to generate a CSFR mapping through the density probability distribution functions (PDFs) commonly used to study the role of turbulence in the star-forming regions of the Galaxy. We obtain a consistent mapping from redshift z 20 up to the present (z = 0). Our results show that the turbulence exhibits a dual character, providing high values for the star formation efficiency (h"i 0.32) in the redshift interval z 3.5−20 and reducing its value to h"i = 0.021 at z = 0. The value of the Mach number (Mcrit), from which h"i rapidly decreases, is dependent on both the polytropic index (􀀀) and the minimum density contrast of the gas. We also derive Larsons first law associated with the velocity dispersion (hVrmsi) in the local star formation regions. Our model shows good agreement with Larsons law in the 0.1 − 30pc range (when our model is compared to the observational data), providing typical temperatures T0 2−50K for the gas associated with star formation. As a consequence, dark matter halos of great mass could contain a number of halos of much smaller mass, and be able to form structures similar to globular clusters. Thus, Larsons law emerges as a result of the very formation of large-scale structures, which in turn would allow the formation of galactic systems, including our Galaxy. |
