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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

Connecting the Cosmic Star Formation Rate with the Local Star Formation

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Autor(es):
Gribel, Carolina [1] ; Miranda, Oswaldo D. [1] ; Vilas-Boas, Jose Williams [1]
Número total de Autores: 3
Afiliação do(s) autor(es):
[1] INPE, Div Astrofis, Av Astronautas 1-758, Sao Jose Dos Campos, SP - Brazil
Número total de Afiliações: 1
Tipo de documento: Artigo Científico
Fonte: ASTROPHYSICAL JOURNAL; v. 849, n. 2 NOV 10 2017.
Citações Web of Science: 2
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 commonly used to study the role of turbulence in the star-forming regions of the Galaxy. We obtain a consistent mapping from redshift z similar to 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 (<epsilon > similar to 0.32) in the redshift interval z similar to 3.5-20 and reducing its value to <epsilon > = 0.021 at z = 0. The value of the Mach number (M-crit), from which <epsilon > rapidly decreases, is dependent on both the polytropic index (Gamma) and the minimum density contrast of the gas. We also derive Larson's first law associated with the velocity dispersion (< V-rms >) in the local star formation regions. Our model shows good agreement with Larson's law in the similar to 10-50 pc range, providing typical temperatures T-0 similar to 10-80 K 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, Larson's 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. (AU)

Processo FAPESP: 14/11156-4 - O que determina o crescimento da massa estelar de galáxias elípticas? Intrínseco ou ambiente: a saga contínua
Beneficiário:Reinaldo Ramos de Carvalho
Linha de fomento: Auxílio à Pesquisa - Temático