|Support type:||Scholarships in Brazil - Post-Doctorate|
|Effective date (Start):||January 01, 2011|
|Effective date (End):||December 31, 2012|
|Field of knowledge:||Physical Sciences and Mathematics - Astronomy - Stellar Astrophysics|
|Principal researcher:||Marcos Perez Diaz|
|Grantee:||Manoel Carlos Vieira de Moraes Junior|
|Home Institution:||Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG). Universidade de São Paulo (USP). São Paulo , SP, Brazil|
Novae stars emerge from the ejection of matter due to a thermonuclear detonation on the surface of a white dwarf that accrets hydrogen rich matter from its companion. The material is ejected at high speeds and is ionized by the remanescent of the eruption that radiates mainly in ultra-violet spectrum. The radiation from these shells can be observed as emission lines in optical and infra-red wavelengths. The photoionization models of these ejected shells can bring new information on the temperature and luminosity of the central source. Furthermore, it may provide links to the models of eruption and enrichment in CNO that occurs in these systems. The current models with a homogeneous distribution of matter and spherical symmetry fail to reproduce the characteristics of the observed spectrum. Three dimensions shell models require observational spatially resolved data in order to reduce the degeneracy of the solutions. Observations with spatially resolved spectra, using integral field spectrographs are ideal for providing the constrains to 3D models. This project proposes to obtain three-dimensional models for the nova remnants of V842 Cen and RS Oph. Both were observed in by GMOS-IFU in 2010A by Gemini South telescope. The data will be processed using the tools developed in the work of HR Del (the PhD) and the results will be applied to 3D models using the RAINY3D code, which has also developed and operational. The data and models can answer questions not yet answered about the nova phenomenon, the evolution of binary and type Ia supernovae progenitors.