| Grant number: | 14/10326-3 |
| Support Opportunities: | Scholarships in Brazil - Doctorate |
| Start date: | September 01, 2014 |
| End date: | July 31, 2018 |
| Field of knowledge: | Physical Sciences and Mathematics - Astronomy - Stellar Astrophysics |
| Agreement: | Coordination of Improvement of Higher Education Personnel (CAPES) |
| Principal Investigator: | Marcos Perez Diaz |
| Grantee: | Larissa Takeda |
| Host Institution: | Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG). Universidade de São Paulo (USP). São Paulo , SP, Brazil |
Abstract The project consists in the study of neon novae and in the development of photoionization modeling tools. The "neon novae" are peculiar novae, with overabundance of neon due to the presence of a rare ONeMg white dwarf. These novae represent less than 10% of the total observed novae population. The current identification of neon novae is subject to large errors of calculation and modeling, which induce errors of up to 1 dex in the neon abundance estimates. Neither the characteristics of the ONeMg white dwarfs, and their evolution, are well known in the scenario of high mass white dwarfs formation in binary systems. The properties of novae with ONeMg white dwarfs are directly related to the evolution of the binary system and to the detonation conditions near the Chandrasekhar limit. The first stage of the project consists in the observation of spatially resolved envelopes of these novae with IFU spectroscopy, which will provide data cubes with information of the spatial distribution of luminosity in different spectral lines. The observations will be performed with the VIMOS instrument (ESO-VLT), and/or with GMOS (Gemini). A second stage of the project will consist in the development of codes to execute the deprojection of the intensity distributions of the observed data, in order to accomplish a 3D mapping. The resultant structure will be modeled using the RAINY3D photoionization code to provide detailed information about the shell. Therefore, it will be possible to determine with accuracy the abundances, ejected mass in the eruption and the properties of the envelopes, characterizing the class of neon novae in the sense of nucleosynthesis and of its role on the binaries evolution. (AU) | |
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