The accretion flow onto white dwarfs and its X-ray emission properties /
- Autores: Nataly Ospina Escobar
- Directores de la Tesis: Margarida Hernanz Carbó (dir. tes.), Javier Rodríguez Viejo (tut. tes.)
- Lectura: En la Universitat Autònoma de Barcelona ( España ) en 2017
- Idioma: español
- Tribunal Calificador de la Tesis: Domitilla De Martino (presid.), Glòria Sala Cladellas (secret.), Pablo Rodríguez Gil (voc.)
- Programa de doctorado: Programa Oficial de Doctorado en Física
- Materias:
- Enlaces
- Resumen
Explosive burning of hydrogen on top of accreting white dwarfs causes nova outbursts. The binary system where classical novae occur is a cataclysmic variable whereas, some, recurrent novae occur in symbiotic binaries. The analysis of the X-ray emission from novae in their post outburst stages provides important information about the nova ex- plosion mechanism and the reestablishment of accretion. In some cases, like V2487 Oph 1998, observations with XMM-Newton a few years after outburst indicate that accretion has been re-established and its X-ray spectra look like those of magnetic cataclysmic vari- ables, of the intermediate polar class.
In this work a numerical model of accretion flow onto magnetic white dwarfs and their corresponding X-ray emission has been developed to be compared with observations of post outburst novae where accretion is active again. Distributions of the different physical quantities that describe the emission region have been obtained for different masses of white dwarf and different accretion rates. The associated X-ray spectrum has been also obtained with the main objective of studying accretion in the emission region. These results have been applied to the nova V2487 Oph 1998 with the aim to obtain the mass of the white dwarf since this nova has been identified as a recurrent nova, with a previous eruption in 1900, and therefore as a good candidate for a type Ia Supernova progenitor.
