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El objetivo de esta tesis es el estudio de las caractersticas espectrales presentes en el plsar de rayos X 4U 153852/QV Nor, su variacin a lo largo de un perodo orbital y el anlisis de las correlaciones entre los parmetros que definen las lneas espectrales y el continuo. Las observaciones se han obtenido de la base de datos del observatorio espacial Rossi Xray Timing Explorer (RXTE). Tambin se utilizaron ms de 400 ventanas cientficas de este sistema obtenidos con el satlite INTErnational GammaRay Astrophysics Laboratory (INTEGRAL) para conseguir un espectro con INTEGRAL Soft GammaRay Imager (ISGRI) en el rango de energas 17100 keV. A partir del modelo que describa bien los espectros, se estudi la variabilidad de la lnea ciclotrn fundamental que permiti establecer correlaciones entre la anchura relativa y la profundidad ptica de la lnea ciclotrn, y entre la anchura de la lnea ciclotrn y su energa (RodesRoca et al. 2008). Tambin presentamos evidencias de la presencia del segundo armnico cuya confirmacin se present en RodesRoca et al. (2009). Finalmente, se obtuvo una estimacin de la prdida de masa de la estrella supergigante.
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