Publication: Caracterización de la emisión de muy alta energía de los púlsares con los telescopios Magic
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2016-07-07
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Universidad Complutense de Madrid
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Abstract
En 1967, la estudiante de doctorado Jocelyn Bell Burnell, observ o por primera vez la se~nal procedente de un p ulsar. Estos objetos estelares han sido desde entonces intensamente estudiados a todas las longitudes de onda. Debido a su intenso campo magn etico y gravitatorio, los p ulsares se han convertido en uno de los mejores laboratorios para el estudio de la materia en condiciones extremas. Recientemente, la detecci on de emisi on de muy alta energ as (VHE > 100 GeV) del p ulsar del Cangrejo ha obligado a replantearnos nuestras ideas sobre el funcionamiento de estas estrellas, ya que tal emisi on parec a descartada a priori por los modelos te oricos existentes. Estos modelos proponen distintos lugares en las magnetosferas de los p ulsares, y en torno a estas, como origen de la emisi on de muy alta energ a detectada, cada uno con caracter sticas propias en la distribuci on espectrales de energ a y en las curva de luz esperadas. Las observaciones de los p ulsares a muy altas energ as son por lo tanto fundamentales para entender la ubicaci on y los mecanismos de la emisi on y distinguir entre los distintos modelos. Esta tesis trata de la caracterizaci on de la emisi on de muy alta energ a de los p ulsares. Este estudio est a basado en las observaciones de p ulsares con los telescopios MAGIC y Fermi-LAT y en una estimaci on anal tica de la e ciencia de emisi on en rayos X y rayos gamma de los p ulsares en el contexto del modelo del \outer gap" o de \zona externa"...
For several decades, since their discovery in 1967 by Jocelyn Bell Burnell, pulsars have been under intense investigation. Due to their huge magnetic and gravitational elds, pulsars are one of the best laboratories to study matter in extreme conditions. Recently, the detection of emission from the Crab pulsar at Very High Energies (VHE, > 100 GeV) was a breakthrough, as such emission was totally unexpected. Even though pulsars are being deeply studied, their emission location and mechanisms are still poorly understood. Several regions where the VHE gamma rays are expected to be emitted where proposed, each of them exhibiting di erent features in the pulsars emission, such as energy spectrum and light curve properties. The observation of pulsars at VHE is then fundamental in order to understand their emission properties and distinguish between the current models. This thesis deals with the characterization of the VHE emission from pulsars. This study relies on the observations of pulsars with the MAGIC telescopes and the analytic calculation of the pulsar X-ray and gamma-ray emission e ciencies in the framework of the outer-gap model. Two pulsars were selected for the observations with the MAGIC telescopes, namely, the Crab and Geminga pulsars. These pulsars are the two brightest gamma-ray pulsars observable from the Northern Hemisphere. The study of the Crab pulsar revealed the signi cant emission from the interpulse region, also called bridge, located between the two main peaks. This component, already observed at low energies and predicted at VHE, was not previously detected at VHE. Furthermore, the relative emission between the two main peaks and the bridge was computed, including the analysis of 6.5 years of Fermi-LAT data. The behaviors of P2/P1 and bridge/P1 revealed a similar trend, unveiling similar properties in the emission of these distinct components...
For several decades, since their discovery in 1967 by Jocelyn Bell Burnell, pulsars have been under intense investigation. Due to their huge magnetic and gravitational elds, pulsars are one of the best laboratories to study matter in extreme conditions. Recently, the detection of emission from the Crab pulsar at Very High Energies (VHE, > 100 GeV) was a breakthrough, as such emission was totally unexpected. Even though pulsars are being deeply studied, their emission location and mechanisms are still poorly understood. Several regions where the VHE gamma rays are expected to be emitted where proposed, each of them exhibiting di erent features in the pulsars emission, such as energy spectrum and light curve properties. The observation of pulsars at VHE is then fundamental in order to understand their emission properties and distinguish between the current models. This thesis deals with the characterization of the VHE emission from pulsars. This study relies on the observations of pulsars with the MAGIC telescopes and the analytic calculation of the pulsar X-ray and gamma-ray emission e ciencies in the framework of the outer-gap model. Two pulsars were selected for the observations with the MAGIC telescopes, namely, the Crab and Geminga pulsars. These pulsars are the two brightest gamma-ray pulsars observable from the Northern Hemisphere. The study of the Crab pulsar revealed the signi cant emission from the interpulse region, also called bridge, located between the two main peaks. This component, already observed at low energies and predicted at VHE, was not previously detected at VHE. Furthermore, the relative emission between the two main peaks and the bridge was computed, including the analysis of 6.5 years of Fermi-LAT data. The behaviors of P2/P1 and bridge/P1 revealed a similar trend, unveiling similar properties in the emission of these distinct components...
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Tesis inédita de la Universidad Complutense de Madrid, Facultad de Ciencias Físicas, Departamento de Física Atómica, Molecular y Nuclear, leída el 09/02/2016