X-ray/TeV observations of pulsar systems
Abstract
The results of this study indicate that there are as yet no pulsed >1012 eV [special characters omitted]-rays from the Crab pulsar, PSR B1951+32, PSR B1823-13 and PSR J0538+2817. In addition there was no steady emission above the sensitivity of the detector for PSR B0656+14, PSR B0355+54, PSR B0114+58 and PSR B2334+61. If such primary [special characters omitted]-rays are required to make the pulsar emit at other frequencies then the TeV upper limits constrain the site of the emission region above the polar cap where magnetic pair production would absorb these photons. While inverse Compton scattering is a plausible mechanism for high energy emission in pulsar systems such as the Crab Nebula it has not resulted in a viable mechanism for producing TeV photons in PSR B1823-13 and PSR B1951+32 as predicted. Standard analysis, using a typical background estimate, indicated a marginally significant signal in the case of PSR B0656+14 and PSR B1823-13. Since this is highly dependent on the background, some control observations are required to establish the status of these promising candidates. The lack of TeV pulsations from PSR B1951+32 provides a strong discriminant between pulsar emission models. Periodic analysis of PSR J0538+2817 indicates that the probability of the validity of the null hypothesis is 0.013% which indicates a possible signal. An improved timing solution is needed to make a conclusive statement.
Degree
Ph.D.
Advisors
Finley, Purdue University.
Subject Area
Astronomy|Astrophysics
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