Abstract
Rotation-powered pulsars can produce observable high-energy emission by a number of mechanisms. Non-thermal X-rays and gamma-rays are produced by relativistic particles, accelerated in the pulsar magnetosphere at a still unknown location, via curvature, synchrotron and inverse Compton radiation. Thermal X-rays may be produced at the stellar surface by cooling of the neutron star or by a variety of possible heating mechanisms that include the bombardment of the surface by backflowing particles and internal friction. In pulsars with ultra-strong fields, known as magnetars, the magnetic field is the dominant energy source responsible for both the radiation and the spin-down behavior. I will review models for pulsar emission in light of recent X-ray data from ROSAT, ASCA and RXTE.
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
