A Comprehensive Study of the X-Ray Pulsar Population in the Small Magellanic Cloud

Document Type

Student Presentation

Presentation Date



College of Arts and Sciences


Department of Physics

Faculty Sponsor

Dr. Daryl Macomb


X-ray pulsars form from binary star systems containing a neutron star and a companion star. Due to the strong gravitational pull, particles from the companion star accumulate into an accretion disk around the neutron star. The gas that is accreted from the companion star is channeled to the magnetic poles when the neutron star has a strong magnetic field. As the neutron star spins, we can detect those x-rays in pulses. Using data from the Chandra Space Telescope, we intend to search for unidentified strong x-ray pulsars and weakly pulsing, accreting x-ray pulsars in the Small Magellanic Cloud. We will also use data gathered on potential new and already known sources to see what spin can tell us about accretion, and search for correlations between pulse profiles and luminosity.

This document is currently not available here.