The supernova remnant G109.1-1.0 and the X-ray pulsar 1E2259+586

The Supernova remnant (SNR) G109.1-1.0 has three features of particular interest: a central X-ray pulsar, 1E2259+586; jet-like emission curving out from the pulsar across the SNR; and a possible interaction with a nearby molecular cloud associated with the HII regions S147-S153. In this thesis I present work on all three of these aspects using data from a wide range of wavelengths. The discovery and early observations of G109.1-1.0 and 1E2259+586 are reviewed, as well as the theoretical interpretations of these results. The relationship between G109.1-1.0 and the molecular cloud is investigated using archive far-IR data from the IRAS satellite. The correlation between the X-ray, far-IR and CO emission provides convincing evidence of a physical interaction. The jet-like feature also appears to be part of this general correlation, and the possible significance for different interpretations of this emission are discussed. New X-ray results are presented from the study of archive data from two satellites, HEAO-1 and EXOSAT. An attempt is made to develop a low mass X-ray binary (LMXRB) model for 1E2259+586 that is consistent with these observational results, relating 1E2259+586 to G109.1-1.0. One idea is that the spin down is due to the recent formation of the pulsar, producing a system that has yet to reach equilibrium. Other possible models for 1E2259+586 are also discussed in the light of the observational data presented in this thesis. It is concluded that the LMXRB model is the most convincing to date, but that confirmation will probably have to wait until results from new X-ray satellites become available. (author)