Pulsar Astrometry in the Presence of Low Frequency Noise

Abstract

The following results of dissertation are submitted for defense: 1. Precise measurements of coordinates and proper motion of the pulsar PSR 0329+54 using the VLBI method. 2. Establishing of the reason for the discrepancy between the coordinates of pulsars measured by VLBI and timing methods, which comes down to the influence of low-frequency noise at the time of pulse arrivals (TOAs) from the pulsar. 3. A special method for processing timing observations that allows you to correct TOA - coordinates of pulsars. 4. Theoretical dependencies of the behavior of dispersion of pulsar parameter depending on the observation interval and the type of correlated noise, on the basis of which it became possible to propose a new time scale BPT based on the orbital motion of pulsar in binary system stable over long periods of time (more than 10 years). 5. A theory that explains spontaneous changes in the rotational frequency of pulsars through their interaction with the passing gravitating mass and the theoretical power spectrum of low-frequency fluctuations of the pulsar rotational phase caused by gravitational disturbances from the passage of bodies near the pulsar.