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Parkes observations for project P888 semester 2015APRS_BPSR_02
Erratically-emitting neutron stars like Rotating Radio Transients (RRATs), represent approximately 3% (and increasing) of radio-emitting pulsars as they are found via searches of archival and current pulsar surveys. The sporadic emission from these sources makes them difficult to study and nearly all information about the properties of the objects ... moreis the result of dedicated monitoring and timing programs at Parkes telescope. This project represents an effort to obtain accurate timing solutions of a sample of sparse-emitting pulsars. We will monitor and time 6 sources to determine basic RRAT properties including spin period, spin period derivative, and polarization properties. Thus enabling us to identify physical causes for the extreme emission, enable high-energy follow-up observations, deduce how these pulsars are related to the general pulsar and magnetar populations, and explore the distribution of extreme radio intermittence in neutron stars. less
Astronomical and Space Sciences not elsewhere classified
01 Apr 2015
30 Sep 2015
Creative Commons Attribution 4.0 International Licence
Petroff, Emily; Johnston, Simon; van Straten, Willem; Keane, Evan; Caleb, Manisha (2015): Parkes observations for project P888 semester 2015APRS_BPSR_02. v1. CSIRO. Data Collection.
All Rights (including copyright) CSIRO 2015.
The metadata and files (if any) are available to the public.
Australia Telescope National Facility
P888 - Expanding the rotating radio transient parameter space
Neutron stars are the result of stellar explosions (supernovae) which occur in massive stars once they have reached the ends of their lives. Most pulsars are detectable by their regular intervals of pulsed emission (occurring every few seconds, up to several hundred times a second!), which happens because the star is rotating and flashing a beam of... more radio light across Earth. Since the first discovery of pulsars we have discovered some very sporadically-emitting pulsars, which are not emitting all the time. Understanding the reason for this may assist us in explaining the origin of radio emission in neutron stars. We are monitoring a small subset of these sources to determine their age, magnetic field strengths, and emissive properties. These observations should lead to a more complete physical understanding of these strange behaviours and pulsar-emission origins. less
Willem van Straten
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