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Parkes observations for project P1052 semester 2020APRS_01
After five decades of study, the physics of radio wave emission and propagation in the pulsar magnetosphere remains poorly understood. This is largely due to the wide variety of dynamic phenomena observed in pulsar signals that are neither predicted nor explained by current theory, the limited window of the pulsar spectrum that previously could be... more studied simultaneously, and the biased sample of the pulsar population that has been studied to date. To address these limitations, we have developed pioneering statistical methods that provide new interpretive insights and enable us to study the dynamics of the radio pulsar signal on short time scales (e.g. drifting and quasi-periodic sub-pulse structure, transitions between orthogonally polarized modes of emission, nulling, etc.) even when individual pulses cannot be detected. Using our novel methods and the ultra-wide bandwidth receiver at Parkes, we will undertake a large-scale survey of pulsar radio emission statistics and explore two previously inaccessible regions where pulsar flux densities are typically much lower: the pulsar spectrum above 2 GHz, and the recycled pulsar population. Measuring the instantaneous bandwidth of impulsive emission events will yield new constraints on the physical conditions in the pulsar magnetosphere, such as the spatial scale of strong turbulence in the magnetospheric plasma. The breadth of our sample, from millisecond pulsars to magnetars, will enable us to study the evolution of emission and propagation physics over four orders of magnitude in magnetospheric size and seven orders of magnitude in magnetic field strength. less
Astronomical and Space Sciences not elsewhere classified
01 Apr 2020
30 Sep 2020
Creative Commons Attribution 4.0 International Licence
van Straten, Willem; Green, James; Johnston, Simon; Hobbs, George; Karastergiou, Aris; Bhat, Ramesh; Keith, Michael; Weltevrede, Patrick; Toomey, Lawrence; Jameson, Andrew; Dempsey, James; Tiburzi, Caterina; Jankowski, Fabian; Venkatraman Krishnan, Vivek; McSweeney, Samuel James; Primak, Natalia; Parthasarathy, Aditya; Oswald, Lucy; Shaifullah, Golam; Griffin, Anthony; Hankin, Robin; Maan, Yogesh; Szary, Andrzej; Dyks, Jaroslaw; Vohl, Dany (2020): Parkes observations for project P1052 semester 2020APRS_01. v1. CSIRO. Data Collection.
All Rights (including copyright) CSIRO 2020.
Access to this collection's metadata and/or files (if any) are restricted until 30 Mar 2022.
Australia Telescope National Facility
P1052 - Pulsar Radio Emission Statistics Survey (PRESS)
We are observing signals from a type of star known as a pulsar, one of the most extreme objects in the Universe. A pulsar is born during a dramatic explosion known as a supernova, which happens when a bright star many times bigger than our Sun runs out of fuel. The heavy core of the star collapses under its own weight into something more dense th... morean the nucleus of an atom! Imagine squashing our enormous Sun down to something about the size of Sydney! Pulsars have magnetic fields that are millions of times stronger than what can be produced here on Earth. Like a cosmic lighthouse, this magnetic field generates beams that sweep across the Galaxy with each rotation of the star. Unlike the steady beam of a lighthouse, a pulsar's beam crackles and pops with lightning-like discharges of energy. By studying this highly dynamic signal, we learn about what generates the radio waves and what happens as they travel through the turbulent plasma in the pulsar’s strong magnetic field. We have developed new techniques that enable us to study the weak signals from pulsars that have been overlooked to date. Using a cutting-edge receiver at The Dish, we are surveying a wide variety of pulsars with the aim of better understanding strong magnetic fields and the behaviour of high-energy particles of matter and antimatter, which stream along a pulsar’s magnetic field lines at close to the speed of light. less
Willem van Straten
Vivek Venkatraman Krishnan
Samuel James McSweeney