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Parkes observations for project P995 semester 2018OCTS_19
We propose to perform observations of the very young pulsar PSR B0540–69 in the Large Magellanic Cloud to detect pulsed flux from this traditionally radio-quiet source. We are motivated to do so due to a relatively recent X-ray observation of a 36% change in its spin down rate, thought to be due to a state change in its magnetospheric proces... moreses. There is reason to believe this may be accompanied by an increase in pulsed flux, as has been seen in intermittent pulsar behaviour, for example. Additionally, PSR B0540–69 is known to emit giant pulses, one of only a small number of pulsars to do so. With the new Ultra Wideband Low-frequency (UWL) receiver system, we will be able to conduct the highest sensitivity observations of this source yet achieved at radio wavelengths. A successful detection of pulsed flux will provide important insight into the magnetospheric evolution and behaviour in this pulsar, and a better understanding of how its glitch behaviour may influence its emission. Even without such a detection, we will be able to study the giant pulse behaviour of PSR B0540–69 with unprecedented sensitivity. less
Astronomical and Space Sciences not elsewhere classified
01 Oct 2018
01 Apr 2019
supernovae / supernovae remnants
Creative Commons Attribution 4.0 International Licence
Ferdman, Robert; Kaspi, Victoria ; Archibald, Robert (2018): Parkes observations for project P995 semester 2018OCTS_19. v1. CSIRO. Data Collection.
All Rights (including copyright) CSIRO 2018.
Access to this collection's metadata and/or files (if any) are restricted until 01 Oct 2020.
Australia Telescope National Facility
P995 - A search for pulsed emission from PSR~B0540–69 after a state change
PSR B0540–69 is a very young pulsar in the Large Magellanic Cloud, a satellite galaxy of our Milky Way. It was formed as a very dense, fast-spinning neutron-star remnant of a violent supernova explosion that occurred nearly 1700 years ago. We see a "pulse" with each rotation of these objects, as its emission beam sweeps past out line of sight, lik... moree a cosmic lighthouse. Unlike their older counterparts, young pulsars are known to behave more erratically, showing pronounced changes in their rotation over time. This behaviour can be due to several factors, including processes that occur within their exotic interiors, of which much is still not understood, as well as with their magnetic fields, which are among the strongest in the Universe. These processes can often cause pulsars to change their rotational velocity significantly, and in turn their observed emission properties. We believe this may have happened to PSR B0540–69. We have so far not been able to observe radio-wavelength emission from PSR B0540–69, but it has recently undergone a major change in its rotational behaviour, and we intend to search for radio pulsed emission, which we believe may have accompanied this change. This would give us new insight into the magnetic field evolution and behaviour of young pulsars. less
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