Speaker
Description
We investigated a novel pulsar planet detection method based on radio emissions produced by the interaction of a terrestrial planet with the pulsar wind.
Using the PLUTO code, we simulate relativistic magnetohydrodynamics of an Earth-sized planet surrounded by highly relativistic pulsar wind. We achieved a Lorentz factor of approximately 5.8 or a pulsar wind speed of approximately 98.5% of the speed of light in our simulation.
We consider two distinct planetary response regimes: with the planet modeled as a perfect conductor and a ferromagnetic scenario, where the external magnetic field magnetizes the planet in turn.
We examine the effects of changes in pulsar wind densities and external magnetic field strengths on the radio emission characteristics and compare the results with previous studies at lower velocity. The resulting emissions show characteristics similar to those of Alfven wing structures, in which wing-like disturbances in the flow are produced by the interaction of a conducting barrier with a magnetized plasma. We evaluated whether currently known pulsar planets can be found by their radioemissions. For this, we consider two planet classes: terrestrial and diamond planets. We evaluated whether these planets could be detected with current radio telescopes.