<html><head><meta http-equiv="Content-Type" content="text/html charset=us-ascii"></head><body style="word-wrap: break-word; -webkit-nbsp-mode: space; -webkit-line-break: after-white-space;" class="">Dear all,<div class=""><br class=""></div><div class="">Tomorrow (Wednesday) at<b class=""> 3 p.m. </b>in <b class="">F201</b> of the Physics Department dr. <b class="">Charlotte Sobey</b> is going to give a talk on <b class="">pulsars</b> and their effect on surrounding regions. </div><div class=""><br class=""></div><div class=""><b class="">Presenter</b>: Dr. Charlotte Sobey (ICRAR & CSIRO, Perth, Australia)</div><div class=""><br class=""></div><div class=""><b class="">Title</b>: Using low-frequency polarisation observations of pulsars to investigate the 3-D structure of the Galactic magnetic field</div><br class=""><div class=""><b class="">Abstract</b>:</div><div class="">Polarisation observations of pulsars using next-generation low-frequency radio telescopes provide powerful probes <br class="">of astrophysical plasmas. For example, dispersion and rotation measures (DMs and RMs) towards pulsars provide <br class="">an efficient method to determine the average strength and direction of magnetic fields in intervening regions.<br class="">Low-frequency radio observations with large fractional bandwidths provide precise DMs and RMs, demonstrated <br class="">by a catalogue of RMs (corrected for ionospheric Faraday rotation) using LOFAR (Low-Frequency Array), and a <br class="">growing complementary catalogue in the southern hemisphere using the MWA (Murchison Widefield Array). <br class="">These measurements further our knowledge of the three-dimensional structure of the Galactic magnetic field, <br class="">which plays a role in many astrophysical processes, but is not yet well understood.</div><div class=""><br class=""></div><div class="">See you Tomorrow.</div><div class=""><br class=""></div><div class="">Cheers,</div><div class="">Lana Ceraj</div></body></html>