Pulsar Polarization studies at low radio frequencies

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Presentation transcript:

Pulsar Polarization studies at low radio frequencies Dipanjan Mitra Ncra, Tifr, Pune India Collaborators: J Rankin, S Johnston, A Karasterigiou, S Kudale Y Gupta, J Gil Thanks to GMRT / NCRA colleagues for their support during various projects 19/02/2019

Polarization observation at low frequencies (GMRT) 150 MHz 325 MHz Mitra, Gupta, Kudale (2004) 19/02/2019

GMRT – Parkes, Pulsar Polarization survey:243, 325, 660, 1400, 3100 MHz Johnston, Karasterigiou, Mitra, Gupta (2008) 19/02/2019

19/02/2019

Average Polarization Properties Linear polarization of pulsars decreases with increasing frequency RFM , OPM PA traverses often don’t agree with RVM and sometimes are frequency dependent. Circular polarization is usually, higher towards the pulse centre Younger pulsars are more polarized than older pulsars All these indicate that average polarization properties results from some incoherent averaging process. 19/02/2019

Complication in Pulsar Polarization: PSR B0329+54 Mitra, Rankin, Gupta 2007 19/02/2019

The kinky features are frequency Independent, and spans a range of 90 degrees in PA 19/02/2019

Core Intensity dependent polarization behaviour If pulsars after supernova kicks move along the rotation axis then one can find the X mode or O mode of emission O mode should suffer from propagation effects 19/02/2019

More examples of PA distortions 19/02/2019

Examples of PA distortions in single pulses 19/02/2019

90 deg PA SWINGS 19/02/2019

Highly polarized, narrow emission pulses With sign changing circular. Single particle Curvature radiation like emission 19/02/2019

Core intensity dependence 19/02/2019

19/02/2019

PA swing due to averaging Of coherent emission A/R causing shift in the PA 19/02/2019

PA below the core emission is a result of Incoherent addition of several smaller units of emission with OPM jumps in a given subpulse. This result maybe confirmed by the observed 90 deg PA swings, and sign changing circular, low subpulse polarization Due to height dependent emission of the core. This result arises from the earlier Arrival of the core emission with intensity. The smaller units of emission are highly polarized and show sign changing Circular , just like a single particle curvature radiation. 19/02/2019

Partial cone pulsars 19/02/2019

Flared Pulses Mitra, Rankin, Sarala 2008 19/02/2019

19/02/2019

A/R effect 19/02/2019

Episiodic illumination : There are different from flared pulses Rankin et al 2007 19/02/2019

Conclusion Probability of pulsar emission varies from almost 95% to ~3% across the Pulse. The polarization properties of partial cones are just like other normal pulsars And the conal emission seems to arise from about 300-400 km (like other Pulsars). Collaborators: J Rankin, S Johnston, A Karasterigiou, S Kudale Y Gupta, J Gil Thanks to GMRT / NCRA staff for their support during various projects 19/02/2019