Tackling Radio Polarization of Energetic Pulsars

Abstract

The traditional, geometrical rotating vector model (RVM) has proved particularly poor at capturing the polarization sweeps of the young energetic and millisecond pulsars detected by \textit{Fermi}. We augment this model by including finite altitude effects using a swept back vacuum dipole geometry. By further including the effects of orthogonal mode jumps, multiple emission altitudes, open zone growth via y-point lowering, and interstellar scattering, we show that a wide range of departures from RVM can be modeled well while retaining a geometrical picture. We illustrate these effects by fitting six \textit{Fermi}-detected pulsars (J0023$+$0923, J1024$-$0719, J1744$-$1134, J1057$-$5226, J1420$-$6048, and J2124$-$3358) and we describe how such modeling can improve our understanding of their emission geometry.

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Cited by in corpus (9)

• The Thousand-Pulsar-Array programme on MeerKAT XI: Application of the rotating vector model
• On the difference between gamma-ray-detected and non-gamma-ray-detected pulsars
• A broadband radio study of the average profile and giant pulses from PSR B1821-24A
• The NANOGrav 11-Year Data Set: Arecibo Observatory Polarimetry And Pulse Microcomponents
• The NANOGrav 12.5-Year Data Set: Polarimetry and Faraday Rotation Measures from Observations of Millisecond Pulsars with the Green Bank Telescope
• Polarized emission from of an off-centred dipole
• A broadband radio study of PSR J0250+5854: the slowest-spinning radio pulsar known
• Modeling Multi-wavelength Pulse Profiles of Millisecond Pulsar PSR B1821-24
• Effects of gravitational waves on the polarization of pulsars