Radio Pulsar Phenomenology: What can we learn from pulsar profiles?

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Assumptions aboutradio emission• Emission from open fieldlines above polar cap• Dipolar magnetic field• Emission from near surface• Must be coherent emission(unlike at high energies)Could argue about allthese assumptions!
Pulsar geometry and therotating vector modelImportant angles are:α – angle between therotation and magnetic axisβ – closest approach of lineof sight to magnetic axisρ – cone opening angleThe RVM uses the PA swing to derive the geometry
Page 1 and 2: Radio Pulsar Phenomenology:What can
Page 3: Basic Observables and Derivables. I
Page 17 and 18: Basic Observables and Derivables. I
Page 19 and 20: Kramer et al. 2006Image: NASAVerbie
Page 21: Basic Observables and Derivables. V
Page 25 and 26: The Rotating Vector Model (RVM) for
Page 37 and 38: α = 30, β = -1.7α = 86, β = -3.
Page 39 and 40: Mapping the magnetosphere• We can
Page 41 and 42: Beam modelof Lyne &ManchesterIn a n
Page 43 and 44: Young pulsarstudy ofJohnston &Weisb
Page 45 and 46: Polarization and the P-Pdot diagram
Page 47 and 48: Orthogonal RotatorsWeltevrede & Wri
Page 49 and 50: Summary• The integrated profiles

Radio Pulsar Phenomenology: What can we learn from pulsar profiles?

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