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

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Basic Observables and Derivables. III.MeasurePulse arrival times, glitch parameters,timing noise, binary parametersDeriveTests of general relativityDetection of gravitational waves<strong>Pulsar</strong> distancesNS interior density profile and structureEquation of state
Kramer et al. 2006Image: NASAVerbiest et al. 2010
Page 1 and 2: Radio Pulsar Phenomenology:What can
Page 3: Basic Observables and Derivables. I
Page 17: Basic Observables and Derivables. I
Page 21 and 22: Basic Observables and Derivables. V
Page 23 and 24: Pulsar geometry and therotating vec
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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