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

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Pulse width versus EdotOrthogonal rotatorsHigh Edot, widebeam single poleLow Edotaligned rotatorsWeltevrede &Johnston studyof interpulse<strong>pulsar</strong>s.In a nutshell: Random orientation of B-Ω axis atbirth, becoming aligned over time.
Orthogonal RotatorsWeltevrede & Wright 2009Kramer & Johnston 2008Beam mapping of B0906-49 (left) and B1055-52(above) following RVM fits. Emission heights similarabove both poles. Evidence for emission <strong>from</strong> theclosed field lines (see also Keith et al. 2010).
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 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: Polarization and the P-Pdot diagram
Page 49 and 50: Summary• The integrated profiles

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

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