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

More documents

Recommendations

Info

RVM is a useful tooland geometry iscrucial for testingmodels of γ-rayemission (and radioemission). In practice,hard to constrain.This PA swing is “forbidden” by the RVM, and is likelythe result of magnetospheric or propagation effects.
Mapping the magnetosphere• We can use the radio observations to make a3D map of the emission zones– Need geometry– Need a method of computing altitudes– Need a large sample of pulsars• BUT– Geometry often uncertain– Conflicting results from altitude derivations• Models of the beam
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: α = 30, β = -1.7α = 86, β = -3.
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?

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?