Abstract
We present an inverse mapping approach to determining the emission height of the optical photons from pulsars, which is directly constrained by empirical data. The model discussed is for the case of the Crab pulsar. Our method, using the optical Stokes parameters, determines the most likely geometry for emission including magnetic field inclination angle (α), observer's line-of-sight angle (χ) and emission height. We discuss the computational implementation of the approach, along with any physical assumptions made. We find that the most likely emission altitude is at 20 per cent of the light cylinder radius above the stellar surface in the open field region. We also present a general treatment of the expected polarization from synchrotron source with a truncated power-law spectrum of particles.
Original language | English (US) |
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Pages (from-to) | 730-744 |
Number of pages | 15 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 417 |
Issue number | 1 |
DOIs | |
State | Published - Oct 2011 |
Externally published | Yes |
Keywords
- Methods: numerical
- Pulsars: general
- Pulsars: individual: Crab
- Radiation mechanisms: non-thermal
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science