Refraction in a pulsar magnetosphere - The effect of a variable emission height on pulse morphology

P. Weltevrede; B. W. Stappers; L. J. Van Den Horn; R. T. Edwards

doi:10.1051/0004-6361:20031461

Refraction in a pulsar magnetosphere - The effect of a variable emission height on pulse morphology

P. Weltevrede, B. W. Stappers, L. J. Van Den Horn, R. T. Edwards

Research output: Contribution to journal › Article › peer-review

Abstract

The Petrova (2000) model to calculate pulse profiles is extended to a variable emission height model to make it physically self-consistent. In this context variable means that the emission height is no longer considered to be the same for different magnetic field lines. The pulse profiles calculated using this new model seem to be less realistic due to a focusing effect and cannot be used to fit (typical) multifrequency pulsar observations. Apart from the focusing effect the general morphology of pulse profiles is not greatly affected by introducing a variable emission height. Additional extensions of the model will be needed to be able to fit observations, and several suggestions are made.

Original language	English
Pages (from-to)	473-479
Number of pages	6
Journal	Astronomy and Astrophysics
Volume	412
Issue number	2
DOIs	https://doi.org/10.1051/0004-6361:20031461
Publication status	Published - Dec 2003

Keywords

Plasmas
Stars: pulsar general
Waves

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10.1051/0004-6361:20031461

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title = "Refraction in a pulsar magnetosphere - The effect of a variable emission height on pulse morphology",

abstract = "The Petrova (2000) model to calculate pulse profiles is extended to a variable emission height model to make it physically self-consistent. In this context variable means that the emission height is no longer considered to be the same for different magnetic field lines. The pulse profiles calculated using this new model seem to be less realistic due to a focusing effect and cannot be used to fit (typical) multifrequency pulsar observations. Apart from the focusing effect the general morphology of pulse profiles is not greatly affected by introducing a variable emission height. Additional extensions of the model will be needed to be able to fit observations, and several suggestions are made.",

keywords = "Plasmas, Stars: pulsar general, Waves",

author = "P. Weltevrede and Stappers, {B. W.} and {Van Den Horn}, {L. J.} and Edwards, {R. T.}",

year = "2003",

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T1 - Refraction in a pulsar magnetosphere - The effect of a variable emission height on pulse morphology

AU - Weltevrede, P.

AU - Stappers, B. W.

AU - Van Den Horn, L. J.

AU - Edwards, R. T.

PY - 2003/12

Y1 - 2003/12

N2 - The Petrova (2000) model to calculate pulse profiles is extended to a variable emission height model to make it physically self-consistent. In this context variable means that the emission height is no longer considered to be the same for different magnetic field lines. The pulse profiles calculated using this new model seem to be less realistic due to a focusing effect and cannot be used to fit (typical) multifrequency pulsar observations. Apart from the focusing effect the general morphology of pulse profiles is not greatly affected by introducing a variable emission height. Additional extensions of the model will be needed to be able to fit observations, and several suggestions are made.

AB - The Petrova (2000) model to calculate pulse profiles is extended to a variable emission height model to make it physically self-consistent. In this context variable means that the emission height is no longer considered to be the same for different magnetic field lines. The pulse profiles calculated using this new model seem to be less realistic due to a focusing effect and cannot be used to fit (typical) multifrequency pulsar observations. Apart from the focusing effect the general morphology of pulse profiles is not greatly affected by introducing a variable emission height. Additional extensions of the model will be needed to be able to fit observations, and several suggestions are made.

KW - Plasmas

KW - Stars: pulsar general

KW - Waves

U2 - 10.1051/0004-6361:20031461

DO - 10.1051/0004-6361:20031461

M3 - Article

SN - 0004-6361

VL - 412

SP - 473

EP - 479

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 2

ER -

Refraction in a pulsar magnetosphere - The effect of a variable emission height on pulse morphology

Abstract

Keywords

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