On the timing formula for isolated pulsars - The case of bunching emission

Details On the timing formula for isolated pulsars - The case of bunching emission On the timing formula for isolated pulsars - The case of bunching emission

Aug 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...331..397b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 331, Aug. 1, 1988, p. 397-401. CAICYT-supported research.

Astronomy and Astrophysics

Astrophysics

Astrophysics, Magnetohydrodynamics, Pulsars, Stellar Radiation, Gravitational Effects, Periodic Variations, Stellar Magnetic Fields, Stellar Models, Stellar Rotation

Scientific paper

The authors argue that the timing formula used to fit the pulse arrival times for an isolated pulsar is very sensitive to phenomena occurring in the emission zone. It is shown that, even when no gravitational effects are taken into account, the usual polynomial expansion for the number of pulses in terms of the arrival times is very likely not to be appropriate for very long term observations. For the case of bunching emission (acceleration parallel to the magnetic field) there is a long-term periodic residual (period ≈1 yr) in the timing formula, which could be of crucial importance when analyzing the timing noise.

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