Origin of pulsar radio emission. I. High frequency data.

Details Origin of pulsar radio emission. I. High frequency data. Origin of pulsar radio emission. I. High frequency data.

Jun 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...322..846k&link_type=abstract

Astronomy and Astrophysics, v.322, p.846-856

Astronomy and Astrophysics

Astrophysics

36

Pulsars: General, Pulsars: Individual: B0329+54 (Psr 0329+54), B0355+54 (Psr 0355+54), B0540+23 (Psr 0540+23), B1133+16 (Psr 1133+16), B1706-16, B1929+10 (Psr 1929+10), B2020+28 (Psr 2020+28), B2021+51 (Psr 2021+51), Radiation Mechanisms: Miscellaneous

Scientific paper

Using the pulse arrival times from pulsar observations made between 1.4 and 32 GHz, we constrain the location and size of the magnetospheric region which is responsible for the observed radio emission. We demonstrate that for long period pulsars the magnetic field maintains its dipolar form throughout the whole emission region. The emission region itself is located very close to the stellar surface and confined to a small slab of a few tens stellar radii in height.

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