Astron. Astrophys. 332, L21-L24 (1998)
2. Coherent curvature radiation
Curvature radiation can be described in terms of emission by a
relativistic particle moving around the arc of a circle chosen such
that the actual acceleration corresponds to centripetal acceleration.
A relativistic electron with Lorentz factor ,
constrained to follow a path with radius of curvature
, radiates similarly to an electron in a circular
orbit with frequency . The critical frequency
where most of the radiation is emitted is approximately given by (e.g.
Zheleznyakov 1996, p. 231)
![[EQUATION]](img4.gif)
Or if we observe a particular frequency we find the corresponding
Lorentz factor via
![[EQUATION]](img5.gif)
The curvature radius of the field lines in a magnetic dipole field
can be expressed as (Smirnow 1973, p. 211)
![[EQUATION]](img6.gif)
where is the collateral angle of a point on
the field line starting at at the pulsar
surface. A reasonable approximation up to is
given by
![[EQUATION]](img10.gif)
where is the curvature radius at the pulsar
surface.
The total power radiated by a particle of energy
along a curved field line is
( denotes the charge)
![[EQUATION]](img14.gif)
The classical Goldreich-Julian charge density in the pulsar
magnetosphere (Goldreich and Julian 1969)
![[EQUATION]](img15.gif)
provides us with a typical particle density of
if P=0.5 s and G. It
enables us to estimate the typical size of the emission region for
incoherent curvature emission. For the lowest luminosity
(0655+64 (Taylor et al. 1993) we find
. Using Eqs. (1b), (4) and (5) together with the
simplifying assumption that the emission region extends across the
line of sight as well as along it, we find that the predicted profile
widths for incoherent curvature emission turn out to be within
![[EQUATION]](img20.gif)
For frequencies below we predict profile
widths of roughly 180 degrees and only when we approach
( ) can we expect widths
of around 25 degrees. Typical pulsar profile widths at radio
frequencies are however of the order of 5-10 degrees (e.g. Izvekova
et. al. 1994, Seiradakis et. al. 1995). Because of the narrow profiles
of the pulsed emission we must rule out any consideration of
incoherent curvature emission as the source of the observed
pulsar radio luminosities.
As incoherent emission is obviously insufficient it might be
worthwhile to turn or attention to coherent curvature emission
which has been suggested as an emission mechanism (see references
above). Coherence exists in volumes of the order of
(Melrose 1992). The power output of such a
coherence volume is then given by:
![[EQUATION]](img25.gif)
with being the number of particles within a
coherence volume. To account for the observed luminosity L one
requires of these volumes, which will give us
an estimate of the total number of particles involved
![[EQUATION]](img28.gif)
and the minimal size of the emission region
![[EQUATION]](img29.gif)
Energy conservation alone provides us with an important constraint
that will enable us to restrict the free parameter
and to check the consistency of the model.
The energy loss of a charge within the emission region is now
![[EQUATION]](img30.gif)
which must never exceed the energy of the particle
itself.
The bunching of particles requires an external electric force which
confines the particles in a coherence volume. Although electrostatic
instabilities have been criticized for several reasons, the principal
argument, that electrostatic plasma wave can be responsible for the
bunching of particles has not been questioned, only processes that
excite the waves are under discussion. The Doppler shifted plasma
waves oscillate with the local plasma frequency
of the particles and therefore their electrostatic fields present the
ideal bunching force. When the particles are in resonance with the
wave they experience the wave electric field most intensively and they
are confined (bunched) in the coherence volume .
The same resonance condition holds for the propagation of
electromagnetic waves with frequency (where
), which defines a certain radius in the pulsar
magnetosphere, at which the coherent radiation can escape from the
plasma. Particle bunching and wave propagation is determined by the
same condition (e.g. Melrose 1992). Since the
bunching leads to a very fast and efficient emission the place at
which the condition is fulfilled is also the place of emission, i.e.
the emission height. For larger radii only lower frequencies can be
emitted (see Eqs. (1a) and (3)). An increase in density corresponds to
an increase in frequency at a given radius (Eq. (5)). With the
determination of the minimum emission height from
using Eq. (1b) to eliminate
![[EQUATION]](img36.gif)
we can express the ratio of emitted energy over the total energy
as
![[EQUATION]](img37.gif)
which cannot exceed unity. From the condition
we obtain a condition for the luminosity by
inserting Eqs. (1-9) into Eq. (10), leaving
![[EQUATION]](img39.gif)
© European Southern Observatory (ESO) 1998
Online publication: March 10, 1998
helpdesk@link.springer.de  |