The Net Advance of Physics: Gamma-Ray Pulsar Emission Models, by Alice K. Harding -- Section 3A.
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Polar cap models divide according to the mechanism of
acceleration above the surface of the neutron star (see Usov 1996,
for more detailed review of acceleration mechanisms). In pulsars
having , where is the direction of the rotation axis, the
corotation charge ( ) above the magnetic poles is
negative. If the neutron star surface temperature,
K
where is the electron surface binding temperature, then electrons
are freely released from the surface to be accelerated in parallel
electric fields induced by space-charge-limited flow (Michel 1991),
field-line curvature (Arons & Scharlemann 1979, Arons 1983)
and inertial frame dragging (Muslimov & Tsygan 1992). In these
models, at the surface and increases with height.
In pulsars having , the corotation charge above the poles
is positive and if
K, where is the ion surface binding temperature, then the ions are
trapped in the surface. Since the corotation charge cannot be supplied, a
vacuum gap and thus a non-zero grows at the stellar surface
(Ruderman & Sutherland 1975). In most cases, the is
shorted out at some altitude by the onset of electron-positron pair
cascades in the strong
magnetic field. However, the creation of bound-pairs (Shabad & Usov 1985)
instead of free-pairs in fields could delay the
shorting out of to larger heights above the surface, thus
increasing the acceleration energy. But Usov & Melrose (1995) found this to
be an important effect only in Ruderman-Sutherland type models.
Several different kinds of models for polar cap pair cascades have been
studied. If the accelerated primary particles reach energies of
, then curvature radiation will dominate their energy loss.
For inverse Compton scattering of X-rays, either
non-thermal cascade emission or thermal emission from a hot
polar cap, will be more important. More specifically, the energy loss
for curvature radiation of an electron moving parallel to a
magnetic field with radius of curvature cm will exceed
the energy loss due to non-magnetic inverse Compton scattering of
blackbody radiation at temperature K, when
(valid for
in fields around G, Dermer 1990).
At , resonant Compton scattering will be
important because the soft photons at temperatures near K
will be blueshifted into the cyclotron resonance in the electron rest
frame, greatly enhancing the scattering cross section and thus the
energy loss rate (Daugherty & Harding 1989, Dermer 1989). The
accelerated particles will radiate
-rays by curvature radiation,
inverse Compton scattering (or a combination of both) which then pair
produce by the process in the strong
magnetic field. The pairs are produced in excited Landau states which
decay by emission of synchrotron photons, many of which will also
produce pairs. The cascade will continue, reprocessing and thus softening
the primary emission spectrum, until the photons escape.
Although it is possible for emission from both polar caps to be visible to
observers in the proper orientation, these models have focussed in the
last few years on emission from a single polar cap (SPC). In both the
curvature radiation-induced pair cascade (CRPC) and the Inverse
Compton-induced pair cascade (ICPC) models, the -ray emission pattern
is a hollow cone. Since the radius
of curvature of the magnetic field lines is infinite at the poles and
decreases towards the polar cap rim, the curvature emission is a maximum at
the rim in the CRPC models. In the ICPC models, the emission is also
maximum at
the rim where the angle between the relativistic particles moving along field
lines and the soft photons is largest.
The -ray beam half-angle, , is determined
approximately by the locus of the tangents to the outermost open field lines:
where is the polar cap half-angle, r is the radius of emission
and R is the neutron star radius. When as shown in Figure 1, an observer may see a broad double-peaked
-ray pulse profile, with bridge emission from inside the polar cap
rim. In CRPC models one can allow for extended acceleration regions
(up to several stellar
radii) above the polar cap, and the outward flaring of the field lines with
height rapidly increases to as large as to
(Daugherty & Harding 1996, hereafter DH96).
Thus, CRPC models no longer require very small
inclinations to accommodate large phase separations in doubly-peaked profiles,
as in previous SPC models (Daugherty & Harding 1994; Sturner et al. 1995,
Sturner et al. 1995). Figure 2 shows simulated distibutions of
double pulse peak separations, , expected for random observers
and various assumed distributions of pulsar obliquity. For uniform ,
the distributions predict enough large phase separations only for very large
, and are then too sharply peaked to allow many small values
of . But when is limited to even moderately small values,
the predicted distributions are more consistent with those observed and will
allow smaller values of .
Polar Cap Models
Figure 1: Geometry of single polar cap (SPC) emission. is the observer
polar angle.
Figure 2: Simulated (solid lines) and observed (shaded histogram)
distributions of pulse peak separation, for uniform
(upper left) and limited obliquity .
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