We should note that the neutrino damping of nonradial pulsations discussed by D. Kazanas and D. N. Schramm, Astrophys. J. 214, 819 (1977), is not relevant here. The nonaxisymmetric configuration is a lowest-energy (equilibrium) state of the core and is not associated with pulsations.^^The arguments presented earlier with regard to magnetic fields apply even more strongly here. If neutron-star fields are any indication, there simply is not enough time for sufficient winding of the field lines. ^^B. D. Miller, Astrophys. J. 187, 609 (1974); M. N. Fedorov and V. P. Tsvetkov, Zh. Eksp. Teor. Fiz. 65^, 1289) [Sov. Phys. JETP 38, 641 (1974] . ^^Descriptions of representative experiments are given by J. Weber, Phys. Rev. Lett. 22, 1320Lett. 22, (1969;
For the Crab pulsar (L = 10^^ erg/sec, ^ = 200 rad/ sec), Jc~ 1.7x10^^ particles/sec and e^^^ «2.8 xlO^^(J^/J) eV. Thus, for a given L, a larger flux of lower energy or smaller flux of higherenergy cosmic rays may be obtained, depending on J. In either case, 50% of the pulsar wave luminosity is converted into cosmic rays of energy less than Cj^^x-Within the superrelativistic approximation, these conclusions may be valid for the relativistic injection of neutral plasma of any composition, Care must be exercised in drawing far-reaching quantitative conclusions from our plane-wave model. Dependences on the azimuthal and polar angles in spherical geometry have been ignored. Furthermore, for a plane wave to be a good approximation, the radial excursion D of a particle during a half-period ?7 = TT, D = {TTC/Q)P/{^^ ~ 1), should be smaller than the radial scale length. This is only marginally satisfied at the injection radius and even less well at larger radii. Clearly, investigation of the spherical wave is called for.We acknowledge discussions with P. K.
The slope b (s) of the forward diffraction peak of p-p elastic scattering has been measured in the momentum-transfer-squared range 0.005^ U i^ 0.09 (GeV/c) 2 and at incident proton energies from 8 to 400 GeV. We find that b(s) increases with s, and in the interval 100^s^750 (GeV) 2 it can be fitted by the form b (s) =b 0 +2a' Ins with 6 0 = 8.23 ±0.27, a' =0.278 ± 0.024 (GeV/c)" 2 .
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