DOE OSTI2013
The Russian-3 (R3) HANE, a 60 km high-latitude burst with yield estimated at 300 kt, was chosen for the demonstration. This test was selected because it allowed LLNL to leverage existing funding, which was directed at extending LLNL’s capability to simulate HANEs at atmospheric altitudes (<100 km). David Larsen (LLNL) developed a new particle-tracing code that tracks monoenergetic electrons of various energies from a point source as they interact with the atmosphere, losing energy and ‘pitch-angle scattering’ as they are transported. A relatively large fraction of the initial electrons are able to escape the atmosphere and were handed off to LANL for further processing to calculate the effect on space based assets. LANL binned the electrons into a phase-space density as a function of energy and equatorial pitch-angle and showed that all of the electrons would travel along field lines to the conjugate point in the Southern hemisphere, where they would likely be absorbed, because their equatorial pitch-angles were too field-aligned to permit them to ‘mirror’ above the atmosphere and be ‘trapped’. Thus, the initial LLNL output did not produce any trapped electrons to input into LANL’s diffusion code and so no study of the long-term evolution of the trapped population and its effect on space-based assets could be performed. It was recognized that LLNL’s calculation did not properly model the low-probability, large-angle scattering associated with a single Coulomb interaction between a beta-decay electron and the nucleus of the neutral particles in the high atmosphere, which would be the dominant interaction above some altitude (>100 km) and might allow the electrons to be pitch-angle scattered sufficiently to become trapped. A second LLNL calculation that properly included this single interaction probability was conducted and the output processed by LANL. It was shown that a small fraction of the initial population (~0.01%) would be ‘locally trapped’; however, even this small population would likely be absorbed within a few minutes as the electrons drifted around earth and eventually ended up on field lines where they would be absorbed in the atmosphere. The output of the second LLNL calculation was found to produce about 4x fewer backscattered electrons than previous work (Selesnick et al 2012), and so the remainder of the FY13 LANL effort on the project was aimed at trying to resolve this discrepancy. LANL implemented a stochastic differential equation to simulate the backscatter process so that the results could be compared to Larsen and Selesnick. Initial results from this capability have been obtained, but no quantitative comparison to Larsen or Selesnick has been done yet.
73 NUCLEAR PHYSICS AND RADIATION PHYSICS↗