Data for: Response Function Generation for Cerenkov Radiation Production and Transport in a TRIGA Coolant Channel

Published: 31-03-2020| Version 1 | DOI: 10.17632/w2wm38jyc9.1
Jason Hearne


The attached table shows the correlation factors for the amount of visible Cerenkov radiation observed 2m above the core midplane produced by electrons in a segment with energies within a specified range. Only electrons within the segment and energy range contribute to the Cerenkov total for each factor. A separate MCNP deck was run for each energy bin and spatial bin, such that electrons are spawned in the region with an energy distribution in the energy bin and electrons that leave the region or drop below the energy cutoff of the bin are killed. The method of obtaining the factors is described the section of the article labeled: Electron to Cerenkov Flux Response Function Generation. The segment number and the z position of the upper bound and lower bound of each segment are shown in the first 3 columns. The minimum and maximum energy for each electron energy bin are shown the fourth and fifth columns. The sixth column, labeled P_flux/E_flux, shows the ratio of the photon flux 2m above the core caused by electrons in the segment and energy bin to the flux of electrons in that bin. The seventh column has the relative Monte Carlo uncertainty, which is the uncertainty obtained by propagating the uncertainties output from MCNP for the photon flux and electron flux. The bottommost (segment 1) and topmost (segment 16) segments were not run correctly in the simulations due to the geometrical cutoff. These two segments instead use duplicated data for the E_flux/P_flux from segments 2 and 15. This adds a very little error when implemented because the difference between neighboring segments is small, and the contribution of the end segments to the total is a small portion of the whole, due to the lower gamma and electron fluxes further from the core midplane.