A. de Almeida | Searcharxiv

arXiv2018

Calculation of molecular line intensity in stellar atmospheres

Molecular line intensity calculations are not a straightforward task. We present a description of the basics for including molecular linesin synthetic spectra, and of the input data needed. We aim both at describing ways in which molecular lines are computed in the context of photospheres of F-G-K stars, and to present a new online available version of our code for spectrum synthesis of cool stars. We apply calculations to molecular bands in the ultraviolet, visible and near-infrared main features, and comparisons with spectra of reference stars are shown. We provide user-friendly tools for the free use of the code PFANT. The code is available at http://trevisanj.github.io/PFANT.

astro-ph.SR↗

arXiv2007

Application of Macro Response Monte Carlo method for electron spectrum simulation

During the past years several variance reduction techniques for Monte Carlo electron transport have been developed in order to reduce the electron computation time transport for absorbed dose distribution. We have implemented the Macro Response Monte Carlo (MRMC) method to evaluate the electron spectrum which can be used used as a phase space input for others simulation programs. Such technique uses probability distributions for electron histories previously simulated in spheres (called kugels). These probabilities are used to sample the primary electron final state, as well as the creation secondary electrons and photons. We have compared the MRMC electron spectra simulated in homogeneous phantom against the Geant4 spectra. The results showed an agreement better than 6% in the spectra peak energies and that MRMC code is up to 12 times faster than Geant4 simulations.

physics.med-ph↗