Abstract
Abstract Data are presented over a wide range of impact energies describing the ionization or stripping probability, projectile energy loss, and ejected electron and recoiling target energies and angles for proton and hydrogen passage through hydrogen astrophysical environments. These kinematic and reaction data are tabulated at three levels of detail for use in heavy-particle (H+, H) and secondary-electron transport simulations: (1) the integral scattering cross section and average values of the distributions of energy and angle of the particles, (2) the singly differential cross sections as a function of particle energy and angle, and (3) a subset of the many possible doubly differential cross sections as functions of the particle energy and angle chosen to be most relevant to transport simulations.
Highlights
The creation and use of models of astrophysical environments, as well as the interpretation of astrophysical observations, requires a significant amount, quality, and detail of information from laboratory astrophysics
We find that the energy loss given by Equation (2) provides a numerically less “noisy” value, owing to the inherent numerical errors in the integration of the equations of motion of the particles in the classical trajectory Monte Carlo (CTMC) method
The comprehensiveness required for modeling necessitates inclusion of data for the full range of impact energies considered even if results for the differential cross sections at the lowest energies cannot be benchmarked in this way or calculated without use of normalization to the total cross section that constrains them
Summary
The creation and use of models of astrophysical environments, as well as the interpretation of astrophysical observations, requires a significant amount, quality, and detail of information from laboratory astrophysics. Prominent examples include spectral lines and transition probabilities and electron, proton, and heavier-particle collision data. Availability of such data enables modeling of astrophysical emission and absorption, energy, momentum, and particle transport, as well as reactions. Data for H+ + H and H + H in the literature, for the most part, have been largely incomplete with regard to coverage of relevant impact energies, reaction channels, and kinematics (e.g., availability of the cross-section differential in the scattering angle or energy loss of the projectile). Here, and in previously published work, we seek to make available data that are as comprehensive as currently feasible for collisions relevant to ISM shocks, supernova remnants and bubbles, H I clouds, young stellar objects, winds within stellar spheres, and other astrophysical environments. We add to the reactions considered by treating ionization of H by protons and H, as well as stripping (i.e., projectile ionization) of H by H impact
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