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New determination of the production cross section for secondary positrons and electrons in the Galaxy
by Luca Orusa, Mattia Di Mauro, Fiorenza Donato and Michael Korsmeier
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Submission summary
| Authors (as registered SciPost users): | Luca Orusa |
| Submission information | |
|---|---|
| Preprint Link: | scipost_202208_00070v1 (pdf) |
| Code repository: | https://github.com/lucaorusa/positron_electron_cross_section |
| Date accepted: | 2022-09-23 |
| Date submitted: | 2022-08-25 14:57 |
| Submitted by: | Orusa, Luca |
| Submitted to: | SciPost Physics Proceedings |
| Proceedings issue: | 21st International Symposium on Very High Energy Cosmic Ray Interactions (ISVHECRI2022) |
| Ontological classification | |
|---|---|
| Academic field: | Physics |
| Specialties: |
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| Approaches: | Theoretical, Phenomenological |
Abstract
The cosmic-ray fluxes of electrons and positrons (e±) are measured with high precision by the space-borne particle spectrometer AMS-02. To infer a precise interpretation of the production processes for e± in our Galaxy, it is necessary to have an accurate descrip- tion of the secondary component, produced by the interaction of cosmic-ray proton and helium with the interstellar medium atoms. We determine new analytical functions of the Lorentz invariant cross section for the production of e± by fitting data from collider experiments. The total differential cross section dσ/dTe±(p + p → e± + X) is predicted with an uncertainty of about 5-7% in the energies relevant for AMS-02 positron flux.
Published as SciPost Phys. Proc. 13, 006 (2023)
Reports on this Submission
Report #1 by Anonymous (Referee 1) on 2022-9-20 (Invited Report)
- Cite as: Anonymous, Report on arXiv:scipost_202208_00070v1, delivered 2022-09-20, doi: 10.21468/SciPost.Report.5714
Report
This contribution provides a concise summary of more detailed work by the same authors published in Physical Review D. This work provides the most accurate evaluation of the electron and positron ($e^±$) production cross sections from proton-proton collisions. Based on this evaluation, together with other nuclei collision channels, the source terms of secondary $e^±$ flux are calculated with high precision. These results are of fundamental importance in the understanding and interpretation of recent high-precision cosmic-ray measurements.