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Note, in the animated gif image: low-energy (10TeV) proton induced shower, Earth magnetic field * 100, particle cutoff ~50GeV, black: hadrons, red: muons, orange: photons, blue: electrons.
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_____ _ _ _ _
/ ____| | | | | | | (_)
| | ___ _ __ __ _ _ __ __ _| |_ _ _| | __ _| |_ _ ___ _ __ ___
| | / _ \| '_ \ / _` | '__/ _` | __| | | | |/ _` | __| |/ _ \| '_ \/ __|
| |___| (_) | | | | (_| | | | (_| | |_| |_| | | (_| | |_| | (_) | | | \__ \
\_____\___/|_| |_|\__, |_| \__,_|\__|\__,_|_|\__,_|\__|_|\___/|_| |_|___/
__/ |
|___/
The very first full shower was simulated in CORSIKA8 today!
--> Hadrons, muons, electrons, magnetic fields. Great!!!! See animated image here
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Other topics:
* Output format for binary data: apache/parquet
* Refactoring roadmap to conclude was presented, speed testing (compile time, run time) must be part of first checks
* For tracking: important to also keep modularity here. It must be possible to change / modify tracking algorithms also later.
* In tracking and stepping in general: energy conservation and phase-space conservation are potential issues. In particular when the step-width is not constant (as it is for us). There are dedicated solvers to improve here. Lukas may have more details on this. However, it is not clear if this is relevant in the context of CORSIKA8 - probably not in general.
* for high-performance tracking in IGMF models it was observed that "tan" can be up to 50% slower than sin/cos... Quite interesting, but Augusto mentioned that maybe there is a good reason for this and tan is actually 50% better than sin/cos...
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