Supernova remnants
Supernova remnants, shocks and energetic particles
The original flash fades, but moving ejecta keep driving shocks. Start with why remnants shine, build the gas and particle pictures, then calculate independent benchmarks and read a fixed frontier paper.
L1
Why supernova remnants keep shining
An explosion ends quickly, but its fast-moving debris keeps driving shocks. Hot gas and energetic particles then produce different kinds of light.
L1
How a strong shock turns motion into heat
Derive the density, speed and pressure jumps from conserved fluxes, then calculate the temperature with the electron-ion assumption stated.
L2
Two shocks and a separate point explosion
Build the ejecta-envelope similarity law, match the two shells at their contact and compare a separately integrated Sedov–Taylor benchmark.
L3
Energetic seeds gain momentum one mean cycle at a time
Derive the competition between mean gain and escape, give prescribed Bohm diffusion a physical clock and stop a passive short-window model honestly.
L3
Recalculate a point blast and read the fixed HESS 2004 spectrum
Run independent Python physics offline, then inspect one exact historical photon table, its units, fit approximations and preserved chi-square failures.
L4
Read the upstream X-ray hotspots before inferring a magnetic field
Follow the fixed 2026 paper from selected X-ray spots and projected profiles to conditional diffusion, magnetic-field and acceleration estimates.
Sources and calculation scope
- Chevalier (1982), Self-similar solutions for the interaction of stellar ejecta with an external medium, ApJ258,790–797
Original complete text and printed equations/Table1. Separate cold spherical Euler shells, n>5 envelope phase; no continuation through the core or arbitrary shocked-density interpolation.
- Bell (1978), The acceleration of cosmic rays in shock fronts—I, MNRAS182,147–156
Complete original read; parallel leading-order gain, escape and transport from equations3,7,10. Prescribed scattering centres follow the gas. The printed oblique equation29 inconsistency is retained in scientific notes and that expression is not adopted. Section3, printed151–154, is read conceptually for resonant wave growth and ion–neutral damping; no nonlinear gas-feedback or damping solver is claimed.
- Leahy & Williams (2017), A Python Calculator for Supernova Remnant Evolution, arXiv1701.05942v2
Selected sections3.2.1/3.3.3 and printed coefficient on page16. The own Euler point-blast integral is independently recalculated; only these source sections, not the complete paper, are claimed read. TM99 full text was not acquired.
- Aharonian et al. (2006), A detailed spectral and morphological study of RX J1713.7−3946 with HESS, astro-ph/0511678v2
Fixed historical 2004 whole-remnant Figure12, sections2.5.2/3.2 and Table1. Selected original methods/results read; no original event/response reconstruction. Both point-centre and finite-bin chi-square comparison failures are retained.
- Official HESS auxiliary page for the historical Figure12 whole-remnant spectrum
Exact9734-byte HTML, complete SHA in the reader setup;25 named high-level photon rows. Optional reader acquires it locally. Original table and observation-derived plots are not redistributed.
- Kawabata, Tanaka, Suzuki & Inoue (2026), upstream magnetic amplification and the acceleration limit, arXiv2610.16296v1
Fixed12October2026 version, all17pages read and critical printed Figures/equations viewed. Main Figures1–4, Supplementary Figures1–2 and methods equations2–7. Selected spots and projected decline precede the conditional emission/diffusion interpretation.
- Communications Physics, DOI10.1038/s42005-026-02906-y, official early-publication metadata
Published8October2026; early peer-reviewed accepted version subject to further edits, not automatically the final Version of Record. Publisher states CC-BY4 with third-party exceptions. No original figure or paper is bundled here.
- Sandbox Physics independent supernova-remnant Python science reader
Own offline Euler n7/n12, independent zero-ejecta point blast, mean cohorts, angle/first-passage/Jensen checks and synthetic plots. Recalculates fresh coefficients and all default steps; original papers/data and app/Engine code excluded.