Ram pressure and returning gas
Ram pressure and returning gas
Gas can leave a galaxy disk while remaining bound. Start with its motion, then follow the wind pulse, the fuel counted inside the disk and the light of successive stellar generations.
L1
Why cluster galaxies become redder
A cluster can reduce a galaxy’s cold fuel or its future supply. Follow how fewer young blue stars change the combined light, and how dust can mimic that change.
L1
Why a galaxy tail can fall back
A cluster wind can lift gas that still belongs to its galaxy. Follow the difference between a visible tail, gravitational binding and permanent fuel loss.
L2
From a wind pulse to a restoring force
Derive ram acceleration from a gas column, compare impulse with vertical gravity, and see when a static pressure threshold is useful.
L2
Follow fuel across the disk boundary
Derive how a moving gas population changes disk star formation, while the global rate can remain identical across different wind paths.
L3
Recompute five fixed gas slices
Use an independent offline package to recompute disk mass, binding, star formation and the static restoring-force reference from five exact synthetic slices.
L3
Why global colour needs a history
Build stellar light from populations of different ages, then separate a specified shutdown, dust reddening and the location of stripped gas.
L4
Read exposure histories and multiphase tail physics
Read pressure and exposure statistics in a fixed GAEA–TNG paper, then connect their limits to cooling and magnetic fields in gas-tail research.
Independent scientific materials
Download the offline scientific ZIP · Read units and calculation scope
Python, NumPy and SciPy recompute the five fixed synthetic slices, the local static restoring-force reference and four-age global colour ratios. This package evaluates saved scientific data; original gas integration and native SSP convolution are separate calculations.
Files, sizes and SHA-256
- README.md (4173 B)
963ce7a0921c497a5556558faa685310a3ad424db826831c794f031492b7ad90 - requirements.txt (27 B)
39b93fa1b8397265839a510ca7601608248a7f3524067b61667e977bf4351475 - criterion.py (4267 B)
ab0ce3a9e95a01ca886e3a9f997e162cee4c7d9081d36c7e1cec2ae5d1c1b2e0 - recompute.py (2612 B)
47b44c4dd30ddecb64226dc6f1b0c59c6e25e769ec8e8885f38b581b77b68a5f - fixed-slices.json (82090 B)
e536102615f5fc2bfdda56b4374dc63fc0307229a0a248c6e84a7ab8ad2638ca - expected.json (19249 B)
4816379eba85e94a8477f6268b8186cba5b23f8ee2f079075cff31fcf7ef7d0e - ram-pressure-science-v1.zip (45741 B)
979dbcbd25d63a9a9f79e85f921976d051c46a57eac82f21713dee288297a2f2
Sources and calculation scope
- Köppen, Jáchym, Taylor & Palouš, Ram Pressure Stripping Made Easy, arXiv:1806.05887v1 (2018)
Sections2.1–2.2 and5.4 explain the slow-pressure/impulse limits and re-accretable gas. Our fixed three-component potential, equal-mass sheets and consuming gas are specified independently; the own static comparison does not reproduce every published simulation or observational sample.
- Xie et al., The impact of ram pressure on cluster galaxies, arXiv:2504.12863v1 / A&A 698, A73 (2025)
Fixed 17 April 2025 scientific text: sections 2.4/3.1, Figures 1–2 and 5–7. The v1 body has received/accepted placeholders; the current arXiv bibliographic page lists A&A 698, A73 and acceptance. The guide reads pressure definitions and aggregate exposure statistics; it does not join summary tables into an individual TNG trajectory.
- Gronke & Oh, The growth and entrainment of cold gas in a hot wind, arXiv:1806.02728v2 (2018)
Controlled three-dimensional cloud-in-wind cooling study. Mixed-gas cooling, material origin, downstream domain and resolution are the relevant reading questions. It is not a self-gravitating star-forming disk or a calibration of this gas-sheet model.
- Dursi & Pfrommer, Draping of Cluster Magnetic Fields over Bullets and Bubbles, arXiv:0711.0213v2 (2008)
Three-dimensional magnetic draping around an initially unmagnetized projectile, including analytic and MHD arguments. Explicit thermal conduction is omitted; a geometric heat-flow inference is distinguished from a simulated conductivity. The gas-sheet Lab does not evolve this field.
- Bruzual & Charlot, Stellar population synthesis at the resolution of 2003, astro-ph/0309134v1
Section 2.3 supplies the initially formed-mass convention and population convolution. The fixed numerical input is easyGalaxy commit 133c62b383fae964701b673e62517293161b41d5, tests/data/bc03_ssp_z_0.02_salp.model, SHA5b2e2f9f2ecdbbd329ff4993f84a5d4bd7f8bfef6877b38d2042e9a0cf96e1fd. Its Salpeter label is retained; an unspecified track release is not invented.
- Calzetti et al., The Dust Content and Opacity of Actively Star-Forming Galaxies, astro-ph/9911459v1 / ApJ533 (2000)
Empirical attenuation context for the separately specified screens. The own calculation restricts the prescription to 1200–22000 Angstrom; it does not fit a measured dust parameter or solve infrared re-emission.
- Bianconi et al., LoCuSS pre-processing in infalling galaxy groups, arXiv:1710.04230v1 (2017)
Focused primary HTML reading of sections 2–4 and Figure 2 caption: X-ray group selection, spectroscopic members, massive-galaxy cut and infrared formation threshold. The comparison is of selected populations at projected cluster radius; no object-by-object gas-loss history or causal intervention is reproduced.
- Dou, Yu & Hou, Pre-processing and protection during cluster infall, arXiv:2605.23314v1 (2026)
Fixed 22 May 2026 paper, accepted by A&A according to its bibliographic page. Focused reading: sections 2.1–2.4, 3.1–3.2, 5.3–5.5 and summary. A 25-cluster sample, full spectroscopic structure labels and 7092 mass-complete galaxies support a statistical environment comparison. Its projected infall proxy is phenomenological; pre-processing and apparent protection are distinguished from individual timing or demonstrated gas shielding.
- Original fixed-slice and static-restoring-force materials
Our five exact synthetic slices with sixty-four sheets and thirteen fields, initial common arrays, two global-light histories/three screens/four-age band subset, independent Python static maxima and mask/energy/colour diagnostics. Original trajectory and native SSP production are distinct earlier calculations; this offline package repeats diagnostics and band ratios. No browser Engine, original FITS/SED, paper, author code or observed-galaxy data is included.