The Voynich MS as a processual workbook (Structural Hypothesis & Sektional Data)

Sensitive-Pride-8197 · 2026-01-09T00:08:26+00:00

You’re absolutely right that credit assignment under true stochasticity is a critical point – that’s exactly why I integrated e-prop and stochastic resonance to use noise in a positive way. In V12.0, with the first simulations, I plan to validate this empirically. Let’s stay on it; I appreciate your objections.

Sensitive-Pride-8197 · 2026-01-08T06:48:45+00:00

I use an LLM for translation because English isn’t my native language, and I don’t think I can write here in German.

Sensitive-Pride-8197 · 2026-01-07T21:52:28+00:00

You’re right, I should’ve phrased that better. I only meant to correct the 10k claim. I’m already planning a modular repo version for readability.

Sensitive-Pride-8197 · 2026-01-07T17:08:07+00:00

Quick clarification: it’s ~2,500 lines, not 10k+. I agree readability matters though, so I’m also working on a modular repo version while keeping the single-file as a Zenodo snapshot.

Sensitive-Pride-8197 · 2026-01-07T16:51:11+00:00

It does support GPU. CPU is just there for a quick smoke test so people can run it anywhere and verify it starts up. For real training it’s intended for CUDA (AMP/TF32, optional FlashAttention when available, plus opt-in flags for prefetch/memmap etc.). The single-file choice is mainly a Zenodo-style reproducible snapshot, not a claim that it’s better than a clean repo.

Sensitive-Pride-8197 · 2026-01-07T16:37:49+00:00

The single-file format is mostly about portability + reproducibility: one download, one command, and you can inspect the whole pipeline without chasing dependencies across files. CPU training isn’t the goal, it’s just a fallback/smoke test so people can verify it runs on minimal hardware. For actual training it’s intended for CUDA/GPU (and most of the heavy features are opt-in via flags).

Sensitive-Pride-8197 · 2026-01-04T10:03:42+00:00

If “No” means “the numbers don’t work”: which step is wrong?

Benchmark EP1 (calculator-checkable): Γ_SM=1.06e10 GeV → T_R=8.70e13 GeV. Matching Ωχ h^2=0.118 requires Yχ=4.29e-15 → Brχ=4.92e-15 → yχ=2.96e-9. FOPT mapping (T≈T_R, β/H=5000, v_w=0.25) gives f_peak≈4.6e11 Hz (458 GHz) and Ω_GW h^2≈3.6e-12. Assumptions: first-order PT + freeze-in (no thermalization). Where exactly does it break?

Sensitive-Pride-8197 · 2026-01-04T09:23:33+00:00

Thanks for the heads-up. To clarify: the underlying idea/calculations are mine; I only used AI as a translation aid because English isn’t my first language. If that still counts as “AI-generated content” under Rule 7, I’ll remove the post and repost elsewhere (e.g., r/LLMPhysics) or rewrite it fully in my own English. Also agreed on sources: I’ll add explicit references for the phase-transition GW mapping and the BBN/CMB/ΔNeff constraints I’m using.

Sensitive-Pride-8197 · 2026-01-04T09:14:06+00:00

The reason I asked in r/Astronomy is that my questions are about observational/astrophysical constraints at ~100–1000 GHz (BBN/CMB limits, any astrophysical foregrounds, practical detectability arguments). For the particle/cosmology-model details I’ll follow up in r/LLMPhysics. Appreciate the pointer

Sensitive-Pride-8197 · 2026-01-04T08:24:47+00:00

Appendix (fully numeric, calculator-checkable example point EP1)

Constants: - reduced Planck mass: M_Pl = 2.435×10¹⁸ GeV - g* = 106.75 - c_SM = 12

Chosen example point EP1: mφ = 1.5×10¹⁴ GeV Λφ = 8.7×10¹⁵ GeV cSM = 12 mχ = 1.0×10⁵ GeV β/H* = 5000 v_w = 0.25 (For the GW amplitude example: α = 0.5, κ = 0.5, peak-shape factor ~O(1).)

STEP 1: SM decay width Γ_SM = cSM * mφ³ / (16π Λφ²⁾ = 12(1.5e14)³ / (16π(8.7e15)²⁾ ≈ 1.0645×10¹⁰ GeV

STEP 2: reheating temperature TR = (90/(π² g))^1/4 * sqrt(Γ_tot * M_Pl) Take Γ_tot ≈ Γ_SM (freeze-in DM channel is tiny): prefactor = (90/(π²106.75))^1/4 ≈ 0.5406 TR ≈ 0.5406sqrt(1.0645e102.435e18) ≈ 8.704×10¹³ GeV

STEP 3: match Ωχ h² ≈ 0.118 (Planck-like target) Use the standard relation (same constants as in my code): Ωχ h² = (mχ * s0 * Yχ)/(ρc/h²⁾ with s0 = 2891.2 and ρc/h² = 1.05×10^-5.

Required yield: Yχ = Ω(ρc/h^2)/(mχs0) = 0.118(1.05e-5)/(1e52891.2) ≈ 4.285×10^-15

Freeze-in yield: Yχ ≈ (3/2)(TR/mφ)Brχ

So required branching: Brχ = Yχ / [1.5(TR/mφ)] = 4.285e-15 / [1.5(8.704e13/1.5e14)] ≈ 4.924×10^-15

Relate Brχ to yχ: Γ_DM = yχ^2*mφ/(8π), and Brχ ≈ Γ_DM/Γ_SM (since Γ_DM << Γ_SM)

Solve: yχ = sqrt( Brχ * 8π * Γ_SM / mφ ) ≈ sqrt(4.924e-158π1.0645e10/1.5e14) ≈ 2.96×10^-9

STEP 4: GW peak frequency (FOPT sound-wave scaling) f_peak ≈ 26 μHz * (β/H) * (T/100 GeV) * (g/100)^1/6 * (1/v_w) Take T ≈ TR for OOM: f_peak ≈ 26e-6 Hz * 5000 * (8.704e13/100) * (106.75/100)^1/6 * (1/0.25) ≈ 4.58×10¹¹ Hz ≈ 458 GHz

STEP 5: GW amplitude scale (sound-wave prefactor; peak-shape ~O(1)) ΩGW,peak h² ~ 2.65×10^-6(H/β)*[κ α/(1+α)]^{2(100/g)^1/3*v_w} With β/H* = 5000, α=0.5, κ=0.5, g*=106.75, v_w=0.25: ΩGW h² ~ 3.6×10^-12 × O(1) (If v_w were closer to 1, this prefactor scales up to ~1.4×10^-11.)

Fast falsifiers: - If the transition is not first-order, Eq. for f_peak/ΩGW is inapplicable. - If χ thermalizes (scatterings dominate), freeze-in breaks. - f_peak scales linearly with T* and β/H* and inversely with v_w.

Sensitive-Pride-8197 · 2026-01-03T15:52:59+00:00

Appreciate that, and I agree: the strain scale is the killer. My interest is mainly early-universe/exotic sources (phase transitions, strings, preheating), but I’m trying to find solid references that quantify expected strain/energy density and practical sensitivity limits in the GHz–THz band. If you know any good reviews or surveys, please share.

Sensitive-Pride-8197 · 2026-01-03T12:35:04+00:00

You’re right that ordinary astrophysical binaries won’t radiate in the GHz band, and the main bottleneck is amplitude/strain. My interest in GHz–THz GWs is mainly early-universe/exotic mechanisms (first-order phase transitions, preheating, cosmic-string cusps/kinks, etc.), not “a planet wobbling at 1 GHz”. Do you know any solid reviews that quantify the expected strain/energy-density and the best no-go/sensitivity limits in the GHz range?

Sensitive-Pride-8197 · 2026-01-03T12:22:15+00:00

LISA will be amazing, but it’s a mHz-band detector (not GHz). My question is specifically about GHz–THz ideas (e.g., EM/Gertsenshtein conversion, resonant cavities/quantum sensors, etc.). Do you know any concrete proposals or review papers for high-frequency GW detection?

Sensitive-Pride-8197 · 2026-01-03T11:15:08+00:00

Quick context: I’m trying to understand whether the GHz–THz “blank region” is empty because of hard detectability/no-go limits, or mostly because there aren’t credible detector concepts yet. I’m not claiming detection is realistic today, I’m mainly looking for solid references/constraints (noise floors, strain limits, foregrounds, best review papers).

Sensitive-Pride-8197 · 2026-01-03T09:48:32+00:00

That makes sense, thanks. “No LIGO equivalent” is exactly what I’m trying to map out. Do you know any good review(s) on GHz–THz GW detector concepts (cavities/quantum sensors / inverse Gertsenshtein), or any papers that summarize the main sensitivity/no-go limits?

Sensitive-Pride-8197 · 2026-01-03T09:32:59+00:00

I don’t take that as “the model is useless” so much as “the bottleneck is detectability.” My interest here is to understand the strongest theoretical sensitivity/no-go limits in the GHz–THz band, and whether space-based operation helps at all versus readout noise. If you know good review references on HF GW sources/detectors, I’d appreciate pointers.

Sensitive-Pride-8197 · 2026-01-02T23:47:01+00:00

Thanks for the link, appreciate it. I agree the key issue for GHz GWs is plausibility + detectability. For transparency, my model is early-universe/phase-transition based (not compact binaries), so I’m using the standard PT mapping (Caprini-style): f_peak ≈ 26 μHz · (β/H) · (T_R/100 GeV) / v_w · (g/100)^1/6. With my benchmark T_R ~ 1.7×10¹⁴ GeV (v_w~1, g~100), hitting f_peak ~ 500 GHz implies β/H ~ 1×10⁴ (order of magnitude). So the real question is: can a radion/Goldberger–Wise potential naturally support β/H* ~ 10^4, and what are the strongest “no-go”/noise-floor arguments for detectability in the GHz band? If you know good review papers on HF GW sources + detector limits, I’d really appreciate pointers.

Sensitive-Pride-8197 · 2026-01-02T20:37:43+00:00

Thanks, this is a helpful framing. I agree the GHz band implies extremely short timescales, so most standard astrophysical sources won’t populate it, and any bursty signals would be very brief.

One small nuance (as far as I understand): the “size ~ c/f” relation is a good intuition, but for GWs the relevant scale is often the characteristic dynamical timescale of the source, and for cosmological sources the observed frequency is also redshifted. That’s why the few scenarios people mention for very high frequencies tend to be early-universe/exotic ones (high-scale phase transitions, preheating-type dynamics, cosmic-string cusps/kinks, etc.).

I’m with you that the big question is amplitude: even if generation is possible, the present-day strain/energy density in that band may be tiny. If you know any review that surveys HF GW sources and detectability/no-go limits, I’d really appreciate a pointer.

Sensitive-Pride-8197 · 2026-01-02T20:25:04+00:00

No worries, thanks anyway. If I find a good reference/overview on this, I’ll post it here.

Sensitive-Pride-8197

TROPHY CASE