Jump to content
Main menu
Main menu
move to sidebar
hide
Navigation
Main page
Recent changes
Random page
freem
Search
Search
Appearance
Create account
Log in
Personal tools
Create account
Log in
Pages for logged out editors
learn more
Contributions
Talk
Editing
Openai/6897769e-4ee4-800f-aba5-69cca34f701c
(section)
Add languages
Page
Discussion
English
Read
Edit
Edit source
View history
Tools
Tools
move to sidebar
hide
Actions
Read
Edit
Edit source
View history
General
What links here
Related changes
Special pages
Page information
Appearance
move to sidebar
hide
Warning:
You are not logged in. Your IP address will be publicly visible if you make any edits. If you
log in
or
create an account
, your edits will be attributed to your username, along with other benefits.
Anti-spam check. Do
not
fill this in!
=== Assistant: Done — I ran a small, transparent numerical experiment code + table exploring Option 1 and saved the results for you to… === Done — I ran a small, transparent numerical experiment (code + table) exploring Option 1 and saved the results for you to inspect. Short summary of findings (quick, non-technical): • With the simple surface-event model and the assumptions I used, the estimated gravitational constant simplifies analytically to Gest = c5 τ22ℏG_{\rm est} \;=\; \frac{c^{5}\,\tau^{2}}{2\hbar}Gest=2ℏc5τ2 where τ\tauτ is the characteristic event time (the interval associated with each photon–electron interaction). • If you take τ\tauτ equal to the Planck time tP=ℏG/c5t_{P}=\sqrt{\hbar G/c^{5}}tP=ℏG/c5, the formula returns Gest=G/2G_{\rm est}=G/2Gest=G/2 — the right order of magnitude and only a factor 1/2 off. That is striking for such a tiny, heuristic model. • The numeric table I produced (visible in the table window) shows how GestG_{\rm est}Gest scales with τ\tauτ. As expected, Gest∝τ2G_{\rm est}\propto\tau^{2}Gest∝τ2: very short event times give tiny G estimates; longer τ\tauτ rapidly blows G up. Important caveats (please read — these matter): • This is a back-of-the-envelope toy model, not a derivation from a full relativistic Lagrangian or a rigorous matching to Einstein’s equations. I used rough flux→energy-density steps, a thin-shell approximation, and a simple curvature estimate (1/r² scale). The r-dependence cancelled in that setup — helpful for a toy estimate but not proof of a deep identity. • The factor-of-two mismatch (G/2) for τ = t_P highlights both promise and fragility: it shows the dimensional logic is on the right track, but details (order-unity factors, exact shell thickness assumptions, correct GR matching, coupling to stress-energy tensor components, quantum corrections, plasma effects, etc.) will change the numerical prefactor. If you want next steps, here are useful, practical options (pick one or more): # Tighten the model: replace the naive curvature ≈ 1/r² step with a proper weak-field solution (derive the metric perturbation from a surface stress-energy tensor and compute the effective G). I can try to do that next (longer math, but doable). # Vary modeling choices and run a parametric sweep (I can include shell thickness, different definitions of E_event, event rates other than 1/τ, etc.). # Attempt a Lagrangian-level derivation: write a toy action for a surface energy density from photon-electron events, vary to find T_{μν}, and then compare to GR's field equations (harder, but the right way to make this rigorous). # Explore physical interpretations of the factor 1/2 and where it could come from (e.g., shell thickness, two events per cycle, spin factors, choice of flux→density relation). Which of these would you like me to do next? Or do you want me to post the numeric table and the analytic note into your canvas document?
Summary:
Please note that all contributions to freem are considered to be released under the Creative Commons Attribution-ShareAlike 4.0 (see
Freem:Copyrights
for details). If you do not want your writing to be edited mercilessly and redistributed at will, then do not submit it here.
You are also promising us that you wrote this yourself, or copied it from a public domain or similar free resource.
Do not submit copyrighted work without permission!
Cancel
Editing help
(opens in new window)