Wookie(golf clap) scored some points and pointed out I am looking for an assessment of mass through measuring the energy required to enforce a particle’s curvature of space.

I have no idea where anyone else would start or how to measure a particle’s mass in this manner. Best I can do is look at a photon’s potential wavelengths as a basic comparison for how pliable space is at a fundamental level.

I began with the force unification energies because this just seemed to be the place to begin. There are somewhat relevant comparative energy threshold’s available for further analysing the universe’s energy boundaries with solar cycles and planetary bodies. The list I would make would be:

Mass required for core generated planetary EM fields

Mass required for fusion

Mass required for degeneration

BH mass

Each of these are curving space beyond a specific unification threshold as I understand.

Because of this I expect that the Milky Way’s disc would have boundaries that are comparative to unification thresholds due to the compression of time as Sag A is approached and solar orbits are confined to denser interactions.

While I have often heard the speed of galactic periphery’s mentioned I have not read much on the measurability of time compression between the center and wings of a galaxy. Something I would query regarding the speeds of peripheral stars involves their relative buoyancy to the heavier stars I would expect closer to Sag A. How are factors such as local time compression ruled out and DM nominated to begin with?

Postpocelipse said:

How are factors such as local time compression ruled out and DM nominated to begin with?

…. also, when a star reaches degenerative mass, what is assumed happens to it’s strong and weak fields?

if I were you I’d have a go at getting your HSC astronomy, this would most likely give you a basic starting point

Postpocelipse said:

Postpocelipse said:

How are factors such as local time compression ruled out and DM nominated to begin with?

…. also, when a star reaches degenerative mass, what is assumed happens to it’s strong and weak fields?

A further question of interest is ‘what is the result of confining EM fields to specific wavelengths? ie; what is the difference between an IR polarised field in comparison to a UV field?

Postpocelipse said:

Postpocelipse said:

Postpocelipse said:

How are factors such as local time compression ruled out and DM nominated to begin with?

…. also, when a star reaches degenerative mass, what is assumed happens to it’s strong and weak fields?

A further question of interest is ‘what is the result of confining EM fields to specific wavelengths? ie; what is the difference between an IR polarised field in comparison to a UV field?

I expect a galactic EM field of our variety would have skins like an onion. How UV/IR generation interacts locally for the galaxy’s components and globally with the universe’s field seems a basic requirement that I am not aware of having been distinguished?

A classic formula for pi has been discovered hidden in hydrogen atoms

New paper claims that the EM Drive doesn’t defy Newton’s 3rd law after all