What Are the Implications of Domain Wall Problems in L=kρσ Interactions?

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So I have learned that an interaction term in a Lagrangian like: L= kρσ
can result in "domain wall" problems between the fields ρ and σ.

I imagine this means that it can result in particles spontaneously changing mass, spin, or some other property, violating conservation laws. Is that why this is a problem, or is there some other issue?

Is this sort of thing akin to a B-L sphaleron?

Is this in any way related to neutrino oscillation, or theoretical possibility that a muon oscillates into an electron without producing any other decay products?
 
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DuckAmuck said:
So I have learned that an interaction term in a Lagrangian like: L= kρσ
can result in "domain wall" problems between the fields ρ and σ.

I imagine this means that it can result in particles spontaneously changing mass, spin, or some other property, violating conservation laws. Is that why this is a problem, or is there some other issue?

Is this sort of thing akin to a B-L sphaleron?

Is this in any way related to neutrino oscillation, or theoretical possibility that a muon oscillates into an electron without producing any other decay products?

a very good question! or questions. Maybe @fzero has an answer.
I can only give a hint to this problem, because I'm not sure how to solve and if I'm right.

If we have a theory with a M background, then it must be covariant like in the superspace and then the Lagrangian does not contain non dynamical-fields nor Lagrange multipliers.
But I think @fzero is able to explain it much better.
 
https://arxiv.org/pdf/2503.09804 From the abstract: ... Our derivation uses both EE and the Newtonian approximation of EE in Part I, to describe semi-classically in Part II the advection of DM, created at the level of the universe, into galaxies and clusters thereof. This advection happens proportional with their own classically generated gravitational field g, due to self-interaction of the gravitational field. It is based on the universal formula ρD =λgg′2 for the densityρ D of DM...
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