Effective potential at finite temperature in a constant hypermagnetic field: Ring diagrams in the standard model

Abstract

We study the symmetry breaking phenomenon in the standard model during the electroweak phase transition in the presence of a constant hypermagnetic field. We compute the finite temperature effective potential up to the contribution of ring diagrams in the weak field, high temperature limit and show that under these conditions, the phase transition becomes stronger first order.

Phase diagram for charged scalars in a magnetic field at finite temperature

“…(20), (22) and (31) which yields In order that the one-loop correction to the vacuum energy for qB = 0 preserves the tree-level values of v 0 as well as the sigma field mass, we implement the stability conditions introducing two finite constants δµ 2 and δλ in such a way that…”

“…Peripheral collisions of heavy nuclei at high energies, neutron stars and even the early universe are examples of systems where magnetic fields can help catalyze the deconfinement/chiral restoration [1][2][3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18], the superfluid [19] and the electroweak phase transitions [20,21], respectively. Lattice simulations have also recently paid attention to the QCD phase structure in the presence of magnetic fields.…”

Symmetry restoration at finite temperature with weak magnetic fields

“…(24). This means that in general, these self-energies can be written as linear combinations of nine independent structures [43,44].…”

“…In a recent work [24], the development of the EWPT in the MSM from the symmetric phase has been studied in the presence of a weak external hypermagnetic field up to the contribution of ring diagrams. The main result from that work is that the presence of the field strengthens the first order nature of the phase transition.…”

A non-perturbative study of the evolution of cosmic magnetised sources

“…In the above mentioned articles on early times cosmological magneto-genesis the dynamics of the magnetic interaction in the cosmic fluid is examined by means of a variety of techniques and theoretical frameworks depending on the specific transition: numerical simulations, Kinetic Theory, Statistical Mechanics, or gauge invariant vector perturbations over a spatially flat FLRW background (see details in [8,9,10,11], see other approaches to primordial magnetism in [17,18,19]). However, a classical Maxwellian electromagnetic interaction (not necessarily restricted to early cosmic times) can also be incorporated into the full dynamics of General Relativity through an elegant first order system based on covariant objects defined in a 4-velocity frame (the 1+3 formalism [9,20,21]).…”