Speaker
Description
Rotation is known to restore chiral symmetry at high angular velocities, but it is also expected that rotation can induce an axial-vector condensate. This condensate, often overlooked, can significantly alter the behavior of the chiral condensate, potentially enhancing it under rapid rotation. To investigate this interplay, we compute the phase diagram of the chiral and axial vector condensates within a NJL-model in a rigidly rotating frame in the mean field approximation.
Our results indicate that when chiral symmetry is fully restored, the axial vector condensate vanishes. Conversely, in regimes where chiral symmetry is spontaneously broken, a finite axial vector condensate emerges. Notably, at low temperatures and moderate angular velocities, the chiral condensate is enhanced in the same region where the axial vector condensate becomes finite. At high temperatures, both condensates vanish, consistent with theoretical expectations.
Our findings reveal novel phases with implications for the physics of neutron stars, where rapid rotation can generate axial vector condensates. The axial vector condensate, closely linked to magnetization, provides a compelling framework to explain the extreme magnetization observed in neutron stars.
