A phenomenological model of magnetic flux tubes in strong fields induced by axion-origin photons

TL;DR

This paper introduces a phenomenological model linking axion physics to magnetic flux tubes in the Sun, explaining sunspot formation and coronal heating through axion-photon conversions and dark matter interactions, with results matching helioseismological data.

Contribution

It presents a novel model connecting axion physics and solar magnetic flux tubes, supported by theoretical estimates and observational constraints.

Findings

Velocities and rise times of magnetic flux tubes match helioseismological data.

Model predicts axion-related modulations correlated with solar activity cycles.

Provides testable predictions linking axion physics to solar phenomena.

Abstract

We propose a phenomenological model in which empty flux tubes in strong magnetic fields are associated with both the conversion of axions to photons of axion origin to generate coronal heating, and the simultaneous preservation of the Parker-Biermann cooling effect by converting high-energy photons from the radiative zone to axions from the convective zone through the O-loop tachocline, is the source of the rise of the magnetic flux tube from the tachocline to the photosphere in the form of sunspots. The model is characterized by two free parameters, justified by existing theoretical and observational constraints, the axion mass m_a ~3.2*10^{-2} eV, and asymmetric dark matter (ADM) with a particle mass m_ADM ~5 GeV gravitationally captured by the Sun. In this scenario, temporal modulations of the axion density are caused by anticorrelated 11-year modulations of ADM gravitationally captured by the Sun. We also obtained theoretical estimates of the velocities and times in empty magnetic tubes in strong fields rising from the tachocline to the surface of the photosphere in the form of sunspots. This ensured complete agreement with known experimentally measured velocities and times using local helioseismological time-distance inversions along the ray trajectories of acoustic waves. This allows us to study not only the subsurface structure and dynamics of active regions, but also the depths of the empty magnetic flux tube, extending up to 200,000 km from the tachocline to the photosphere. The proposed model links the phenomenology of axions with the magnetic structures of the Sun and provides testable consequences for astrophysical and solar observations.