Coronal heating problem solution by means of axion origin photons

In this paper we advocate for the idea that two seemingly unrelated mysteries with almost 90 year history – the nature of dark matter and the million-degree solar corona – may be but two sides of the same coin – the axions of dark matter born in the core of the Sun and photons of axion origin in the million-degree solar corona, whose modulations are controlled by the anticorrelated modulation of the asymmetric dark matter (ADM) density in the solar interior. It is shown that the photons of axion origin, that are born in the almost empty magnetic flux tubes (with B∼107G) near the tachocline and then pass through the photosphere to the corona, are the result of the solar corona heating variations, and thus, the Sun luminosity variations. Since the spectrum of the incident photons of axion origin is modulated by the frequency dependence of the cross-section, then, first, the energy distribution of the emitted axions is far from being a blackbody spectrum, and second, for a typical solar spectrum, the maximum of the differential axion flux occurs at the average axion energy is 〈Ea∕T〉≈4.4 (Raffelt, 1986). This means that the average energy of the photon of axion origin can generate a temperature of the order of Ta∼1.11⋅107K under certain conditions of coronal substances, which is close to the temperature Tcore∼1.55⋅107K of the Sun core. As a result, the free energy accumulated by the photons of axion origin in a magnetic field by means of degraded spectra due to multiple Compton scattering, is quickly released and converted into heat and plasma motion with a temperature of ∼4⋅106K at maximum and ∼1.5⋅106K at minimum of solar luminosity. Since the photons of axion origin are the result of the Sun luminosity variations, then, unlike the self-excited dynamo, an unexpected but simple question arises: is there a dark matter chronometer hidden deep in the Sun core? A unique result of our model is the fact that the periods, velocities and modulations of S-stars are the fundamental indicator of the modulation of the ADM halo density in the fundamental plane of the Galaxy center, which closely correlates with the density modulation of the baryon matter near the SMBH. If the modulations of the ADM halo at the GC lead to modulations of the ADM density on the surface of the Sun (through vertical density waves from the disk to the solar neighborhood), then there is an “experimental” anticorrelation identity between the indicators, e.g. the modulation of the ADM density in t