Dynamism in the solar core

Abstract

Recent results of a mixed shell model heated asymmetrically by transient increases in nuclear burning indicate the transient generation of small ‘hot spots’ inside the Sun somewhere between 0.1 and 0.2 solar radii (Wolff, 2009). Similar hot bubbles are followed by a nonlinear differential equation system with finite amplitude non-homologous perturbations which is solved in a solar model. Our results show the possibility of a direct connection between the dynamic phenomena of the solar core and the atmospheric activity. Namely, already ΔQ0 ≈ 1031 –1037 ergs initial heating is enough for a bubble to reach the outer convective zone. Actually, when a hot bubble is enveloped into a magnetic plasmoid, the maintenance of its integrity is enhanced and its surfacing facilitated. Our calculations show that a hot bubble can arrive into subphotospheric regions with ΔQfinal ≈ 1028 –1034 ergs approaching the sound speed ~10 km s-1. We point out that the developing sonic boom transforms the shock front into accelerated particle beam injected upwards into the top of loop carried out by the hot bubble above its forefront traveling from the solar interior. As a result, a new approach to explain flare energetics had arisen, which, if confirmed, may yield a favorable approach over the best-yet, until now exclusively magnetic flare models. We show that the particle beams generated by energetic deep-origin hot bubbles in the subphotospheric layers have masses, energies, and chemical compositions in the observed range of solar chromospheric and coronal flares. It is shown how the emergence of a hot bubble into subphotospheric regions offers a natural mechanism that can generate both the eruption leading to the flare and the observed coronal magnetic topology for reconnection. We show a tentative list of yet unexplained facts that our model explains, and present a list of predictions for observations, some of which are planned to be realized in the near future.