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We study how active-region-scale flux tubes rise buoyantly from the base ofthe convection zone to near the solar surface by embedding a thin flux tubemodel in a rotating spherical shell of solar-like turbulent convection. Thesetoroidal flux tubes that we simulate range in magnetic field strength from 15kG to 100 kG at initial latitudes of 1 degree to 40 degrees in bothhemispheres. This article expands upon Weber, Fan, and Miesch (Astrophys. J.,741, 11, 2011) (Article 1) with the inclusion of tubes with magnetic flux of10^20 Mx and 10^21 Mx, and more simulations of the previously investigated caseof 10^22 Mx, sampling more convective flows than the previous article, greatlyimproving statistics. Observed properties of active regions are compared toproperties of the simulated emerging flux tubes, including: the tilt of activeregions in accordance with Joy's Law as in Article 1, and in addition thescatter of tilt angles about the Joy's Law trend, the most commonly occurringtilt angle, the rotation rate of the emerging loops with respect to thesurrounding plasma, and the nature of the magnetic field at the flux tube apex.We discuss how these diagnostic properties constrain the initial field strengthof the active region flux tubes at the bottom of the solar convection zone, andsuggest that flux tubes of initial magnetic field strengths of \geq 40 kG aregood candidates for the progenitors of large (10^21 Mx to 10^22 Mx) solaractive regions, which agrees with the results from Article 1 for flux tubes of10^22 Mx. With the addition of more magnetic flux values and more simulations,we find that for all magnetic field strengths, the emerging tubes show apositive Joy's Law trend, and that this trend does not show a statisticallysignificant dependence on the magnetic flux.

solar physics

Comparing Simulations of Rising Flux Tubes Through the Solar Convection  Zone with Observations of Solar Active Regions: Constraining the Dynamo Field  Strength