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Attracted by the fascinating magnetism of the Sun
Full text linkThe Sun is a quite active star, where still enigmatic phenomena characterize its life. This one is modulated at large scales by a remarkable degree of order (11-yr cycle and other superimposed cycles) even if the regenerating convective source of the whole magnetic activity is characterized by a chaotic and turbulent behavior. Several aspects of the solar magnetic activity are still not completely understood, such as the time-length of cycles, the dependency of the activity on the latitude, the actual role of the tachocline with the exact location of the dynamo regenerating sources. Here the solar dynamo problem is reviewed in the light of recent developments in theories and observations. In particular, global spherical simulations of convective dynamos and numerical experiments on Parker dynamo waves will be discussed. This latter are recently drawing a possible way for an unitary view of both large-scale and small-scale dynamo, contrary to the conventional theory that considers these as complementary approaches of the same problem: the astrophysical magnetism
An Argument in Favor of Magnetic Polarity Reversals Due to Heat Flux Variations in Fully Convective Stars and Planets
No full textLow-mass M dwarf stars, T Tauri stars, as well as planets such as the Earth and Jupiter are permeated by large-scale magnetic fields generated by the convection-driven dynamo operating in their convection zones. These magnetic fields are often characterized by a significant time variability, most prominently expressed by the inversions of their polarity, denoted as reversals, whose mechanism has not been completely understood. This work aims to gain some insights into the mechanism that generates these reversals. With this purpose, a simplified nonlinear model is developed to investigate the role played in polarity reversals by the convective heat transfer occurring in stellar and planetary convection zones. A model result is the enhancement of the global heat transport before polarity reversals, showing the crucial role that heat transport might play in their occurrence. This role is elucidated by considering that a reversal has a greater than 70% probability of occurring during a burst of convective heat transport. This high probability has been found in 94 out of 101 numerical simulations obtained by changing characteristic model parameters. Moreover, the causal relationship between the convective heat flux growth and the magnetic field variations is highlighted by the temporal antecedence of the former relative to the latter and by convergent cross mapping, namely a statistical test for detecting causality. It would thus be expected that higher levels of temporal variability in the planetary and stellar magnetic fields may be correlated to a higher heat transfer efficiency achieved in the interior of these celestial bodies
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