Supercomputer simulations provide a better picture of the sun's magneticfield NatureAstronomy
Magnetic fields on small scales are ubiquitous in the Universe. Although they can often be observed in detail, their generation mechanisms are not fully understood. One possibility is the so-called small-scale dynamo . Prevailing numerical evidence, however, appears to indicate that an SSD is unlikely to exist at very low magnetic Prandtl numbers such as those that are present in the Sun and other cool stars.
Contrary to earlier findings, the SSD not only turns out to be possible for Prbelow about 0.05. We relate this behaviour to the known hydrodynamic phenomenon referred to as the bottleneck effect. Extrapolating our results to solar values of PrAstrophysical flows are considered to be susceptible to two types of dynamo instability. First, a large-scale dynamo is excited by flows exhibiting helicity, or more generally, lacking mirror symmetry, due to rotation, shear and/or stratification.
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