Modelling the evolution of the Sun’s open and total magnetic flux. (arXiv:2103.15603v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Krivova_N/0/1/0/all/0/1">N. A. Krivova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Solanki_S/0/1/0/all/0/1">S. K. Solanki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hofer_B/0/1/0/all/0/1">B. Hofer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_C/0/1/0/all/0/1">C.-J. Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Usoskin_I/0/1/0/all/0/1">I. G. Usoskin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cameron_R/0/1/0/all/0/1">R. Cameron</a>
Solar activity in all its varied manifestations is driven by the magnetic
field. Particularly important for many purposes are two global quantities, the
Sun’s total and open magnetic flux, which can be computed from sunspot number
records using models. Such sunspot-driven models, however, do not take into
account the presence of magnetic flux during grand minima, such as the Maunder
minimum. Here we present a major update of a widely used simple model, which
now takes into account the observation that the distribution of all magnetic
features on the Sun follows a single power law. The exponent of the power law
changes over the solar cycle. This allows for the emergence of small-scale
magnetic flux even when no sunspots are present for multiple decades and leads
to non-zero total and open magnetic flux also in the deepest grand minima, such
as the Maunder minimum, thus overcoming a major shortcoming of the earlier
models. The results of the updated model compare well with the available
observations and reconstructions of the solar total and open magnetic flux.
This opens up the possibility of improved reconstructions of sunspot number
from time series of cosmogenic isotope production rate.
Solar activity in all its varied manifestations is driven by the magnetic
field. Particularly important for many purposes are two global quantities, the
Sun’s total and open magnetic flux, which can be computed from sunspot number
records using models. Such sunspot-driven models, however, do not take into
account the presence of magnetic flux during grand minima, such as the Maunder
minimum. Here we present a major update of a widely used simple model, which
now takes into account the observation that the distribution of all magnetic
features on the Sun follows a single power law. The exponent of the power law
changes over the solar cycle. This allows for the emergence of small-scale
magnetic flux even when no sunspots are present for multiple decades and leads
to non-zero total and open magnetic flux also in the deepest grand minima, such
as the Maunder minimum, thus overcoming a major shortcoming of the earlier
models. The results of the updated model compare well with the available
observations and reconstructions of the solar total and open magnetic flux.
This opens up the possibility of improved reconstructions of sunspot number
from time series of cosmogenic isotope production rate.
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