Zobrazeno 1 - 10
of 924
pro vyhledávání: '"Schüßler M"'
Publikováno v:
A&A 671, A87 (2023)
The length of the solar activity cycle fluctuates considerably. The temporal evolution of the corresponding cycle phase, that is, the deviation of the epochs of activity minima or maxima from strict periodicity, provides relevant information concerni
Externí odkaz:
http://arxiv.org/abs/2301.07469
Autor:
Cameron, R. H., Schuessler, M.
Publikováno v:
A&A 636, A7 (2020)
The polarity of the toroidal magnetic field in the solar convection zone periodically reverses in the course of the 11/22-year solar cycle. Among the various processes that contribute to the removal of `old-polarity' toroidal magnetic flux is the eme
Externí odkaz:
http://arxiv.org/abs/2002.05436
Autor:
Schüssler, M., Cameron, R. H.
Publikováno v:
A&A 618, A89 (2018)
The frequency spectrum of the hemispheric asymmetry of solar activity shows enhanced power for the period ranges around 8.5 years and between 30 and 50 years. This can be understood as the sum and beat periods of the superposition of two dynamo modes
Externí odkaz:
http://arxiv.org/abs/1807.10061
Publikováno v:
A&A 609, A56 (2018)
Context. The solar dynamo consists of a process that converts poloidal field to toroidal field followed by a process which creates new poloidal field from the toroidal field. Aims. Our aim is to observe the poloidal and toroidal fields relevant to th
Externí odkaz:
http://arxiv.org/abs/1710.07126
Autor:
Cameron, R. H., Schuessler, M.
Publikováno v:
A&A 599, A52 (2017)
In 1969 Leighton developed a quasi-1D mathematical model of the solar dynamo, building upon the phenomenological scenario of Babcock(1961). Here we present a modification and extension of Leighton's model. Using the axisymmetric component of the magn
Externí odkaz:
http://arxiv.org/abs/1611.09111
Autor:
Cameron, R. H., Schuessler, M.
In order to match observed properties of the solar cycle, flux-transport dynamo models require the toroidal magnetic flux to be stored in a region of low magnetic diffusivity, typically located at or below the bottom of the convection zone. We infer
Externí odkaz:
http://arxiv.org/abs/1604.07340
A number of observational and theoretical aspects of solar magnetoconvection are considered in this review. We discuss recent developments in our understanding of the small-scale structure of the magnetic field on the solar surface and its interactio
Externí odkaz:
http://arxiv.org/abs/1511.04214
We discuss recent observational, theoretical and modeling progress made in understanding the Sun's internal dynamics, including its rotation, meridional flow, convection and overshoot. Over the past few decades, substantial theoretical and observatio
Externí odkaz:
http://arxiv.org/abs/1503.08539
Magnetic activity in Sun-like and low-mass stars causes X-ray coronal emission, which is stronger for more rapidly rotating stars. This relation is often interpreted in terms of the Rossby number, i.e., the ratio of rotation period to convective over
Externí odkaz:
http://arxiv.org/abs/1408.6175
The tilt angles of sunspot groups represent the poloidal field source in Babcock-Leighton-type models of the solar dynamo and are crucial for the build-up and reversals of the polar fields in Surface Flux Transport (SFT) simulations. The evolution of
Externí odkaz:
http://arxiv.org/abs/1406.5564