Symmetries of Magnetic Fields Driven by Spherical Dynamos of Exoplanets and Their Host Stars

Sokoloff, Dmitry; Malova, H. V.; Yushkov, E. V.

doi:10.3390/sym12122085

Cited by 6 publications

(6 citation statements)

References 64 publications

(78 reference statements)

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“…Comparison of the left and right panels in Figure 3 shows that the mixing of the dipole and quadrupole components is the reason of the formation of the magnetic field asymmetry in the Northern and Southern hemispheres. This conclusion is also consistent with other investigations [70,71].…”

Section: Description Of the Solar Wind Structures In The Framework Of...supporting

confidence: 94%

Ulysses Flyby in the Heliosphere: Comparison of the Solar Wind Model with Observational Data

et al. 2022

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A model capable of reproducing a set of solar wind parameters along the virtual spacecraft orbit out of an ecliptic plane has been developed. In the framework of a quasi-stationary axisymmetric self-consistent MHD model the spatial distributions of magnetic field and plasma characteristics at distances from 20 to 1200 Solar radii at almost all solar latitudes could be obtained and analyzed. This model takes into account the Sun’s magnetic field evolution during the solar cycle, when the dominant dipole magnetic field is replaced by the quadrupole one. Self-consistent solutions for solar wind characteristics were obtained, depending on the phase of the solar cycle. To verify the model, its results are compared with the observed characteristics of solar wind along the Ulysses trajectory during its flyby around the Sun from 1990 to 2009. It is shown that the results of numerical simulation are generally consistent with the observational data obtained by the Ulysses spacecraft. A comparison of the model and experimental data confirms that the model can adequately describe the solar wind parameters and can be used for heliospheric studies at different phases of the solar activity cycle, as well as in a wide range of latitudinal angles and distances to the Sun.

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Section: Description Of the Solar Wind Structures In The Framework Of...supporting

confidence: 94%

Ulysses Flyby in the Heliosphere: Comparison of the Solar Wind Model with Observational Data

et al. 2022

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“…After reaching the Alfvén surface, these current sheets propagate in almost unchanged state over the whole astrosphere, therefore determining the peculiarities of its large scale structure. As a result, the formation of a large-scale current system takes place in accordance with the dominating kind of the stellar multipole magnetic field and its symmetric or asymmetric distribution in the northern and southern hemispheres of the stars (Sokoloff, Malova, and Yushkov, 2020;Maiewski et al, 2020). The evolution of stellar current sheets may also be fundamentally different from what we observe in the solar system.…”

Section: Discussionmentioning

confidence: 63%

“…It should be mentioned that the relation of the structure and dynamics of solar/stellar magnetic fields with the dynamo processes inside them has not been studied well. The most consistent earlier publications were presented recently by Maiewski et al (2020) and Sokoloff, Malova, and Yushkov (2020). While these results were investigated mostly in theory, in practice the Zeeman-Doppler imaging studies appeared as a useful and available tools to investigate the structure and evolution of stellar magnetic fields (Babcock, 1958;Borra and Deschatelets, 2015;Linsky and Schöller, 2015).…”

Section: Introductionmentioning

confidence: 85%

“…Therefore the position and shape of the large-scale heliospheric current sheet in the whole heliosphere can carry the information about its origin in the interior of the Sun. Recently the role of large-scale current sheets as tracers of the internal Sun's magnetic field and dynamo processes was proposed and discussed by Sokoloff, Malova, and Yushkov (2020).…”

Section: Introductionmentioning

confidence: 99%

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Migrating Dynamo Waves and Consequences for Stellar Current Sheets

et al. 2022

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We study the relation between stellar dynamo-wave propagation and the structure of the stellar magnetic field. Modeling dynamo waves by the well-known Parker migratory dynamo, we vary the intensity of dynamo drivers in order to obtain activity-wave propagation toward the Equator (as in the solar-activity cycle) or towards the Poles. We match the magnetic field in the dynamo active shell with that in the surrounding stellar material, using a simple dissipativ magnetohydrodynamic system for the transition region. Introducing E. Yushkov

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“…An important property of exoplanets and their host stars may be the presence or absence of the intrinsic magnetic field associated with possible dynamo processes in the liquid conducting cores of rotating bodies (Sokoloff et al 2020), which is of great interest to theorists (see Choudhuri 1990;Baliunas et al 1996;Brandenburg & Subramanian 2005;Rüdiger & Hollerbach 2006;Stepanov et al 2006;Winn & Fabrycky 2015;Santos 2018;Cauley et al 2019;Deleuil et al 2020, and references therein). There are many works suggesting that exoplanets have a magnetic field (see Turner et al 2021 and references therein).…”

Section: Introductionmentioning

confidence: 99%

Impact of Heavy Ions on the Structure of Current Sheets in the Gravity Field of Exoplanets and Stars

Kislov

Malova

Khabarova

et al. 2023

ApJ

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Boundary current sheets (CSs) can be formed in collisionless space plasmas in the environment of exoplanets and cold stars. Usually they represent curved surfaces carrying the electric current analogous to the well-known planetary ionospheres, magnetopauses, or stellar coronas surrounding celestial bodies. At smaller local scales, some of them can be imagined as planar current layers of a finite scale located parallel to the surface of a celestial object and, correspondingly, perpendicular to the direction of the gravitational force. In some cases, this force crossed with magnetic field can influence the dynamics of charged particles in CSs and substantially change the structure of both the current layer and the magnetic field. We have generalized our prior model, taking into account a multi-ion plasma composition and a magnetic field configuration with a shear. It is shown that, due to the drift motion of plasma particles in the crossed gravitational and magnetic fields, the structure of CSs becomes more complex, accruing asymmetric and shifted profiles of the current and plasma densities that depend on dominating current carriers and the characteristics of the magnetic shear. We discuss possible applications of the results to the interpretation of observations of boundary layers in different space plasmas.

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Symmetries of Magnetic Fields Driven by Spherical Dynamos of Exoplanets and Their Host Stars

Cited by 6 publications

References 64 publications

Ulysses Flyby in the Heliosphere: Comparison of the Solar Wind Model with Observational Data

Ulysses Flyby in the Heliosphere: Comparison of the Solar Wind Model with Observational Data

Migrating Dynamo Waves and Consequences for Stellar Current Sheets

Impact of Heavy Ions on the Structure of Current Sheets in the Gravity Field of Exoplanets and Stars

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