Giant magnetospheres in our solar system: Jupiter and Saturn compared

Krupp, N.

doi:10.1007/s00159-014-0075-x

Cited by 2 publications

(1 citation statement)

References 81 publications

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“…In most cases, the source of their magnetic flux is convection in liquid or metallic cores, an effect known as a planetary dynamo [34]. Gas giants can have large magnetospheres and generate relatively strong magnetic fluxes [35]. Equatorial magnetic flux density of Jupiter is reported as 4.17 × 10 −4 T, with maximum values on the surface reaching 2 × 10 −3 T [36].…”

Section: Introductionmentioning

confidence: 99%

Calculation of a magnetic force acting on small superconducting celestial bodies

Tomkow

2021

Eur. Phys. J. Plus

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Recent discoveries of superconducting phases in the samples of meteorites suggest the possibility of a natural occurrence of superconducting state in space. Superconductors are known to exhibit interesting behaviours when subjected to external magnetic fields, such as levitation. Similar force may act on a superconducting bit in space. The goal of this paper is to quantify this force and assess its effects. Several scenarios in which a superconducting bit can be produced and interact with a magnetic field in space are suggested. The force acting on a superconductor in different conditions is calculated with numerical simulations. The dependence on a magnetic flux density, its gradient, and the geometry and the properties of the superconductor are found. The empirical formulas are derived and used to calculate a magnetic force. The resultant force is extremely weak in all analysed scenarios. It is found that its strength decreases rapidly with the distance from the source of the magnetic flux. Its effect on trajectory of the superconductor is almost negligible. Some possibilities of increasing its strength and the effects are considered.

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Section: Introductionmentioning

confidence: 99%

Calculation of a magnetic force acting on small superconducting celestial bodies

Tomkow

2021

Eur. Phys. J. Plus

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Understanding Space Weather: Part III: The Sun’s Domain

Strong

Viall

Schmelz

et al. 2017

Bulletin of the American Meteorological Society

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The Sun exports a continuous outflow of plasma into interplanetary space: the solar wind. The solar wind primarily comprises two components: high- and slow-speed flows. These move with velocities ranging from 200 to 800 km s-1 depending on the source of the particular flow. As well as its speed, the density, temperature, and even the composition of the solar wind change. Adding to its intrinsic variability, there are embedded transients resulting from flares and coronal mass ejections that further complicate its dynamics and space weather impacts. The solar wind interacts differently with each of the solar system objects it encounters based on their magnetic and atmospheric properties. Even more complex processes occur as the solar wind encounters the interstellar medium, at the outer boundaries of the Sun’s domain. The solar wind stretches to beyond 100 au (where 1 au ≡ 149 597 870 700 m) from the Sun, which means that Earth is essentially immersed in the very hot solar atmosphere, and that leads to many space weather impacts on life and society. The specific space weather impacts on Earth will be discussed in detail in the next two papers in this series.

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Giant magnetospheres in our solar system: Jupiter and Saturn compared

Cited by 2 publications

References 81 publications

Calculation of a magnetic force acting on small superconducting celestial bodies

Calculation of a magnetic force acting on small superconducting celestial bodies

Understanding Space Weather: Part III: The Sun’s Domain

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