Reply [to “Comment on “Simulation study on fundamental properties of the storm‐time ring current” by Y. Ebihara and M. Ejiri”]

Ebihara, Y.; Ejiri, Masaki

doi:10.1029/2000ja000408

Cited by 7 publications

(3 citation statements)

References 2 publications

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“…The ratio of the Δ B BSI value to the Δ B DPS value is 0.934 for this location and specification of a thin shell. Ebihara and Ejiri [2000, 2001] also found similarity between the perturbation from the DPS relation and that from a Biot‐Savart integration of their model results.…”

Section: Comparisons Of δB Calculationsmentioning

confidence: 55%

Yet another caveat to using the Dessler‐Parker‐Sckopke relation

Liemohn¹

2003

J. Geophys. Res.

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[1] The analytical formulation of the Dessler-Parker-Sckopke (DPS) equation relating the energy content of the ring current to the magnetic field depression at the Earth's center is examined. To conduct this study, a method is presented for numerically integrating inner magnetospheric pressure distributions according to the Biot-Savart law to obtain magnetic field perturbations at an arbitrary location. It is found that the implicit assumption of the DPS relation requiring that all of the particle pressure is included in the integration can generate large errors relative to the true perturbation. When there is a nonzero pressure just inside the outer boundary of the integration volume, the DPS relation implicitly includes large azimuthal currents at this pressure discontinuity. By including ghost cells of adiabatically decreasing pressure beyond the outer boundary, a ''true'' perturbation from the currents within the simulation is obtained. The ratio of this corrected value to the DPS value systematically varies according to a simple pressure ratio. Other aspects of the DPS relation are also confirmed with this code, including the validity criterion imposed by the plasma pressure anisotropy and the validity of the relation for any local time asymmetry. The inclusion of closure currents in the perturbation calculation, which were not part of the DPS derivation, changes the local time profile of the perturbation and can make either a negligible or a substantial contribution in either a positive or a negative sense to the globally averaged perturbation.

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Section: Comparisons Of δB Calculationsmentioning

confidence: 55%

Yet another caveat to using the Dessler‐Parker‐Sckopke relation

Liemohn¹

2003

J. Geophys. Res.

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“…This field acts to maintain quasi-neutrality in the gas by inhibiting the outflow of electrons, which causes an outward pressure on the ions resulting in a flow of ions and electrons from the ionosphere into the magnetosphere. These particles are then distributed throughout the magnetosphere (Ebihara et al 2006) and their ultimate fates are currently a matter of debate. While some studies suggest that most escape the magnetosphere and are lost to interplanetary space (Nilsson et al 2012), others suggest that most are unable to Fig.…”

Section: Exospheres Magnetospheres and Windsmentioning

confidence: 99%

Stellar winds and planetary atmospheres

Johnstone

2021

Preprint

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Interactions between the winds of stars and the magnetospheres and atmospheres of planets involve many processes, including the acceleration of particles, heating of upper atmospheres, and a diverse range of atmospheric loss processes. Winds remove angular momentum from their host stars causing rotational spin-down and a decay in magnetic activity, which protects atmospheres from erosion. While wind interactions are strongly influenced by the X-ray and ultraviolet activity of the star and the chemical composition of the atmosphere, the role of planetary magnetic fields is unclear. In this chapter, I review our knowledge of the properties and evolution of stellar activity and winds and discuss the influences of these processes on the long term evolution of planetary atmospheres. I do not consider the large number of important processes taking place at the surfaces of planets that cause exchanges between the atmosphere and the planet's interior.

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“…Previous single-polymer and single-particle measurements have revealed a wealth of information regarding the physical and electronic structure of polymers and energy transfer dynamics, but these experiments were performed on fluorescent materials. [36][37][38][39][40][41][42][43][44][45][46][47][48][49] However, conductive films like PEDOT:PSS have polaronic states that quench fluorescence, preventing the use of fluorescence as a probe. [36] Thus, a non-fluorescence-based method of single-polymer spectroscopy must be employed.…”

mentioning

confidence: 99%

Investigating the Mechanism of Post-Treatment on PEDOT:PSS via Single-Particle Absorption Spectroscopy

Rea¹,

Pan²,

Horak³

et al. 2019

Preprint

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The conductive polymer PEDOT:PSS, widely used in optoelectronic devices, exhibits improved conductivity upon post-treatment, but the mechanism of this improvement is difficult to fully ascertain. The effects of thermal annealing and DMSO post-treatment on PEDOT:PSS, from the nano- to mesoscale, are studied using single-particle absorption spectroscopy. An average decrease in size and apparent increase in rotational order of individual particles are observed with both treatments, including unexpected correlations between change in rotational order and initial properties. Simulation of these transformations and correlations occurring during the annealing process reveal that the effects of DMSO-post treatment can be explained by oligomer depletion and do not explicitly require conformational changes including oligomer rotation.

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Reply [to “Comment on “Simulation study on fundamental properties of the storm‐time ring current” by Y. Ebihara and M. Ejiri”]

Cited by 7 publications

References 2 publications

Yet another caveat to using the Dessler‐Parker‐Sckopke relation

Yet another caveat to using the Dessler‐Parker‐Sckopke relation

Stellar winds and planetary atmospheres

Investigating the Mechanism of Post-Treatment on PEDOT:PSS via Single-Particle Absorption Spectroscopy

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