Global configuration of a magnetic cloud

AbstractThe primitive ontology approach to quantum mechanics seeks to account for quantum phenomena in terms of a distribution of matter in three-dimensional space (or four-dimensional spacetime) and a law of nature that describes its temporal development. This approach to explaining quantum phenomena is compatible with either a Humean or powerist account of laws. In this paper, I offer a powerist ontology in which the law is specified by Bohmian mechanics for a global configuration of particles. Unlike in other powerist ontologies, however, this law is not grounded in a structural power that is instantiated by the global configuration. Instead, I combine the primitive ontology approach with Aristotle’s doctrine of hylomorphism to create a new metaphysical model, in which the cosmos is a hylomorphic substance with an intrinsic power to choreograph the trajectories of the particles.

Download Full-text

Flux rope axis geometry of magnetic clouds deduced from in situ data

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313011071 ◽

2013 ◽

Vol 8 (S300) ◽

pp. 265-268

Author(s):

Miho Janvier ◽

Pascal Démoulin ◽

Sergio Dasso

Keyword(s):

Interplanetary Medium ◽

Magnetic Cloud ◽

Flux Rope ◽

Magnetic Clouds ◽

Direct Integration ◽

Axis Orientation ◽

In Situ Data ◽

Geometrical Features ◽

Wide Range

AbstractMagnetic clouds (MCs) consist of flux ropes that are ejected from the low solar corona during eruptive flares. Following their ejection, they propagate in the interplanetary medium where they can be detected by in situ instruments and heliospheric imagers onboard spacecraft. Although in situ measurements give a wide range of data, these only depict the nature of the MC along the unidirectional trajectory crossing of a spacecraft. As such, direct 3D measurements of MC characteristics are impossible. From a statistical analysis of a wide range of MCs detected at 1 AU by the Wind spacecraft, we propose different methods to deduce the most probable magnetic cloud axis shape. These methods include the comparison of synthetic distributions with observed distributions of the axis orientation, as well as the direct integration of observed probability distribution to deduce the global MC axis shape. The overall shape given by those two methods is then compared with 2D heliospheric images of a propagating MC and we find similar geometrical features.

Download Full-text

Effect of solar wind velocity on magnetic cloud-associated magnetic storm intensity

Journal of Geophysical Research Atmospheres ◽

10.1029/2002ja009396 ◽

2002 ◽

Vol 107 (A11) ◽

Cited By ~ 43

Author(s):

Chin-Chun Wu

Keyword(s):

Solar Wind ◽

Magnetic Storm ◽

Wind Velocity ◽

Solar Wind Velocity ◽

Magnetic Cloud ◽

Storm Intensity

Download Full-text

Main Cause of the Poloidal Plasma Motion Inside a Magnetic Cloud Inferred from Multiple-Spacecraft Observations

Solar Physics ◽

10.1007/s11207-017-1077-4 ◽

2017 ◽

Vol 292 (4) ◽

Cited By ~ 8

Author(s):

Ake Zhao ◽

Yuming Wang ◽

Yutian Chi ◽

Jiajia Liu ◽

Chenglong Shen ◽

...

Keyword(s):

Magnetic Cloud ◽

Plasma Motion ◽

Multiple Spacecraft

Download Full-text

Specific interplanetary conditions for CIR-, Sheath-, and ICME-induced geomagnetic storms obtained by double superposed epoch analysis

Annales Geophysicae ◽

10.5194/angeo-28-2177-2010 ◽

2010 ◽

Vol 28 (12) ◽

pp. 2177-2186 ◽

Cited By ~ 57

Author(s):

Yu. I. Yermolaev ◽

N. S. Nikolaeva ◽

I. G. Lodkina ◽

M. Yu. Yermolaev

Keyword(s):

Large Scale ◽

Geomagnetic Storms ◽

Magnetic Cloud ◽

Magnetic Storms ◽

Main Phase ◽

Corotating Interaction Region ◽

Superposed Epoch Analysis ◽

Epoch Analysis ◽

Archive Data ◽

Scale Types

Abstract. A comparison of specific interplanetary conditions for 798 magnetic storms with Dst <−50 nT during 1976–2000 was made on the basis of the OMNI archive data. We categorized various large-scale types of solar wind as interplanetary drivers of storms: corotating interaction region (CIR), Sheath, interplanetary CME (ICME) including both magnetic cloud (MC) and Ejecta, separately MC and Ejecta, and "Indeterminate" type. The data processing was carried out by the method of double superposed epoch analysis which uses two reference times (onset of storm and minimum of Dst index) and makes a re-scaling of the main phase of the storm in a such way that all storms have equal durations of the main phase in the new time reference frame. This method reproduced some well-known results and allowed us to obtain some new results. Specifically, obtained results demonstrate that (1) in accordance with "output/input" criteria the highest efficiency in generation of magnetic storms is observed for Sheath and the lowest one for MC, and (2) there are significant differences in the properties of MC and Ejecta and in their efficiencies.

Download Full-text