The Vector Direction of the Interstellar Magnetic Field Outside the Heliosphere

Swisdak, M.; Opher, M.; Drake, J. F.; Bibi, F. Alouani

doi:10.1088/0004-637x/710/2/1769

Cited by 146 publications

(229 citation statements)

References 45 publications

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“…This plateau is related to the region of the reconnection jets predicted by Swisdak et al (2010) and propagating flows of Alfvén waves, similar to those reported by McComas et al (1995) and Gosling et al (2011).…”

Section: Zharkova and O Khabarova: Additional Acceleration Of Solsupporting

confidence: 86%

“…For example, Swisdak et al (2010) investigated theoretically the conditions of magnetic reconnection in the heliopause and showed that the reconnection can only occur if the interstellar magnetic field points to the heliospheric field in a nearly antiparallel way; this can stabilise the process of reconnection and secure steady streams of ions from the current sheet, which induces large diamagnetic drifts in the reconnecting plasma.…”

Section: Zharkova and O Khabarova: Additional Acceleration Of Solmentioning

confidence: 99%

“…The authors managed to catch the onset of magnetic reconnection in 197 events recorded by the WIND spacecraft and to deduce that the conditions when the reconnection can start and continue to exist are dictated by two factors: the difference in plasma beta on the two sides of the current sheet, which has to be small, and the presence of a magnetic shear across the current sheet as predicted by Swisdak et al (2010).…”

Section: Zharkova and O Khabarova: Additional Acceleration Of Solmentioning

confidence: 99%

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Additional acceleration of solar-wind particles in current sheets of the heliosphere

Zharkova

Khabarova

2015

Ann. Geophys.

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Abstract. Particles of fast solar wind in the vicinity of the heliospheric current sheet (HCS) or in a front of interplanetary coronal mass ejections (ICMEs) often reveal very peculiar energy or velocity profiles, density distributions with double or triple peaks, and well-defined streams of electrons occurring around or far away from these events. In order to interpret the parameters of energetic particles (both ions and electrons) measured by the WIND spacecraft during the HCS crossings, a comparison of the data was carried out with 3-D particle-in-cell (PIC) simulations for the relevant magnetic topology (Zharkova and Khabarova, 2012). The simulations showed that all the observed particle-energy distributions, densities, ion peak velocities, electron pitch angles and directivities can be fitted with the same model if the heliospheric current sheet is in a status of continuous magnetic reconnection. In this paper we present further observations of the solar-wind particles being accelerated to rather higher energies while passing through the HCS and the evidence that this acceleration happens well before the appearance of the corotating interacting region (CIR), which passes through the spacecraft position hours later. We show that the measured particle characteristics (ion velocity, electron pitch angles and the distance at which electrons are turned from the HCS) are in agreement with the simulations of additional particle acceleration in a reconnecting HCS with a strong guiding field as measured by WIND. A few examples are also presented showing additional acceleration of solarwind particles during their passage through current sheets formed in a front of ICMEs. This additional acceleration at the ICME current sheets can explain the anticorrelation of ion and electron fluxes frequently observed around the ICME's leading front. Furthermore, it may provide a plausible explanation of the appearance of bidirectional "strahls" (field-aligned most energetic suprathermal electrons) at the leading edge of ICMEs as energetic electrons generated during a magnetic reconnection at the ICME-front current sheet.

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Section: Zharkova and O Khabarova: Additional Acceleration Of Solsupporting

confidence: 86%

Section: Zharkova and O Khabarova: Additional Acceleration Of Solmentioning

confidence: 99%

Section: Zharkova and O Khabarova: Additional Acceleration Of Solmentioning

confidence: 99%

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Additional acceleration of solar-wind particles in current sheets of the heliosphere

Zharkova

Khabarova

2015

Ann. Geophys.

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“…The modelled spectra are plotted at positions near the centre of each radial bin, as given. Swisdak et al 2010), i.e. the thickness of the heliosheath, as well as the boundary conditions assumed at the HP.…”

Section: Momentum Diffusion and Adiabatic Heatingmentioning

confidence: 99%

Modelling anomalous cosmic ray oxygen in the heliosheath

Strauss

Potgieter

Ferreira

et al. 2010

A&A

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This paper discusses a numerical modulation model to describe anomalous cosmic ray acceleration and transport in the heliosheath, the portion of the heliosphere between the termination shock and the heliopause. The model is based on the well known Parker transport equation and includes, in addition to diffusive shock acceleration at the solar wind termination shock, momentum diffusion (Fermi II, stochastic acceleration) and adiabatic heating occurring in the heliosheath together with both a latitude dependent compression ratio and injection efficiency as inferred from hydrodynamic heliospheric models. The model is applied to the study of anomalous cosmic ray oxygen, with the resulting intensities compared to recent Voyager 1 spacecraft observations in the heliosheath.Comparison shows that the model is able to very satisfactorily reproduce these observations, which includes a modulated spectral form at the termination shock and subsequent unfolding into the heliosheath. It is concluded that a combination of momentum diffusion and adiabatic heating, under certain realistic assumption of the solar wind speed in the heliosheath, form a viable re-acceleration mechanism, or continuous acceleration process, to explain the very contentious anomalous cosmic ray observations in the heliosheath.

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“…If there is also a guide field, then the combination of this and asymmetry across the current sheet can in theory suppress reconnection entirely. This is the so-called beta-shear condition (Swisdak et al 2003(Swisdak et al , 2010). This was first tested in the solar wind, where it was found that all reconnecting current sheets satisfied this condition (Phan et al 2010) and led to the conclusion that betashear is indeed a necessary (although not sufficient condition) for reconnection to occur.…”

Section: Asymmetric Plasma Conditions and Reconnection Onsetmentioning

confidence: 99%

What Controls the Structure and Dynamics of Earth’s Magnetosphere?

et al. 2014

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Unlike most cosmic plasma structures, planetary magnetospheres can be extensively studied in situ. In particular, studies of the Earth's magnetosphere over the past few decades have resulted in a relatively good experimental understanding of both its basic structural properties and its response to changes in the impinging solar wind. In this article we provide a broad overview, designed for researchers unfamiliar with magnetospheric physics, of the main processes and parameters that control the structure and dynamics of planetary magnetospheres, especially the Earth's. In particular, we concentrate on the structure and dynamics of three important regions: the bow shock, the magnetopause and the magnetotail. In the final part of this review we describe the current status of global magnetospheric modelling, which is crucial to placing in situ observations in the proper context and providing a better understanding of magnetospheric structure and dynamics under all possible input conditions. Although the parameter regime experienced in the solar system is limited, the plasma physics that is learned by studying planetary magnetospheres can, in principle, be translated to more general studies of cosmic plasma structures. Conversely, studies of cosmic plasma under a wide range of conditions should be used to understand Earth's

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The Vector Direction of the Interstellar Magnetic Field Outside the Heliosphere

Cited by 146 publications

References 45 publications

Additional acceleration of solar-wind particles in current sheets of the heliosphere

Additional acceleration of solar-wind particles in current sheets of the heliosphere

Modelling anomalous cosmic ray oxygen in the heliosheath

What Controls the Structure and Dynamics of Earth’s Magnetosphere?

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