Waves Generated by Electron Beam in a Crater-Shaped Flux Rope

Understanding the nature and characteristics of high-frequency waves inside a flux rope may be important as the wave-particle interaction is important for charged-particle energization and the ensuing dissipation process. We analyze waves generated by an electron beam in a crater-shaped magnetic flux rope observed by MMS spacecraft on the dawnside tailward magnetopause. In this MMS observation, a depression of magnetic field, or a crater, of ∼100 km is located at the center of the magnetic flux rope of ∼650 km. There exist parallel and perpendicular electrostatic wave modes inside the depression of the magnetic field at the center of the flux rope, and they are distinguished by their locations and frequencies. The parallel mode exists at the center of the magnetic depression and its power spectrum peaks below Fce (electron cyclotron frequency). In contrast, the perpendicular mode exists in the outer region associated with the magnetic depression, and its power spectrum peaks near Fce. The linear analysis of kinetic instability using a generalized dispersion solver shows that the parallel mode can be generated by the electron beam of 5,000 km/s. They can thermalize electrons ≲100 eV effectively. However, the generation mechanism of the perpendicular mode is not clear yet, which requires further study.

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Estimation of the spatial structure of a detached magnetic flux rope at Mars based on simultaneous MAVEN plasma and magnetic field observations

Geophysical Research Letters ◽

10.1002/2015gl065720 ◽

2015 ◽

Vol 42 (21) ◽

pp. 8933-8941 ◽

Cited By ~ 10

Author(s):

Takuya Hara ◽

David L. Mitchell ◽

James P. McFadden ◽

Kanako Seki ◽

David A. Brain ◽

...

Keyword(s):

Magnetic Field ◽

Magnetic Flux ◽

Spatial Structure ◽

Flux Rope ◽

Field Observations ◽

Magnetic Flux Rope

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Access of Energetic Particles to a Magnetic Flux Rope from External Magnetic Field Lines

The Astrophysical Journal ◽

10.3847/1538-4357/abc622 ◽

2020 ◽

Vol 906 (1) ◽

pp. 9

Author(s):

T. Laitinen ◽

S. Dalla

Keyword(s):

Magnetic Field ◽

External Magnetic Field ◽

Magnetic Flux ◽

Flux Rope ◽

Energetic Particles ◽

Magnetic Flux Rope ◽

Field Lines

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Microwave indicator of potential geoeffectiveness and magnetic flux-rope structure of a solar active region

Solnechno-Zemnaya Fizika ◽

10.12737/szf-71202101 ◽

2021 ◽

Vol 7 (1) ◽

pp. 3-12

Author(s):

Anastasiia Kudriavtseva ◽

Ivan Myshyakov ◽

Arkadiy Uralov ◽

Victor Grechnev

Keyword(s):

Magnetic Field ◽

Active Region ◽

Magnetic Flux ◽

Neutral Line ◽

Flux Rope ◽

Coronal Magnetic Field ◽

Horizontal Magnetic Field ◽

Magnetic Flux Rope ◽

Magnetic Flux Ropes ◽

Class Flare

We analyze the presence of a microwave neutral-line-associated source (NLS) in a super-active region NOAA 12673, which produced a number of geo-effective events in September 2017. To estimate the NLS position, we use data from the Siberian Radioheliograph in a range 4–8 GHz and from the Nobeyama Radioheliograph at 17 GHz. Calculation of the coronal magnetic field in a non-linear force-free approximation has revealed an extended structure consisting of interconnected magnetic flux ropes, located practically along the entire length of the main polarity separation line of the photospheric magnetic field. NLS is projected into the region of the strongest horizontal magnetic field, where the main energy of this structure is concentrated. During each X-class flare, the active region lost magnetic helicity and became a CME source.

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Pressure enhancement associated with meridional flow in high-speed solar wind: possible evidence for an interplanetary magnetic flux rope

Annales Geophysicae ◽

10.1007/s00585-997-0137-8 ◽

1997 ◽

Vol 15 (2) ◽

pp. 137-142 ◽

Cited By ~ 6

Author(s):

C.-Y. Tu ◽

E. Marsch ◽

K. Ivory ◽

R. Schwenn

Keyword(s):

Magnetic Field ◽

Angular Distribution ◽

Magnetic Flux ◽

High Speed ◽

Electron Distribution Function ◽

Flux Rope ◽

Pressure Rise ◽

High Energy ◽

Magnetic Flux Rope ◽

Background Magnetic Field

Abstract. A sizable total-pressure (magnetic pressure plus kinetic pressure) enhancement was found within the high-speed wind stream observed by Helios 2 in 1976 near 0.3 AU. The proton density and temperature and the magnetic magnitude simultaneously increased for about 6 h. This pressure rise was associated with a comparatively large southward flow velocity component (with Vz ≈ –100 km · s–1) and magnetic-field rotation. The pressure enhancement was associated with unusual features in the electron distribution function. It shows a wide angular distribution of electron counting rates in the low-energy (57.8 eV) channel, while previous to the enhancement it exhibits a wide angular distribution of electron count rate in the high-energy (112, 221 and 309 eV) channels, perhaps indicating the mirroring of electrons in the converging field lines of the background magnetic field. These fluid and kinetic phenomena may be explained as resulting from an interplanetary magnetic flux rope which is not fully convected by the flow but moves against the background wind towards the Sun.

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The expected imprint of flux rope geometry on suprathermal electrons in magnetic clouds

Annales Geophysicae ◽

10.5194/angeo-27-4057-2009 ◽

2009 ◽

Vol 27 (10) ◽

pp. 4057-4067 ◽

Cited By ~ 4

Author(s):

M. J. Owens ◽

N. U. Crooker ◽

T. S. Horbury

Keyword(s):

Magnetic Field ◽

Magnetic Flux ◽

Pitch Angle ◽

Flux Rope ◽

Magnetic Clouds ◽

Magnetic Field Direction ◽

Magnetic Flux Rope ◽

Suprathermal Electron ◽

Angle Scattering ◽

The Magnetic Field

Abstract. Magnetic clouds are a subset of interplanetary coronal mass ejections characterized by a smooth rotation in the magnetic field direction, which is interpreted as a signature of a magnetic flux rope. Suprathermal electron observations indicate that one or both ends of a magnetic cloud typically remain connected to the Sun as it moves out through the heliosphere. With distance from the axis of the flux rope, out toward its edge, the magnetic field winds more tightly about the axis and electrons must traverse longer magnetic field lines to reach the same heliocentric distance. This increased time of flight allows greater pitch-angle scattering to occur, meaning suprathermal electron pitch-angle distributions should be systematically broader at the edges of the flux rope than at the axis. We model this effect with an analytical magnetic flux rope model and a numerical scheme for suprathermal electron pitch-angle scattering and find that the signature of a magnetic flux rope should be observable with the typical pitch-angle resolution of suprathermal electron data provided ACE's SWEPAM instrument. Evidence of this signature in the observations, however, is weak, possibly because reconnection of magnetic fields within the flux rope acts to intermix flux tubes.

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The spatial relation between EUV cavities and linear polarization signatures

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313011253 ◽

2013 ◽

Vol 8 (S300) ◽

pp. 395-396 ◽

Cited By ~ 2

Author(s):

Urszula Bak-Stȩślicka ◽

Sarah E. Gibson ◽

Yuhong Fan ◽

Christian Bethge ◽

Blake Forland ◽

...

Keyword(s):

Magnetic Field ◽

Magnetic Flux ◽

Cross Section ◽

Linear Polarization ◽

Flux Rope ◽

Spatial Relation ◽

Coronal Magnetic Field ◽

Systematic Analysis ◽

Elliptical Cross ◽

Magnetic Flux Rope

AbstractSolar coronal cavities are regions of rarefied density and elliptical cross-section. The Coronal Multi-channel Polarimeter (CoMP) obtains daily full-Sun coronal observations in linear polarization, allowing a systematic analysis of the coronal magnetic field in polar-crown prominence cavities. These cavities commonly possess a characteristic “lagomorphic” signature in linear polarization that may be explained by a magnetic flux-rope model. We analyze the spatial relation between the EUV cavity and the CoMP linear polarization signature.

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Testing a solar coronal magnetic field extrapolation code with the Titov–Démoulin magnetic flux rope model

Research in Astronomy and Astrophysics ◽

10.1088/1674-4527/16/1/015 ◽

2016 ◽

Vol 16 (1) ◽

pp. 015 ◽

Cited By ~ 2

Author(s):

Chao-Wei Jiang ◽

Xue-Shang Feng

Keyword(s):

Magnetic Field ◽

Magnetic Flux ◽

Flux Rope ◽

Coronal Magnetic Field ◽

Magnetic Flux Rope ◽

Solar Coronal

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The structure of an earthward propagating magnetic flux rope early in its evolution: comparison of methods

Annales Geophysicae ◽

10.5194/angeo-27-2215-2009 ◽

2009 ◽

Vol 27 (5) ◽

pp. 2215-2224 ◽

Cited By ~ 12

Author(s):

C. Möstl ◽

C.J. Farrugia ◽

H. K. Biernat ◽

S. A. Kiehas ◽

R. Nakamura ◽

...

Keyword(s):

Magnetic Field ◽

Magnetic Flux ◽

Flux Rope ◽

Leading Edge ◽

Ecliptic Plane ◽

Minimum Variance ◽

Axial Current ◽

Good Evidence ◽

Free Boundaries ◽

Magnetic Flux Rope

Abstract. We analyze a magnetic signature associated with the leading edge of a bursty bulk flow observed by Cluster at −19 RE downtail on 22 August 2001. A distinct rotation of the magnetic field was seen by all four spacecraft. This event was previously examined by Slavin et al. (2003b) using both linear force-free modeling as well as a curlometer technique. Extending this work, we apply here single- and multi-spacecraft Grad-Shafranov (GS) reconstruction techniques to the Cluster observations and find good evidence that the structure encountered is indeed a magnetic flux rope and contains helical magnetic field lines. We find that the flux rope has a diameter of approximately 1 RE, an axial field of 26.4 nT, a velocity of ≈650 km/s, a total axial current of 0.16 MA and magnetic fluxes of order 105 Wb. The field line twist is estimated as half a turn per RE. The invariant axis is inclined at 40° to the ecliptic plane and 10° to the GSM equatorial plane. The flux rope has a force-free core and non-force-free boundaries. When we compare and contrast our results with those obtained from minimum variance, single-spacecraft force-free fitting and curlometer techniques, we find in general fair agreement, but also clear differences such as a higher inclination of the axis to the ecliptic. We further conclude that single-spacecraft methods have limitations which should be kept in mind when applied to THEMIS observations, and that non-force-free GS and curlometer techniques are to be preferred in their analysis. Some properties we derived for this earthward– moving structure are similar to those inferred by Lui et al. (2007), using a different approach, for a tailward-moving flux rope observed during the expansion phase of the same substorm.

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Dual-spacecraft reconstruction of a three-dimensional magnetic flux rope at the Earth's magnetopause

Annales Geophysicae ◽

10.5194/angeo-33-169-2015 ◽

2015 ◽

Vol 33 (2) ◽

pp. 169-184 ◽

Cited By ~ 8

Author(s):

H. Hasegawa ◽

B. U. Ö. Sonnerup ◽

S. Eriksson ◽

T. K. M. Nakamura ◽

H. Kawano

Keyword(s):

Magnetic Field ◽

Magnetic Flux ◽

Three Dimensional ◽

Flux Rope ◽

Angle Distribution ◽

Generation Process ◽

Transfer Event ◽

Magnetic Flux Rope ◽

First Results ◽

Field Lines

Abstract. We present the first results of a data analysis method, developed by Sonnerup and Hasegawa (2011), for reconstructing three-dimensional (3-D), magnetohydrostatic structures from data taken as two closely spaced satellites traverse the structures. The method is applied to a magnetic flux transfer event (FTE), which was encountered on 27 June 2007 by at least three (TH-C, TH-D, and TH-E) of the five THEMIS probes near the subsolar magnetopause. The FTE was sandwiched between two oppositely directed reconnection jets under a southward interplanetary magnetic field condition, consistent with its generation by multiple X-line reconnection. The recovered 3-D field indicates that a magnetic flux rope with a diameter of ~ 3000 km was embedded in the magnetopause. The FTE flux rope had a significant 3-D structure, because the 3-D field reconstructed from the data from TH-C and TH-D (separated by ~ 390 km) better predicts magnetic field variations actually measured along the TH-E path than does the 2-D Grad–Shafranov reconstruction using the data from TH-C (which was closer to TH-E than TH-D and was at ~ 1250 km from TH-E). Such a 3-D nature suggests that the field lines reconnected at the two X-lines on both sides of the flux rope are entangled in a complicated way through their interaction with each other. The generation process of the observed 3-D flux rope is discussed on the basis of the reconstruction results and the pitch-angle distribution of electrons observed in and around the FTE.

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