Plasma and energetic particle structure upstream of a quasi‐parallel interplanetary shock

Kennel, C. F.; Scarf, F. L.; Coroniti, F. V.; Russell, C. T.; Wenzel, K.‐P.; Sanderson, T. R.; Nes, P. van; Feldman, W. C.; Parks, G. K.; Smith, E. J.; Tsurutani, B. T.; Mozer, F. S.; Temerin, M.; Anderson, R. R.; Scudder, J. D.; Scholer, M.

doi:10.1029/ja089ia07p05419

Cited by 91 publications

(45 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The upstream (and downstream) waves act as two walls of a Fermi accelerator (Lee, 1983) leading to exceptional particle acceleration. Evidence of this has been demonstrated by Kennel et al 1984aKennel et al , 1984b. This microscale structure was not examined in the particle acceleration studies discussed in earlier sections.…”

Section: Shock Normal Angles and Particle Accelerationmentioning

confidence: 98%

See 1 more Smart Citation

Short-term variability of the Sun-Earth system: an overview of progress made during the CAWSES-II period

Gopalswamy

Tsurutani

Yan

2015

Prog. in Earth and Planet. Sci.

View full text Add to dashboard Cite

This paper presents an overview of results obtained during the CAWSES-II period on the short-term variability of the Sun and how it affects the near-Earth space environment. CAWSES-II was planned to examine the behavior of the solar-terrestrial system as the solar activity climbed to its maximum phase in solar cycle 24. After a deep minimum following cycle 23, the Sun climbed to a very weak maximum in terms of the sunspot number in cycle 24 (MiniMax24), so many of the results presented here refer to this weak activity in comparison with cycle 23. The short-term variability that has immediate consequence to Earth and geospace manifests as solar eruptions from closed-field regions and high-speed streams from coronal holes. Both electromagnetic (flares) and mass emissions (coronal mass ejections -CMEs) are involved in solar eruptions, while coronal holes result in high-speed streams that collide with slow wind forming the so-called corotating interaction regions (CIRs). Fast CMEs affect Earth via leading shocks accelerating energetic particles and creating large geomagnetic storms. CIRs and their trailing high-speed streams (HSSs), on the other hand, are responsible for recurrent small geomagnetic storms and extended days of auroral zone activity, respectively. The latter leads to the acceleration of relativistic magnetospheric 'killer' electrons. One of the major consequences of the weak solar activity is the altered physical state of the heliosphere that has serious implications for the shock-driving and storm-causing properties of CMEs. Finally, a discussion is presented on extreme space weather events prompted by the 23 July 2012 super storm event that occurred on the backside of the Sun. Many of these studies were enabled by the simultaneous availability of remote sensing and in situ observations from multiple vantage points with respect to the Sun-Earth line.

show abstract

Section: Shock Normal Angles and Particle Accelerationmentioning

confidence: 98%

“…It should be noted that the largest SEP events are associated with quasi-parallel shocks (Kennel et al 1984a(Kennel et al , 1984b. This is because of the presence of upstream turbulence ahead of the shocks (Tsurutani et al 1983), leading to enhanced Fermi-type acceleration across the shocks.…”

Section: Solar Cycle Effectsmentioning

confidence: 99%

Short-term variability of the Sun-Earth system: an overview of progress made during the CAWSES-II period

Gopalswamy

Tsurutani

Yan

2015

Prog. in Earth and Planet. Sci.

View full text Add to dashboard Cite

show abstract

“…But in the sheath adjacent to and upstream of a shock, particles streaming along B can excite high intensities of gyro-resonant waves, which in turn scatter the particles in pitch angle and produce the small scattering mean free paths essential for shock acceleration (Lee 2005). Figure 9 shows an example of such waves measured upstream of a quasi-parallel shock (angle θ Bn between the shock normal and B satisfies θ Bn ≤ 45 • ; Tsurutani et al 1983, see also Kennel et al 1984). The illustration sketches the occurrence of a solar flare and a CME extending a few R S from the Sun.…”

Section: What Are the Roles Of Shocks Reconnection Waves And Turbumentioning

confidence: 99%

“…In the bottom panel the shock passage at ≈00:28:06 UT is accompanied by an increase in the magnetic field magnitude |B|. The Cartesian components (B x , B y , B z ) of the field (top three panels) show large-amplitude fluctuations ahead of the shock generated by energetic ions streaming away from the shock along the mean magnetic field (Kennel et al 1984). From Tsurutani et al (1983) cle sources.…”

Section: What Are the Roles Of Shocks Reconnection Waves And Turbumentioning

confidence: 99%

The Solar Probe Plus Mission: Humanity’s First Visit to Our Star

et al. 2015

View full text Add to dashboard Cite

Solar Probe Plus (SPP) will be the first spacecraft to fly into the low solar corona. SPP's main science goal is to determine the structure and dynamics of the Sun's coronal magnetic field, understand how the solar corona and wind are heated and accelerated, and determine what processes accelerate energetic particles. Understanding these fundamental phenomena has been a top-priority science goal for over five decades, dating back to the 1958 Simpson Committee Report. The scale and concept of such a mission has been revised at intervals since that time, yet the core has always been a close encounter with the Sun. The mission design and the technology and engineering developments enable SPP to meet its science objectives to: (1) Trace the flow of energy that heats and accelerates the solar corona and solar wind; (2) Determine the structure and dynamics of the plasma and magnetic fields at the sources of the solar wind; and (3) Explore mechanisms that accelerate and transport energetic particles. The SPP mission was confirmed in March 2014 and is under development as a part of NASA's Living with a Star (LWS) Program. SPP is scheduled for launch in mid-2018, and will perform 24 orbits over a 7-year nominal mission duration. Seven Venus gravity assists gradually reduce SPP's perihelion from 35 solar radii (R S ) for the first orbit to <10 R S for the final three orbits. In this paper we present the science, B N.J. Fox

show abstract

“…The best known example of such regions is plasma wave turbulence in front of the Earth's bow shock [e.g., Russell and Hoppe, 1983; Le and Russell, 1994; Blanco-Cano et al, 1999]. Interplanetary blast shocks generated by solar flares display similar structures [Kennel et al, 1982[Kennel et al, , 1984Lee, 1983]. Therefore the magnetosphere is exposed to the interplanetary upstream wave turbulence some time before the SI.…”

Section: Introductionmentioning

confidence: 99%

An increase in Pc1 wave activity prior to magnetic sudden impulses

Guglielmi¹,

Kangas²,

Kultima³

et al. 2000

J. Geophys. Res.

View full text Add to dashboard Cite

Abstract. The enhancement of Pcl wave activity after magnetic sudden impulses (Sis) is well established by ground-based and satellite measurements. This phenomenon is explained by compressions of the magnetosphere under the action of interplanetary shocks. In this paper we use long-term ground-based observations of Pcl to study the variation of the Pcl wave activity before Sis. We conclude that there is a tendency for an increase of the rate of Pcl occurrence as the time gets closer to the SI. We interpret this effect as an impact of the interplanetary foreshocks on the Earth's magnetosphere. IntroductionIt is known that a magnetic sudden impulse ( In this work we analyze long-term ground-based observations of Pcl magnetic pulsations to study the probability of the Pcl occurrence within the 1.5-hour time interval preceding the SI. We conclude that an increase in Pcl activity prior to Sis takes place. This new observation is discussed in terms of the We see that the distribution of n (k) is nonuniform with the maximum value n(1) -38 for the first interval 0-5 min. 25,185

show abstract

Plasma and energetic particle structure upstream of a quasi‐parallel interplanetary shock

Cited by 91 publications

References 32 publications

Short-term variability of the Sun-Earth system: an overview of progress made during the CAWSES-II period

Short-term variability of the Sun-Earth system: an overview of progress made during the CAWSES-II period

The Solar Probe Plus Mission: Humanity’s First Visit to Our Star

An increase in Pc1 wave activity prior to magnetic sudden impulses

Contact Info

Product

Resources

About