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Preface 1 Stormy Tour from the Sun to the Earth 2 Physical Foundations 3 Single particle motion 4 Waves in Cold Plasma Approximation 5 Vlasov Theory 6.
Table of contents
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- What is Solar Wind? - The Definition, Cause and Effects Explained | Space
- Space Weather
Here the authors report evidence of a flare-induced rotation of a sunspot, showing nonuniform acceleration following the peaks of X-ray emissions. Article 03 October Open Access. Here, the authors study an even in which the solar wind Mach number remained steadily below one, leading to the evanescence of the bow shock and loss of electrons in the outer belts.
Here the authors compare observations and models of a event to show that electromagnetic ioncyclotron waves provide the dominant loss mechanism at ultra-relativistic energies. Article 15 July Open Access. The causes behind fluctuations in Neptune's brightness as observed from Earth have proved enigmatic. Article 16 June Open Access. Magnetic reconnection is a fundamental process giving rise to topology change and energy release in plasmas, of particular relevance for the Sun.
Here the authors report the observation of fast reconnection in a solar filament eruption, which occurs between a set of ambient fibrils and the filament itself. Article 16 May Open Access.
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Solar eruptions heavily influence space weather, but what are their causes remains an open question. Here the authors present a magnetohydrodynamic model of a solar eruption directly driven by solar magnetograms, following the transition from pre-eruptive to eruptive state. Article 26 October Open Access. Here, the authors analyse records recovered from ice cores and suggest these spikes originated from extreme solar particle events. Article 05 October Open Access. Here, the authors explain the origin of this phenomenon in terms of chorus and magnetosonic waves through simulations and observations of a geomagnetic storm data.
Article 14 July Open Access. Here, the authors uncover their structured and periodic frequency pattern, revealing that they are generated by proton distributions. Article 26 June Open Access. Magnetic reconnection is a fundamental energy release process taking place in various astrophysical environments, but it is difficult to observe it directly. Here, the authors provide evidence of three-dimensional magnetic reconnection in a solar eruption using combined perspectives of two spacecraft.
Article 23 June Open Access. Regional surface climate response to a future decline in solar activity remains uncertain. Here, via numerical simulations, the authors show that a return to Maunder Minimum-like lows by could lead to some areas of significantly reduced surface warming via modulation of the North Atlantic Oscillation.
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Article 26 May Open Access. Coronal mass ejections from the Sun play an important role in space weather, yet a full understanding of their behaviour remains elusive. Article 15 May Open Access. Whistler-mode waves regulate trapped electrons in the magnetosphere, but an accurate determination of their energy budget has remained elusive.
This study presents a full analysis of their magnetic and electric field contributions and finds that a large amount of energy is stored in oblique waves. Article 11 May Open Access. Although magnetic reconnection is recognized as the dominant mode for solar wind plasma to enter the magnetosphere, Kelvin—Helmholtz waves KHW have been suggested to also be involved. Advanced search.
Skip to main content. Article 23 May Open Access Loss-cone instability modulation due to a magnetohydrodynamic sausage mode oscillation in the solar corona Magnetohydrodynamic MHD waves and plasma instabilities can be studied during solar flares. Article 04 March Open Access MMS observations of electron scale magnetic cavity embedded in proton scale magnetic cavity Magnetic cavities are universal phenomena existing in cosmic plasma environments. Article 14 February Open Access Evidence for electron Landau damping in space plasma turbulence Various physical mechanisms are proposed to explain the heating observed in turbulent astrophysical plasmas.
Article 12 February Open Access Direct observations of a surface eigenmode of the dayside magnetopause Surface waves on the boundary between a magnetosphere and the surrounding plasma might get trapped by the ionosphere forming an eigenmode. Article 16 January Open Access Visualization of rapid electron precipitation via chorus element wave—particle interactions Electron precipitation plays major role in magnetospheric physics and space weather.
Article 10 January Open Access A metamaterial-enabled design enhancing decades-old short backfire antenna technology for space applications There is significant interest in providing real-world applications for metamaterials. Article 06 December Open Access The two-fluid dynamics and energetics of the asymmetric magnetic reconnection in laboratory and space plasmas Magnetic energy in the plasma is transferred into particle energy by magnetic reconnection.
Article 30 November Open Access Magnetic reconnection driven by electron dynamics Magnetic reconnection is the process of releasing energy by magnetized and space plasma. Article 15 November Open Access A diagnosis of the plasma waves responsible for the explosive energy release of substorm onset The origin of geomagnetic substorms is still uncertain due to lack of comprehensive quantitative analyses. Article 28 September Open Access Remote sensing of geomagnetic fields and atomic collisions in the mesosphere Remote sensing of geomagnetic fields in mesosphere is both challenging and interesting to explore the magnetic field structures and atomic collision processes.
What is Solar Wind? - The Definition, Cause and Effects Explained | Space
Article 19 September Open Access Sounding-rocket microgravity experiments on alumina dust Alumina is thought to be the main condensate to form in the gas outflow from oxygen-rich evolved stars. Article 20 August Open Access Major upwelling and overturning in the mid-latitude F region ionosphere The ionosphere can give rise to irregularities that can interfere with radio communication, navigation and satellite systems. Article 10 May Open Access Explaining the apparent impenetrable barrier to ultra-relativistic electrons in the outer Van Allen belt The origin of the apparent impenetrable barrier in the outer Van Allen belt is still uncertain.
Article 15 February Open Access Observationally quantified reconnection providing a viable mechanism for active region coronal heating The solar corona heating mechanism is still subject to debate. Article 12 January Open Access Formation and dynamics of a solar eruptive flux tube Solar eruptions are large explosions occurring in the solar atmosphere. Article 03 January Open Access Transient rotation of photospheric vector magnetic fields associated with a solar flare The violent solar eruptions known as flares are caused by magnetic reconnection.
Article 19 December Open Access Increased ionization supports growth of aerosols into cloud condensation nuclei Ions produced by cosmic rays have been thought to influence aerosol and cloud processes by an unknown mechanism. Article 19 December Open Access A circular white-light flare with impulsive and gradual white-light kernels White-light flares are rare solar events entailing emission in the optical continuum. Article 15 November Open Access Imaging spectroscopy of solar radio burst fine structures Radio observations of the solar atmosphere provide a unique view on the non-thermal processes in the outer atmosphere.
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Article 06 November Open Access Buildup of a highly twisted magnetic flux rope during a solar eruption Solar eruptions provide opportunities to study magnetic flux ropes, a structure of fundamental importance for both plasma physics and space weather. Article 13 December Open Access Observation of a reversal of rotation in a sunspot during a solar flare Back reaction of coronal magnetic fields on the solar surface may help to understand the coronal reconfiguration during a solar flare.
As we begin to understand these interactions better in the coming decade, we will also begin to learn more about the next frontier of exploration, the local interstellar medium and the nearby parts of the galaxy that are not in direct plasma contact with our Sun. How do coronal structures evolve into solar wind structures of varying speed, density, kinetic temperature, composition, and magnetic field strength? How do CME-driven disturbances evolve in space and time as they propagate through the heliosphere?
What is the structure of the interplanetary magnetic field at very large distances from the Sun and as a function of the solar cycle? How are plasma, neutrals, heavy ions, turbulent fluctuations, solar energetic particles, and galactic cosmic rays distributed throughout the entire heliospheric volume? How do the solar wind plasma and magnetic field interact with the electromagnetic field, plasma, and neutrals in the nearby region of the galaxy?
How and where is the boundary of the heliosphere established?
How does it move in time, and how do such changes affect our space environment? What is the nature of the local interstellar medium? Challenge 3: Understanding the space environments of Earth and other solar system bodies and their dynamical response to external and internal influences. Nonetheless, important gaps in scientific understanding remain—concerning, for example, the configuration and dynamics of the magnetosphere under extreme solar wind conditions i.
The next decade will see extensive exploration of the magnetosphere of another giant planet, Saturn. Such processes, already extensively studied at Venus by the Pioneer Venus Orbiter, will also be investigated during the next decade at Mars by the Japanese Nozomi mission and the European Mars Express mission. What processes are responsible for the rapid acceleration of charged particles to hundreds of keV at the onset of magnetospheric substorms and to MeV energies during geomagnetic storms?
Do the active auroral displays during substorms arise from instabilities in the ionosphere, or do they simply mirror plasma motions in the outer magnetosphere? What process is responsible for the pulsating x-ray aurora at Jupiter? What is the effect of localized crustal magnetic fields on the solar wind interaction with Mars?
How are outflowing ions on the nightside of Mars accelerated to keV energies? How do substorms at Mercury differ from terrestrial substorms? Challenge 4: Understanding the basic physical principles manifest in processes observed in solar and space plasmas. The ultimate goal of solar and space physics research is not merely to produce a detailed phenomenological description of its various objects of study but also to understand the fundamental physical processes that operate in them.
As these processes largely involve matter in the plasma state, solar physics and space physics can both be considered branches of plasma electrodynamics, to which field they have contributed significantly over the years. The heliosphere is a natural laboratory for the study of plasma physics, and the next decade of research can be expected to lead to advances in our understanding of such fundamental plasma physical processes as magnetic reconnection; turbulence; charged particle acceleration and scattering; generation, transport, and damping of plasma waves; and magnetic dynamo action.
The study of these processes in naturally occurring solar system plasmas will be complemented by their investigation with increasingly sophisticated computer models and in laboratory plasma experiments see Chapter 4. What controls the rate of collisionless magnetic reconnection? How is reconnection initiated?