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preprint2016arXiv

Electron Acceleration Mechanisms in Thunderstorms

Thunderstorms produce strong electric fields over regions on the order of kilometer. The corresponding electric potential differences are on the order of 100 MV. Secondary cosmic rays reaching these regions may be significantly accelerated and even amplified in relativistic runaway avalanche processes. These phenomena lead to enhancements of the high-energy background radiation observed by detectors on the ground and on board aircraft. Moreover, intense submillisecond gamma-ray bursts named terrestrial gamma-ray flashes (TGFs) produced in thunderstorms are detected from low Earth orbit satellites. When passing through the atmosphere, these gamma-rays are recognized to produce secondary relativistic electrons and positrons rapidly trapped in the geomagnetic field and injected into the near-Earth space environment. In the present work, we attempt to give an overview of the current state of research on high-energy phenomena associated with thunderstorms.

preprint2016arXiv

Investigation of muon flux anisotropy during CME

According to CACTus catalog, during periods of a high solar activity every day up to tens of coronal mass ejections are observed. Such ejections have an impact on the flux of cosmic rays that permeate the space around us. Unlike most ground cosmic ray detectors, muon hodoscope URAGAN (MEPhI) allows to investigate not only the integrated counting rate of registered particles, but also the spatial and angular characteristics of the muon flux at ground level. This approach to particle detection allows fixing changes in the flux of cosmic rays not only for geoeffective CMEs, but also for the ejections, the front of which is directed to the opposite side of the Sun. The results of the study of different types of CMEs at different stages of the solar activity from 2008 to 2015 are presented.

preprint2016arXiv

Spatial distribution of high-energy protons in the inner radiation belt on the data of low Earth orbit space experiments

Measurements of the ARINA instrument on board the Resurs-DK1 satellite (altitude $\sim$ 600 km and inclination $\sim$ 70$^{o}$, since 2006 till 2016) and the VSPLESK instrument on board the International Space Station (altitude $\sim$ 400 km and inclination $\sim$ 52$^{o}$, since 2008 till 2013) in low Earth orbits were presented in this report. Both instruments are identical in terms of physical layout. They can measure high-energy protons in the range 30-100 MeV with 10\% energy resolution and 7$^{o}$ angular accuracy. Data analysis was carried out for the total period of proton flux measurement by the instruments. L-B proton distributions in the inner radiation belt (L$<$2) were studied in dependence on proton energy. Geographical and pitch-angle distribution of proton intensity were studied for chosen L-shells. These distributions were analyzed during the decreasing part of the 23$^{rd}$ solar cycle and the main part of the 24$^{th}$ one.

preprint2016arXiv

Collisionless, phase-mixed, dispersive, Gaussian Alfven pulse in transversely inhomogeneous plasma

In the previous works harmonic, phase-mixed, Alfven wave dynamics was considered both in the kinetic and magnetohydrodynamic regimes. Up today only magnetohydrodynamic, phase-mixed, Gaussian Alfven pulses were investigated. In the present work we extend this into kinetic regime. Here phase-mixed, Gaussian Alfven pulses are studied, which are more appropriate for solar flares, than harmonic waves, as the flares are impulsive in nature. Collisionless, phase-mixed, dispersive, Gaussian Alfven pulse in transversely inhomogeneous plasma is investigated by particle-in-cell (PIC) simulations and by an analytical model. The pulse is in inertial regime with plasma beta less than electron-to-ion mass ratio and has a spatial width of 12 ion inertial length. The linear analytical model predicts that the pulse amplitude decrease is described by the linear Korteweg de Vries (KdV) equation. The numerical and analytical solution of the linear KdV equation produces the pulse amplitude decrease in time as $t^{-1}$. The latter scaling law is corroborated by full PIC simulations. It is shown that the pulse amplitude decrease is due to dispersive effects, while electron acceleration is due to Landau da

preprint2017arXiv

Diagnosing Coronal Heating Processes with Spectrally Resolved Soft X-ray Measurements

Decades of astrophysical observations have convincingly shown that soft X-ray (SXR; ~0.1--10 keV) emission provides unique diagnostics for the high temperature plasmas observed in solar flares and active regions. SXR observations critical for constraining models of energy release in these phenomena can be provided using instruments that have already been flown on sounding rockets and CubeSats, including miniaturized high-resolution photon-counting spectrometers and a novel diffractive spectral imager. These instruments have relatively low cost and high TRL, and would complement a wide range of mission concepts. In this white paper, we detail the scientific background and open questions motivating these instruments, the measurements required, and the instruments themselves that will make groundbreaking progress in answering these questions.

preprint2016arXiv

Prediction of Geomagnetic Storm Strength from Inner Heliospheric In Situ Observations

Prediction of the effects of coronal mass ejections (CMEs) on Earth strongly depends on knowledge of the interplanetary magnetic field southward component, Bz. Predicting the strength and duration of Bz inside a CME with sufficient accuracy is currently impossible, which forms the so-called Bz problem. Here, we provide a proof-of-concept of a new method for predicting the CME arrival time, speed, Bz and the resulting Dst index at Earth based only on magnetic field data, measured in situ in the inner heliosphere (< 1AU). On 2012 June 12-16, three approximately Earthward-directed and interacting CMEs were observed the by the STEREO imagers, and by Venus Express (VEX) in situ at 0.72 AU, 6 degree away from the Sun Earth line. The CME kinematics are calculated using the drag-based and WSA-Enlil models, constrained by the arrival time at VEX, resulting in the CME arrival time and speed at Earth. The CME magnetic field strength is scaled with a power law from VEX to Wind. Our investigation shows promising results for the Dst forecast (predicted: -96 and -114 nT (from 2 Dst models), observed: -71 nT), for the arrival speed (predicted: 531 +- 23 km s-1, observed: 488 +- 30 km s-1) and timi

preprint2016arXiv

Assessment of Source and Transport Parameters of Relativistic SEPs Based on Neutron Monitor Data

As part of the HESPERIA Horizon 2020 project, we developed a software package for the direct inversion of Ground Level Enhancements (GLEs) based on data of the worldwide network of Neutron Monitors (NMs). The new methodology to study the release processes of relativistic solar energetic particles (SEPs) makes use of several models, including: the propagation of relativistic SEPs from the Sun to the Earth, their transport in the Earth's magnetosphere and atmosphere, as well as the detection of the nucleon component of the secondary cosmic rays by ground based NMs. The combination of these models allows to compute the expected ground-level NM counting rates caused by a series of instantaneous particle releases from the Sun. The proton release-time profile at the Sun and the interplanetary transport conditions are then inferred by fitting NM observations with modeled NM counting rates. In the paper the used models for the different processes, the software and first findings with the new software are presented.

preprint2016arXiv

Breakdown of the Goldreich-Julian Relation in a Neutron Star

The electromagnetic field in a magnetized neutron star and the underlying volume charges and currents are found. A general case of a rigidly rotating neutron star with infinite conductivity, arbitrary distribution of the internal magnetic field, arbitrarily changing angular velocity, and arbitrary surface velocity less than the velocity of light is considered. Quaternions are used to describe rotation and determine the magnetic field. It is shown that the charge density is not equal to and can exceed significantly the common Goldreich-Julian density. Moreover, corrections to the magnetic field due to stellar rotation are zero. For a rotating neutron star, twisting magnetic field lines causes charge accumulation and current flows. This fact shows a possible link between changing internal magnetic field topology and observed activity of neutron stars.

preprint2016arXiv

Facilities of Athens Neutron Monitor Station to Space Weather services

In the frame of the comprehensive knowledge, detection and forecasting of the solar terrestrial relations as well as space weather events, the ground based measurements of the network of neutron monitor constitutes a vital tool for these studies. This is mainly the reason that Athens Neutron Monitor Station (A.Ne.Mo.S.) beyond of the provision of its real time data, has also developed several research applications. More specifically, applications such as a) an optimized automated Ground Level Enhancement Alert (GLE Alert Plus) b) a web interface, providing data from mul- tiple Neutron Monitor stations (Multi-Station tool) and c) a simulation model, named DYnamic Atmospheric Shower Tracking Interactive Model Application (DYASTIMA), which allows the study of the cosmic ray showers resulted when primary cosmic ray particles enters the atmosphere, have been developed. The two first applications are currently federated products in European Space Agency (ESA) and actually available via the Space Weather Portal operated by ESA. On the other hand, the contribution of the simulation tool DYASTIMA, based on the well known Geant4 toolkit, to the calculations of the radiation dose received by

preprint2016arXiv

Observations of the Abundances of Secondary Galactic Cosmic Rays from Z equals 5 to 28 Between 10 and 200 MeV/nuc Beyond the Heliopause by Voyager, Some Unexpected Anomalies and Their Interpretation Using a LBM for Galactic Propagation

Voyager observations for over 3 years beyond the heliopause have started to define features of the low energy, less than 100 MeV per nuc, cosmic ray secondary nuclei that have a zero or negligibly small source component. As an example, the abundance of B between about 7 and 15 MeV per nuc is unexpectedly large, greater than the prediction of a LBM by 2 or 3 in the measurement and cross section error. On the other hand, for several other heavier secondary nuclei with a low source abundance such as F and Z equal 17 to 19 and 21 to 23 nuclei, in the corresponding energy channels between about 10-20 MeV/nuc, zero nuclei have been observed. The same LBM calculations would predict about 6 to 7 events for the sum of these three groups of nuclei. The B observed intensities could be more closely matched by considering a nested LBM with 0.3-1.0 g/cm2 of matter near the cosmic ray sources, essentially a source component of B. This nested LBM calculation, if extended to the production of the above groups of secondaries, would however predict a total 8 to 12 events thus leading to an even larger discrepancy with the zero events that are observed. The measurements of heavier secondaries at low e

preprint2016arXiv

Space Radiation exposure calculations during different solar and galactic cosmic ray activities

The primary components of radiation in interplanetary space are galactic cosmic rays (GCR) and solar cosmic radiation (SCR). GCR originates from outside of our Solar System, while SCR consists of low energy solar wind particles that flow constantly from the Sun and the highly energetic solar particle events (SPEs) that originate from magnetically disturbed regions of the Sun, which sporadically emit bursts of energetic charged particles. Exposure to space radiation may place astronauts and aviation crews at significant risk for numerous biological effects resulting from exposure to radiation from a major SPE or combined SPE and GCR. Doses absorbed by tissues vary for different SPEs and model systems have been developed to calculate the radiation doses that could have been received by astronauts during previous SPEs. For this reason a new application DYASTIMA-R which constitutes a successor of the Dynamic Atmospheric Shower Tracking Interactive Model Application (DYASTIMA) is being developed. This new simulation tool will be used for the calculation of the equivalent dose during flights scenario in the lower or higher atmosphere, characterized by different altitudes, different geogr

preprint2016arXiv

Determining pitch-angle diffusion coefficients from test particle simulations

Transport and acceleration of charged particles in turbulent media is a topic of great interest in space physics and interstellar astrophysics. These processes are dominated by the scattering of particles off magnetic irregularities. The scattering process itself is usually described by small-angle scattering with the pitch-angle coefficient $D_{μμ}$ playing a major role. Since the diffusion coefficient $D_{μμ}$ can be determined analytically only for the approximation of quasi-linear theory, the determination of this coefficient from numerical simulations has, therefore, become more important. So far these simulations yield particle tracks for small-scale scattering, which can then be interpreted using the running diffusion coefficients. This method has a limited range of validity. This paper presents two new methods that allow for the calculation of the pitch-angle diffusion coefficient from numerical simulations. These methods no longer analyse particle trajectories, but the change of particle distribution functions. It is shown that they provide better resolved results and allow for the analysis of strong turbulence. The application of these methods to Monte Carlo simulations o

preprint2016arXiv

Artificial Intelligence Probes for Interstellar Exploration and Colonization

A recurring topic in interstellar exploration and the search for extraterrestrial intelligence (SETI) is the role of artificial intelligence. More precisely, these are programs or devices that are capable of performing cognitive tasks that have been previously associated with humans such as image recognition, reasoning, decision-making etc. Such systems are likely to play an important role in future deep space missions, notably interstellar exploration, where the spacecraft needs to act autonomously. This article explores the drivers for an interstellar mission with a computation-heavy payload and provides an outline of a spacecraft and mission architecture that supports such a payload. Based on existing technologies and extrapolations of current trends, it is shown that AI spacecraft development and operation will be constrained and driven by three aspects: power requirements for the payload, power generation capabilities, and heat rejection capabilities. A likely mission architecture for such a probe is to get into an orbit close to the star in order to generate maximum power for computational activities, and then to prepare for further exploration activities. Given current level

preprint2016arXiv

Application of a full chain analysis using neutron monitor data for space weather studies

An important topic in the field of space weather is the precise assessment of the contribution of galactic cosmic rays and solar energetic particles on air crew exposure, specifically during eruptive events on the Sun. Here we present a model, a full chain analysis based on ground based measurements of cosmic rays with neutron monitors, subsequent derivation of particle spectral and angular characteristics and computation of dose rate. The model uses method for ground level enhancement analysis and newly numerically computed yield functions for conversion of secondary particle fluence to effective dose and/or the ambient dose equivalent. The precise an adequate information about the solar energetic particle spectra (SEPs) is the basis of the model. Since SEPs possess an essential isotropic part, specifically during the event onset, the angular characteristics should be also derived with good precision. This can be achieved using neutron monitor data during a special class of SEP events the ground level enhancements (GLEs). On the basis of the method representing a sequence of consecutive steps: computation of the NM asymptotic cones, NM rigidity cut-off and application of convenien

preprint2016arXiv

Hybrid simulation of a parallel collisionless shock in the Large Plasma Device

We present two-dimensional hybrid kinetic/magnetohydrodynamic simulations of planned laser-ablation experiments in the Large Plasma Device (LAPD). Our results, based on parameters which have been validated in previous experiments, show that a parallel collisionless shock can begin forming within the available space. Carbon-debris ions that stream along the magnetic-field direction with a blow-off speed of four times the Alfven velocity excite strong magnetic fluctuations, eventually transfering part of their kinetic energy to the surrounding hydrogen ions. This acceleration and compression of the background plasma creates a shock front, which satisfies the Rankine-Hugoniot conditions and can therefore propagate on its own. Furthermore, we analyze the upstream turbulence and show that it is dominated by the right-hand resonant instability.

preprint2016arXiv

Pickup Ion Effect of the Solar Wind Interaction with the Local Interstellar Medium

Pickup ions are created when interstellar neutral atoms resonantly exchange charge with the solar wind (SW) ions, especially in the supersonic part of the wind, where they carry most of the plasma pressure. Here we present numerical simulation results of the 3D heliospheric interface treating pickup ions as a separate proton fluid. To satisfy the fundamental conservation laws, we solve the system of equations describing the flow of the mixture of electrons, thermal protons, and pickup ions. To find the density and pressure of pickup ions behind the termination shock, we employ simple boundary conditions that take into account the \emph{Voyager} observations that showed that the decrease in the kinetic energy of the mixture at the termination shock predominantly contributed to the increase in the pressure of pickup ions. We show that this model adequately describes the flow of the plasma mixture and results in a noticeable decrease in the heliosheath width.

preprint2016arXiv

Hard X-ray morphology of the X1.3 April 25, 2014 partially occulted limb solar flare

At hard X-ray energies, the bright footpoint emission from solar flare loops often prevents a detailed analysis of the weaker loop-top source morphology due to the limited dynamic range available for X-ray imaging. Here, we study the X1.3 April 25, 2014 flare with the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI). This partially occulted limb flare allows the analysis of the loop-top emission in isolation. We present results on the flare light curve at different energies, the source morphology from X-ray imaging and a detailed spectral analysis of the different source components by imaging spectroscopy. The loop-top source, a likely site of particle acceleration, shows a clear composition of different emission components. The results indicate the opportunities that detailed imaging of hard X-rays can provide to learn about particle acceleration, transport and heating processes in solar flares.

preprint2016arXiv

Differential kinetic dynamics and heating of ions in the turbulent solar wind

The solar wind plasma is a fully ionized and turbulent gas ejected by the outer layers of the solar corona at very high speed, mainly composed by protons and electrons, with a small percentage of helium nuclei and a significantly lower abundance of heavier ions. Since particle collisions are practically negligible, the solar wind is typically not in a state of thermodynamic equilibrium. Such a complex system must be described through self-consistent and fully nonlinear models, taking into account its multi-species composition and turbulence. We use a kinetic hybrid Vlasov-Maxwell numerical code to reproduce the turbulent energy cascade down to ion kinetic scales, in typical conditions of the uncontaminated solar wind plasma, with the aim of exploring the differential kinetic dynamics of the dominant ion species, namely protons and alpha particles. We show that the response of different species to the fluctuating electromagnetic fields is different. In particular, a significant differential heating of alphas with respect to protons is observed. Interestingly, the preferential heating process occurs in spatial regions nearby the peaks of ion vorticity and where strong deviations from

preprint2016arXiv

Long-Term Prospects: Mitigation of Supernova and Gamma-Ray Burst Threat to Intelligent Beings

We consider global catastrophic risks due to cosmic explosions (supernovae, magnetars and gamma-ray bursts) and possible mitigation strategies by humans and other hypothetical intelligent beings. While by their very nature these events are so huge to daunt conventional thinking on mitigation and response, we wish to argue that advanced technological civilizations would be able to develop efficient responses in the domain of astroengineering within their home planetary systems. In particular, we suggest that construction of shielding swarms of small objects/particles confined by electromagnetic fields could be one way of mitigating the risk of cosmic explosions and corresponding ionizing radiation surges. Such feats of astroengineering could, in principle, be detectable from afar by advanced Dysonian SETI searches.

preprint2000arXiv

Rotatable-Torsion-Balance Equivalence Principleexperiment for the Spin-Polarized Hofe_{3}

We use a rotatable torsion balance to perform an equivalence principle test on a magnetically shielded spin-polarized body of HoFe_{3}. With a rotation period of one hour, the period of possible signal is reduced from one solar day by 24 times, and hence the 1/f noise is greatly reduced. Our present experimental results gives a limit (0.25 +- 1.26) X 10^{-9} on the Eotvos parameter ηof equivalence of the polarized body compared with unpolarized aluminium-brass cylinders in the solar gravitional field, and a limit (0.34 +- 0.52) X 10^{-9} in the earth gravitional fields. This improves the previous limit on polarized bodies by a factor of 45 for solar field and by a factor of 11 for earth field.

preprint2016arXiv

HILDCAA* events between 1998 and 2007 and their related interplanetary magnetic field and plasma values

We investigate the interplanetary conditions during 135 less strict high-intensity, long-duration, continuous AE activity (HILDCAA*) events between the years 1998-2007. The HILDCAA* events were chosen by following the three "traditional" criteria which describe the high-intensity, long-duration, continuous AE activity (HILDCAA). However, we include a small modification in the criteria that considers: "the AE values do not drop below 200 nT for more than 2 h at a time". This criteria is modified by changing 2 to 4 hours period in which the AE values should not drop below 200 nT. Once the events are selected, we perform a statistical analysis of the interplanetary parameters during their occurrences. The distribution of HILDCAA* events along the solar cycle shows a pattern of double peak, with a peak around the maximum of the sunspot cycle, and an other in the descending phase. This kind of distribution is similar to the distribution of low-latitude coronal holes. For each of the HILDCAA* events, we have found its related Interplanetary Magnetic Field (IMF) and plasma parameter signatures. The average values of AE, AU, AL, and Dst indices, the density and temperature

preprint2016arXiv

Solar Energetic Particle Events with Protons above 500 MeV between 1995 and 2015 Measured with SOHO/EPHIN

The Sun is an effective particle accelerator producing solar energetic particle (SEP) events during which particles up to several GeVs can be observed. Those events observed at Earth with the neutron monitor network are called ground level enhancements (GLEs). Although these events with a high energy component have been investigated for several decades, a clear relation between the spectral shape of the SEPs outside the Earth's magnetosphere and the increase in neutron monitor count rate has yet to be established. Hence, an analysis of these events is of interest for the space weather as well as the solar event community. In this work, SEP events with protons accelerated to above 500 MeV have been identified using data from the Electron Proton Helium Instrument (EPHIN) aboard the Solar and Heliospheric Observatory (SOHO) between 1995 and 2015. For a statistical analysis, onset times have been determined for the events and the proton energy spectra were derived and fitted with a power law. As a result, a list of 42 SEP events with protons accelerated to above 500 MeV measured with the EPHIN instrument onboard SOHO is presented. The statistical analysis based on the fitted spectr

preprint2016arXiv

Energy spectra of 3He-rich solar energetic particles associated with coronal waves

In addition to their anomalous abundances, 3He-rich solar energetic particles (SEPs) show puzzling energy spectral shapes varying from rounded forms to power laws where the later are characteristics of shock acceleration. Solar sources of these particles have been often associated with jets and narrow CMEs, which are the signatures of magnetic reconnection involving open field. Recent reports on new associations with large-scale EUV waves bring new insights on acceleration and transport of 3He-rich SEPs in the corona. We examined energy spectra for 32 3He-rich SEP events observed by ACE at L1 near solar minimum in 2007-2010 and compared the spectral shapes with solar flare signatures obtained from STEREO EUV images. We found the events with jets or brightenings tend to be associated with rounded spectra and the events with coronal waves with power laws. This suggests that coronal waves may be related to the unknown second stage mechanism commonly used to interpret spectral forms of 3He-rich SEPs.

preprint2016arXiv

Automated detection of coronal mass ejections in three-dimensions using multi-viewpoint observations

A new, automated method of detecting coronal mass ejections (CMEs) in three dimensions for the LASCO C2 and STEREO COR2 coronagraphs is presented. By triangulating isolated CME signal from the three coronagraphs over a sliding window of five hours, the most likely region through which CMEs pass at 5 solar radii is identified. The centre and size of the region gives the most likely direction of propagation and approximate angular extent. The Automated CME Triangulation (ACT) method is tested extensively using a series of synthetic CME images created using a wireframe flux rope density model, and on a sample of real coronagraph data; including halo CMEs. The accuracy of the angular difference between the detection and true input of the synthetic CMEs is 7.14 degrees, and remains acceptable for a broad range of CME positions relative to the observer, the relative separation of the three observers and even through the loss of one coronagraph. For real data, the method gives results that compare well with the distribution of low coronal sources and results from another instrument and technique made further from the Sun. The true three dimension (3D)-corrected kinematics and mass/density

648 works

J. Wang

Researcher

J. Wang contributes to research discovery and scholarly infrastructure.

Open to collaborate

575 works

Y. Wang

Researcher

Y. Wang contributes to research discovery and scholarly infrastructure.

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438 works

Lei Zhang

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Lei Zhang contributes to research discovery and scholarly infrastructure.

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405 works

Y. Liu

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Y. Liu contributes to research discovery and scholarly infrastructure.

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387 works

J. Zhang

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J. Zhang contributes to research discovery and scholarly infrastructure.

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331 works

Y. Chen

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Y. Chen contributes to research discovery and scholarly infrastructure.

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319 works

Xin Wang

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Xin Wang contributes to research discovery and scholarly infrastructure.

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316 works

Abraham Loeb

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Abraham Loeb contributes to research discovery and scholarly infrastructure.

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302 works

Bo Li

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Bo Li contributes to research discovery and scholarly infrastructure.

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300 works

Q. Liu

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Q. Liu contributes to research discovery and scholarly infrastructure.

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293 works

Wei Liu

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Wei Liu contributes to research discovery and scholarly infrastructure.

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273 works

Rui Wang

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Rui Wang contributes to research discovery and scholarly infrastructure.

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physics.space-ph

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24 paper(s) to start with

Electron Acceleration Mechanisms in Thunderstorms

Investigation of muon flux anisotropy during CME

Spatial distribution of high-energy protons in the inner radiation belt on the data of low Earth orbit space experiments

Collisionless, phase-mixed, dispersive, Gaussian Alfven pulse in transversely inhomogeneous plasma

Diagnosing Coronal Heating Processes with Spectrally Resolved Soft X-ray Measurements

Prediction of Geomagnetic Storm Strength from Inner Heliospheric In Situ Observations

Assessment of Source and Transport Parameters of Relativistic SEPs Based on Neutron Monitor Data

Breakdown of the Goldreich-Julian Relation in a Neutron Star

Facilities of Athens Neutron Monitor Station to Space Weather services

Observations of the Abundances of Secondary Galactic Cosmic Rays from Z equals 5 to 28 Between 10 and 200 MeV/nuc Beyond the Heliopause by Voyager, Some Unexpected Anomalies and Their Interpretation Using a LBM for Galactic Propagation

Space Radiation exposure calculations during different solar and galactic cosmic ray activities

Determining pitch-angle diffusion coefficients from test particle simulations

Artificial Intelligence Probes for Interstellar Exploration and Colonization

Application of a full chain analysis using neutron monitor data for space weather studies

Hybrid simulation of a parallel collisionless shock in the Large Plasma Device

Pickup Ion Effect of the Solar Wind Interaction with the Local Interstellar Medium

Hard X-ray morphology of the X1.3 April 25, 2014 partially occulted limb solar flare

Differential kinetic dynamics and heating of ions in the turbulent solar wind

Long-Term Prospects: Mitigation of Supernova and Gamma-Ray Burst Threat to Intelligent Beings

Rotatable-Torsion-Balance Equivalence Principleexperiment for the Spin-Polarized Hofe_{3}

HILDCAA* events between 1998 and 2007 and their related interplanetary magnetic field and plasma values

Solar Energetic Particle Events with Protons above 500 MeV between 1995 and 2015 Measured with SOHO/EPHIN

Energy spectra of 3He-rich solar energetic particles associated with coronal waves

Automated detection of coronal mass ejections in three-dimensions using multi-viewpoint observations

12 visible researcher(s)

J. Wang

Y. Wang

Lei Zhang

Y. Liu

J. Zhang

Y. Chen

Xin Wang

Abraham Loeb

Bo Li

Q. Liu

Wei Liu

Rui Wang