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Liu Chen - One of the best experts on this subject based on the ideXlab platform.
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short wavelength geodesic acoustic mode excitation by Energetic Particles
Physics of Plasmas, 2018Co-Authors: Liu Chen, Zhiyong Qiu, F ZoncaAbstract:Taking the collisionless damping of the geodesic acoustic mode (GAM) in the short wavelength limit originally investigated in [Z. Qiu et al., Plasma Phys. Controlled Fusion 51, 012001 (2009)] as an example, the physics processes underlying wave particle resonances in the short wavelength limit are clarified. As an illustrative application, GAM excitation by Energetic Particles in the short wavelength limit is investigated assuming a single pitch angle slowing-down fast ion equilibrium distribution function. Conditions for this Energetic particle-induced GAM to be unstable are discussed.Taking the collisionless damping of the geodesic acoustic mode (GAM) in the short wavelength limit originally investigated in [Z. Qiu et al., Plasma Phys. Controlled Fusion 51, 012001 (2009)] as an example, the physics processes underlying wave particle resonances in the short wavelength limit are clarified. As an illustrative application, GAM excitation by Energetic Particles in the short wavelength limit is investigated assuming a single pitch angle slowing-down fast ion equilibrium distribution function. Conditions for this Energetic particle-induced GAM to be unstable are discussed.
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short wavelength geodesic acoustic mode excitation by Energetic Particles
arXiv: Plasma Physics, 2017Co-Authors: Liu Chen, Zhiyong Qiu, F ZoncaAbstract:Taking the collisionless damping of geodesic acoustic mode (GAM) as an example, the physics processes underlying wave particle resonances in the short wavelength limit are clarified. As illus- trative application, GAM excitation by Energetic Particles in short wavelength limit is investigated assuming a single pitch angle slowing-down fast ion equilibrium distribution function. Conditions for this Energetic particle-induced GAM (EGAM) to be unstable are discussed.
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theory on excitations of drift alfven waves by Energetic Particles i variational formulation
Physics of Plasmas, 2014Co-Authors: Liu Chen, F ZoncaAbstract:A unified theoretical framework is presented for analyzing various branches of drift Alfven waves and describing their linear and nonlinear behaviors, covering a wide range of spatial and temporal scales. Nonlinear gyrokinetic quasineutrality condition and vorticity equation, derived for drift Alfven waves excited by Energetic Particles in fusion plasmas, are cast in integral form, which is generally variational in the linear limit; and the corresponding gyrokinetic energy principle is obtained. Well known forms of the kinetic energy principle are readily recovered from this general formulation. Furthermore, it is possible to demonstrate that the general fishbone like dispersion relation, obtained within the present theoretical framework, provides a unified description of drift Alfven waves excited by Energetic Particles as either Alfven eigenmodes or Energetic particle modes. The advantage of the present approach stands in its capability of extracting underlying linear and nonlinear physics as well as spatial and temporal scales of the considered fluctuation spectrum. For these reasons, this unified theoretical framework can help understanding experimental observations as well as numerical simulation and analytic results with different levels of approximation. Examples and applications are given in Paper II [F. Zonca and L. Chen, “Theory on excitations of drift Alfven waves by Energetic Particles. II. The general fishbone-like dispersion relation,” Phys. Plasmas 21, 072121 (2014)].
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theory on excitations of drift alfven waves by Energetic Particles ii the general fishbone like dispersion relation
Physics of Plasmas, 2014Co-Authors: Liu Chen, F ZoncaAbstract:The theoretical framework of the general fishbone-like dispersion relation (GFLDR), presented and discussed in the Companion Paper [Phys. Plasmas 21, 072120 (2014)], is applied to cases of practical interest of shear/drift Alfven waves (SAWs/DAWs) excited by Energetic Particles (EPs) in toroidal fusion plasmas. These applications demonstrate that the GFLDR provides a unified approach that allows analytical and numerical calculations of stability properties, as well as mode structures and, in general, nonlinear evolutions, based on different models and with different levels of approximation. They also show the crucial importance of kinetic descriptions, accurate geometries and boundary conditions for predicting linear as well as nonlinear SAW/DAW and EP behaviors in burning plasmas. Thus, the GFLDR unified theoretical framework elevates the interpretative capability for both experimental and numerical simulation results.
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nonlinear dynamics of beta induced alfven eigenmode driven by Energetic Particles
Physical Review E, 2012Co-Authors: X Wang, Liu Chen, S Briguglio, C Di Troia, G Fogaccia, G Vlad, F ZoncaAbstract:Nonlinear saturation of a beta-induced Alfven eigenmode, driven by slowing down Energetic Particles via transit resonance, is investigated by the nonlinear hybrid magnetohyrodynamic gyrokinetic code. Saturation is characterized by frequency chirping and symmetry breaking between co- and counter-passing Particles, which can be understood as the evidence of resonance detuning. The scaling of the saturation amplitude with the growth rate is also demonstrated to be consistent with radial resonance detuning due to the radial nonuniformity and mode structure.
F Zonca - One of the best experts on this subject based on the ideXlab platform.
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short wavelength geodesic acoustic mode excitation by Energetic Particles
Physics of Plasmas, 2018Co-Authors: Liu Chen, Zhiyong Qiu, F ZoncaAbstract:Taking the collisionless damping of the geodesic acoustic mode (GAM) in the short wavelength limit originally investigated in [Z. Qiu et al., Plasma Phys. Controlled Fusion 51, 012001 (2009)] as an example, the physics processes underlying wave particle resonances in the short wavelength limit are clarified. As an illustrative application, GAM excitation by Energetic Particles in the short wavelength limit is investigated assuming a single pitch angle slowing-down fast ion equilibrium distribution function. Conditions for this Energetic particle-induced GAM to be unstable are discussed.Taking the collisionless damping of the geodesic acoustic mode (GAM) in the short wavelength limit originally investigated in [Z. Qiu et al., Plasma Phys. Controlled Fusion 51, 012001 (2009)] as an example, the physics processes underlying wave particle resonances in the short wavelength limit are clarified. As an illustrative application, GAM excitation by Energetic Particles in the short wavelength limit is investigated assuming a single pitch angle slowing-down fast ion equilibrium distribution function. Conditions for this Energetic particle-induced GAM to be unstable are discussed.
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short wavelength geodesic acoustic mode excitation by Energetic Particles
arXiv: Plasma Physics, 2017Co-Authors: Liu Chen, Zhiyong Qiu, F ZoncaAbstract:Taking the collisionless damping of geodesic acoustic mode (GAM) as an example, the physics processes underlying wave particle resonances in the short wavelength limit are clarified. As illus- trative application, GAM excitation by Energetic Particles in short wavelength limit is investigated assuming a single pitch angle slowing-down fast ion equilibrium distribution function. Conditions for this Energetic particle-induced GAM (EGAM) to be unstable are discussed.
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theory on excitations of drift alfven waves by Energetic Particles i variational formulation
Physics of Plasmas, 2014Co-Authors: Liu Chen, F ZoncaAbstract:A unified theoretical framework is presented for analyzing various branches of drift Alfven waves and describing their linear and nonlinear behaviors, covering a wide range of spatial and temporal scales. Nonlinear gyrokinetic quasineutrality condition and vorticity equation, derived for drift Alfven waves excited by Energetic Particles in fusion plasmas, are cast in integral form, which is generally variational in the linear limit; and the corresponding gyrokinetic energy principle is obtained. Well known forms of the kinetic energy principle are readily recovered from this general formulation. Furthermore, it is possible to demonstrate that the general fishbone like dispersion relation, obtained within the present theoretical framework, provides a unified description of drift Alfven waves excited by Energetic Particles as either Alfven eigenmodes or Energetic particle modes. The advantage of the present approach stands in its capability of extracting underlying linear and nonlinear physics as well as spatial and temporal scales of the considered fluctuation spectrum. For these reasons, this unified theoretical framework can help understanding experimental observations as well as numerical simulation and analytic results with different levels of approximation. Examples and applications are given in Paper II [F. Zonca and L. Chen, “Theory on excitations of drift Alfven waves by Energetic Particles. II. The general fishbone-like dispersion relation,” Phys. Plasmas 21, 072121 (2014)].
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theory on excitations of drift alfven waves by Energetic Particles ii the general fishbone like dispersion relation
Physics of Plasmas, 2014Co-Authors: Liu Chen, F ZoncaAbstract:The theoretical framework of the general fishbone-like dispersion relation (GFLDR), presented and discussed in the Companion Paper [Phys. Plasmas 21, 072120 (2014)], is applied to cases of practical interest of shear/drift Alfven waves (SAWs/DAWs) excited by Energetic Particles (EPs) in toroidal fusion plasmas. These applications demonstrate that the GFLDR provides a unified approach that allows analytical and numerical calculations of stability properties, as well as mode structures and, in general, nonlinear evolutions, based on different models and with different levels of approximation. They also show the crucial importance of kinetic descriptions, accurate geometries and boundary conditions for predicting linear as well as nonlinear SAW/DAW and EP behaviors in burning plasmas. Thus, the GFLDR unified theoretical framework elevates the interpretative capability for both experimental and numerical simulation results.
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nonlinear dynamics of beta induced alfven eigenmode driven by Energetic Particles
Physical Review E, 2012Co-Authors: X Wang, Liu Chen, S Briguglio, C Di Troia, G Fogaccia, G Vlad, F ZoncaAbstract:Nonlinear saturation of a beta-induced Alfven eigenmode, driven by slowing down Energetic Particles via transit resonance, is investigated by the nonlinear hybrid magnetohyrodynamic gyrokinetic code. Saturation is characterized by frequency chirping and symmetry breaking between co- and counter-passing Particles, which can be understood as the evidence of resonance detuning. The scaling of the saturation amplitude with the growth rate is also demonstrated to be consistent with radial resonance detuning due to the radial nonuniformity and mode structure.
Radoslav Bucik - One of the best experts on this subject based on the ideXlab platform.
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3 he rich solar Energetic Particles solar sources
Space Science Reviews, 2020Co-Authors: Radoslav BucikAbstract:3He-rich solar Energetic Particles (SEPs), showing up to a 10,000-fold abundance enhancement of rare elements like 3He or ultra-heavy nuclei, have been a puzzle for more than 50 years. One reason for the current lack of understanding of 3He-rich SEPs is the difficulty resolving the source regions of these commonly occurring events. Since their discovery, there has been strong evidence that 3He-rich SEP production is associated with flares on the Sun. Anomalous abundances of 3He-rich SEPs have been attributed to a unique acceleration mechanism that must routinely operate at flare sites. Flares associated with 3He-rich SEPs have been often observed in jet-like forms indicating an acceleration in magnetic reconnection involving field lines open to interplanetary space. Owing to a fleet of spacecraft around the Sun, providing a greatly improved resolution of solar imaging observations, 3He-rich SEP sources are now explored in unprecedented detail. This paper outlines the current understanding of 3He-rich SEPs, mainly focusing on their solar sources.
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3he rich solar Energetic Particles in helical jets on the sun
The Astrophysical Journal, 2018Co-Authors: G. M. Mason, Radoslav Bucik, D E Innes, R Gomezherrero, Mark E Wiedenbeck, N. NittaAbstract:Particle acceleration in stellar flares is ubiquitous in the Universe, however, our Sun is the only astrophysical object where Energetic Particles and their source flares can both be observed. The acceleration mechanism in solar flares, tremendously enhancing (up to a factor of ten thousand) rare elements like 3He and ultra-heavy nuclei, has been puzzling for almost 50 years. Here we present some of the most intense 3He- and Fe-rich solar Energetic particle events ever reported. The events were accompanied by non-relativistic electron events and type III radio bursts. The corresponding high-resolution, extreme-ultraviolet imaging observations have revealed for the first time a helical structure in the source flare with a jet-like shape. The helical jets originated in relatively small, compact active regions, located at the coronal hole boundary. A mini-filament at the base of the jet appears to trigger these events. The events were observed with the two Solar Terrestrial Relations Observatories STEREO on the backside of the Sun, during the period of increased solar activity in 2014. The helical jets may be a distinct feature of these intense events that is related to the production of high 3He and Fe enrichments.
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energy spectra of 3he rich solar Energetic Particles associated with coronal waves
arXiv: Solar and Stellar Astrophysics, 2016Co-Authors: Radoslav Bucik, G. M. Mason, D E Innes, M. E. WiedenbeckAbstract: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.
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multi spacecraft observations of recurrent 3he rich solar Energetic Particles
The Astrophysical Journal, 2014Co-Authors: Radoslav Bucik, G. M. Mason, D E Innes, Andreas Korth, Urs Mall, R GomezherreroAbstract:We study the origin of {sup 3}He-rich solar Energetic Particles (<1 MeV nucleon{sup –1}) that are observed consecutively on STEREO-B, Advanced Composition Explorer (ACE), and STEREO-A spacecraft when they are separated in heliolongitude by more than 90°. The {sup 3}He-rich period on STEREO-B and STEREO-A commences on 2011 July 1 and 2011 July 16, respectively. The ACE {sup 3}He-rich period consists of two sub-events starting on 2011 July 7 and 2011 July 9. We associate the STEREO-B July 1 and ACE July 7 {sup 3}He-rich events with the same sizeable active region (AR) producing X-ray flares accompanied by prompt electron events, when it was near the west solar limb as seen from the respective spacecraft. The ACE July 9 and STEREO-A July 16 events were dispersionless with enormous {sup 3}He enrichment, lacking solar Energetic electrons and occurring in corotating interaction regions. We associate these events with a small, recently emerged AR near the border of a low-latitude coronal hole that produced numerous jet-like emissions temporally correlated with type III radio bursts. For the first time we present observations of (1) solar regions with long-lasting conditions for {sup 3}He acceleration and (2) solar Energetic {sup 3}He that is temporarily confined/re-accelerated inmore » interplanetary space.« less
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multi spacecraft observations of recurrent 3he rich solar Energetic Particles
arXiv: Solar and Stellar Astrophysics, 2014Co-Authors: Radoslav Bucik, G. M. Mason, D E Innes, Andreas Korth, Urs Mall, R GomezherreroAbstract:We study the origin of 3He-rich solar Energetic Particles (<1 MeV/nucleon) that are observed consecutively on STEREO-B, ACE, and STEREO-A spacecraft when they are separated in heliolongitude by more than 90{\deg}. The 3He-rich period on STEREO-B and STEREO-A commences on 2011 July 1 and 2011 July 16, respectively. The ACE 3He-rich period consists of two sub-events starting on 2011 July 7 and 2011 July 9. We associate the STEREO-B July 1 and ACE July 7 3He-rich events with the same sizeable active region producing X-ray flares accompanied by prompt electron events, when it was near the west solar limb as seen from the respective spacecraft. The ACE July 9 and STEREO-A July 16 events were dispersionless with enormous 3He enrichment, lacking solar Energetic electrons and occurring in corotating interaction regions. We associate these events with a small, recently emerged active region near the border of a low-latitude coronal hole that produced numerous jet-like emissions temporally correlated with type III radio bursts. For the first time we present observations of 1) solar regions with long-lasting conditions for 3He acceleration and 2) solar Energetic 3He that is temporary confined/re-accelerated in interplanetary space.
G. M. Mason - One of the best experts on this subject based on the ideXlab platform.
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3he rich solar Energetic Particles in helical jets on the sun
The Astrophysical Journal, 2018Co-Authors: G. M. Mason, Radoslav Bucik, D E Innes, R Gomezherrero, Mark E Wiedenbeck, N. NittaAbstract:Particle acceleration in stellar flares is ubiquitous in the Universe, however, our Sun is the only astrophysical object where Energetic Particles and their source flares can both be observed. The acceleration mechanism in solar flares, tremendously enhancing (up to a factor of ten thousand) rare elements like 3He and ultra-heavy nuclei, has been puzzling for almost 50 years. Here we present some of the most intense 3He- and Fe-rich solar Energetic particle events ever reported. The events were accompanied by non-relativistic electron events and type III radio bursts. The corresponding high-resolution, extreme-ultraviolet imaging observations have revealed for the first time a helical structure in the source flare with a jet-like shape. The helical jets originated in relatively small, compact active regions, located at the coronal hole boundary. A mini-filament at the base of the jet appears to trigger these events. The events were observed with the two Solar Terrestrial Relations Observatories STEREO on the backside of the Sun, during the period of increased solar activity in 2014. The helical jets may be a distinct feature of these intense events that is related to the production of high 3He and Fe enrichments.
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energy spectra of 3he rich solar Energetic Particles associated with coronal waves
arXiv: Solar and Stellar Astrophysics, 2016Co-Authors: Radoslav Bucik, G. M. Mason, D E Innes, M. E. WiedenbeckAbstract: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.
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multi spacecraft observations of recurrent 3he rich solar Energetic Particles
The Astrophysical Journal, 2014Co-Authors: Radoslav Bucik, G. M. Mason, D E Innes, Andreas Korth, Urs Mall, R GomezherreroAbstract:We study the origin of {sup 3}He-rich solar Energetic Particles (<1 MeV nucleon{sup –1}) that are observed consecutively on STEREO-B, Advanced Composition Explorer (ACE), and STEREO-A spacecraft when they are separated in heliolongitude by more than 90°. The {sup 3}He-rich period on STEREO-B and STEREO-A commences on 2011 July 1 and 2011 July 16, respectively. The ACE {sup 3}He-rich period consists of two sub-events starting on 2011 July 7 and 2011 July 9. We associate the STEREO-B July 1 and ACE July 7 {sup 3}He-rich events with the same sizeable active region (AR) producing X-ray flares accompanied by prompt electron events, when it was near the west solar limb as seen from the respective spacecraft. The ACE July 9 and STEREO-A July 16 events were dispersionless with enormous {sup 3}He enrichment, lacking solar Energetic electrons and occurring in corotating interaction regions. We associate these events with a small, recently emerged AR near the border of a low-latitude coronal hole that produced numerous jet-like emissions temporally correlated with type III radio bursts. For the first time we present observations of (1) solar regions with long-lasting conditions for {sup 3}He acceleration and (2) solar Energetic {sup 3}He that is temporarily confined/re-accelerated inmore » interplanetary space.« less
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multi spacecraft observations of recurrent 3he rich solar Energetic Particles
arXiv: Solar and Stellar Astrophysics, 2014Co-Authors: Radoslav Bucik, G. M. Mason, D E Innes, Andreas Korth, Urs Mall, R GomezherreroAbstract:We study the origin of 3He-rich solar Energetic Particles (<1 MeV/nucleon) that are observed consecutively on STEREO-B, ACE, and STEREO-A spacecraft when they are separated in heliolongitude by more than 90{\deg}. The 3He-rich period on STEREO-B and STEREO-A commences on 2011 July 1 and 2011 July 16, respectively. The ACE 3He-rich period consists of two sub-events starting on 2011 July 7 and 2011 July 9. We associate the STEREO-B July 1 and ACE July 7 3He-rich events with the same sizeable active region producing X-ray flares accompanied by prompt electron events, when it was near the west solar limb as seen from the respective spacecraft. The ACE July 9 and STEREO-A July 16 events were dispersionless with enormous 3He enrichment, lacking solar Energetic electrons and occurring in corotating interaction regions. We associate these events with a small, recently emerged active region near the border of a low-latitude coronal hole that produced numerous jet-like emissions temporally correlated with type III radio bursts. For the first time we present observations of 1) solar regions with long-lasting conditions for 3He acceleration and 2) solar Energetic 3He that is temporary confined/re-accelerated in interplanetary space.
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the very unusual interplanetary coronal mass ejection of 2012 july 23 a blast wave mediated by solar Energetic Particles
The Astrophysical Journal, 2013Co-Authors: C T Russell, G. M. Mason, R Gomezherrero, R A Leske, R. A. Mewaldt, J G Luhmann, T T Von Rosenvinge, A Klassen, A B GalvinAbstract:The giant, superfast, interplanetary coronal mass ejection, detected by STEREO A on 2012 July 23, well away from Earth, appears to have reached 1 AU with an unusual set of leading bow waves resembling in some ways a subsonic interaction, possibly due to the high pressures present in the very Energetic Particles produced in this event. Eventually, a front of record high-speed flow reached STEREO. The unusual behavior of this event is illustrated using the magnetic field, plasma, and Energetic ion observations obtained by STEREO. Had the Earth been at the location of STEREO, the large southward-oriented magnetic field component in the event, combined with its high speed, would have produced a record storm.
R D Strauss - One of the best experts on this subject based on the ideXlab platform.
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Heliosheath Processes and the Structure of the Heliopause: Modeling Energetic Particles, Cosmic Rays, and Magnetic Fields
Space Science Reviews, 2017Co-Authors: N V Pogorelov, E. C. Stone, M S Potgieter, H. Fichtner, A. Czechowski, A. Lazarian, B. Lembege, J. A. Roux, K. Scherer, R D StraussAbstract:This paper summarizes the results obtained by the team “Heliosheath Processes and the Structure of the Heliopause: Modeling Energetic Particles, Cosmic Rays, and Magnetic Fields” supported by the International Space Science Institute (ISSI) in Bern, Switzerland. We focus on the physical processes occurring in the outer heliosphere, especially at its boundary called the heliopause, and in the local interstellar medium. The importance of magnetic field, charge exchange between neutral atoms and ions, and solar cycle on the heliopause topology and observed heliocentric distances to different heliospheric discontinuities are discussed. It is shown that time-dependent, data-driven boundary conditions are necessary to describe the heliospheric asymmetries detected by the Voyager spacecraft. We also discuss the structure of the heliopause, especially due to its instability and magnetic reconnection. It is demonstrated that the Rayleigh–Taylor instability of the nose of the heliopause creates consecutive layers of the interstellar and heliospheric plasma which are magnetically connected to different sources. This may be a possible explanation of abrupt changes in the galactic and anomalous cosmic ray fluxes observed by Voyager 1 when it was crossing the heliopause structure for a period of about one month in the summer of 2012. This paper also discusses the plausibility of fitting simulation results to a number of observational data sets obtained by in situ and remote measurements. The distribution of magnetic field in the vicinity of the heliopause is discussed in the context of Voyager measurements. It is argued that a classical heliospheric current sheet formed due to the Sun’s rotation is not observed by in situ measurements and should not be expected to exist in numerical simulations extending to the boundary of the heliosphere. Furthermore, we discuss the transport of Energetic Particles in the inner and outer heliosheath, concentrating on the anisotropic spatial diffusion diffusion tensor and the pitch-angle dependence of perpendicular diffusion and demonstrate that the latter can explain the observed pitch-angle anisotropies of both the anomalous and galactic cosmic rays in the outer heliosheath.
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Heliosheath processes and the structure of the heliopause: modeling Energetic Particles, cosmic rays, and magnetic fields
Space Science Reviews, 2017Co-Authors: N V Pogorelov, E. C. Stone, Horst Fichtner, M S Potgieter, A. Czechowski, A. Lazarian, B. Lembege, J. A. Roux, K. Scherer, R D StraussAbstract:This paper summarizes the results obtained by the team "Heliosheath Processes and the Structure of the Heliopause: Modeling Energetic Particles, Cosmic Rays, and Magnetic Fields" supported by the International Space Science Institute in Bern, Switzerland. We focus on the physical processes occurring in the outer heliosphere, especially at its boundary called the heliopause (HP), and in the LISM. The importance of magnetic field, charge exchange between atoms and ions, and solar cycle on the heliopause topology and observed heliocentric distances to different heliospheric discontinuities are discussed. It is shown that time-dependent boundary conditions are necessary to describe the heliospheric asymmetries detected by the Voyager spacecraft. We also discuss the structure of the HP, especially due to its instability and magnetic reconnection. It is demonstrated that the Rayleigh-Taylor instability of the nose of the HP creates consecutive layers of the interstellar and heliospheric plasma which are magnetically connected to different sources. This may be a possible explanation of abrupt changes in the galactic and anomalous cosmic ray fluxes observed by Voyager 1 when it was crossing the HP structure for a period of about one month in the summer of 2012. This paper also discusses the plausibility of fitting simulation results to a number of observational data sets obtained by in situ and remote measurements. The distribution of magnetic field in the vicinity of the HP is discussed in the context of Voyager measurements. We discuss the transport of Energetic Particles in the inner and outer heliosheath, concentrating on the anisotropic spatial diffusion diffusion tensor and the pitch-angle dependence of perpendicular diffusion and demonstrate that the latter can explain the observed pitch-angle anisotropies of both the anomalous and galactic cosmic rays in the outer heliosheath.