arXiv - PHYS - Space Physics最新文献

{"title":"Comparing NASA Discovery and New Frontiers Class Mission Concepts for the Io Volcano Observer (IVO)","authors":"Christopher W. Hamilton, Alfred S. McEwen, Laszlo Keszthelyi, Lynn M. Carter, Ashley G. Davies, Katherine de Kleer, Kandis Lea Jessup, Xianzhe Jia, James T. Keane, Kathleen Mandt, Francis Nimmo, Chris Paranicas, Ryan S. Park, Jason E. Perry, Anne Pommier, Jani Radebaugh, Sarah S. Sutton, Audrey Vorburger, Peter Wurz, Cauê Borlina, Amanda F. Haapala, Daniella N. DellaGiustina, Brett W. Denevi, Sarah M. Hörst, Sascha Kempf, Krishan K. Khurana, Justin J. Likar, Adam Masters, Olivier Mousis, Anjani T. Polit, Aditya Bhushan, Michael Bland, Isamu Matsuyama, John Spencer","doi":"arxiv-2408.08334","DOIUrl":"https://doi.org/arxiv-2408.08334","url":null,"abstract":"Jupiter's moon Io is a highly compelling target for future exploration that\u0000offers critical insight into tidal dissipation processes and the geology of\u0000high heat flux worlds, including primitive planetary bodies, such as the early\u0000Earth, that are shaped by enhanced rates of volcanism. Io is also important for\u0000understanding the development of volcanogenic atmospheres and mass-exchange\u0000within the Jupiter System. However, fundamental questions remain about the\u0000state of Io's interior, surface, and atmosphere, as well as its role in the\u0000evolution of the Galilean satellites. The Io Volcano Observer (IVO) would\u0000address these questions by achieving the following three key goals: (A)\u0000Determine how and where tidal heat is generated inside Io; (B) Understand how\u0000tidal heat is transported to the surface of Io; and (C) Understand how Io is\u0000evolving. IVO was selected for Phase A study through the NASA Discovery program\u0000in 2020 and, in anticipation of a New Frontiers 5 opportunity, an enhanced\u0000IVO-NF mission concept was advanced that would increase the Baseline mission\u0000from 10 flybys to 20, with an improved radiation design; employ a Ka-band\u0000communications to double IVO's total data downlink; add a wide angle camera for\u0000color and stereo mapping; add a dust mass spectrometer; and lower the altitude\u0000of later flybys to enable new science. This study compares and contrasts the\u0000mission architecture, instrument suite, and science objectives for Discovery\u0000(IVO) and New Frontiers (IVO-NF) missions to Io, and advocates for continued\u0000prioritization of Io as an exploration target for New Frontiers.","PeriodicalId":501423,"journal":{"name":"arXiv - PHYS - Space Physics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142223607","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"On the Formation of Super-Alfvénic Flows Downstream of Collisionless Shocks","authors":"Adnane Osmane, Savvas Raptis","doi":"arxiv-2408.08159","DOIUrl":"https://doi.org/arxiv-2408.08159","url":null,"abstract":"Super-Alfv'enic jets, with kinetic energy densities significantly exceeding\u0000that of the solar wind, are commonly generated downstream of Earth's bow shock\u0000under both high and low beta plasma conditions. In this study, we present\u0000theoretical evidence that these enhanced kinetic energy flows are driven by\u0000firehose-unstable fluctuations and compressive heating within collisionless\u0000plasma environments. Using a fluid formalism that incorporates pressure\u0000anisotropy, we estimate that the downstream flow of a collisionless plasma\u0000shock can be accelerated by a factor of 2 to 4 following the compression and\u0000saturation of firehose instability. By analyzing quasi-parallel magnetosheath\u0000jets observed in situ by the Magnetospheric Multiscale (MMS) mission, we find\u0000that approximately 11% of plasma measurements within these jets exhibit\u0000firehose-unstable fluctuations. Our findings offer an explanation for the\u0000distinctive generation of fast downstream flows in both low ($beta<1$) and\u0000high ($beta>1$) beta plasmas, and provide new evidence that kinetic processes\u0000are crucial for accurately describing the formation and evolution of\u0000magnetosheath jets.","PeriodicalId":501423,"journal":{"name":"arXiv - PHYS - Space Physics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178440","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Characterizing Solar Spicules and their Role in Solar Wind Production using Machine Learning and the Hough Transform","authors":"R. Sadeghi, E. Tavabi","doi":"arxiv-2408.07168","DOIUrl":"https://doi.org/arxiv-2408.07168","url":null,"abstract":"Solar winds originate from the Sun and can be classified as fast or slow.\u0000Fast solar winds come from coronal holes at the solar poles, while slow solar\u0000winds may originate from the equatorial region or streamers. Spicules are\u0000jet-like structures observed in the Sun's chromosphere and transition region.\u0000Some spicules exhibit rotating motion, potentially indicating vorticity and\u0000Alfven waves. Machine learning and the Hough algorithm were used to analyze\u0000over 3000 frames of the Sun, identifying spicules and their characteristics.\u0000The study found that rotating spicules, accounting for 21 percent at the poles\u0000and 4 percent at the equator, play a role in energy transfer to the upper solar\u0000atmosphere. The observations suggest connections between spicules, mini-loops,\u0000magnetic reconnection, and the acceleration of fast solar winds. Understanding\u0000these small-scale structures is crucial for comprehending the origin and\u0000heating of the fast solar wind.","PeriodicalId":501423,"journal":{"name":"arXiv - PHYS - Space Physics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178441","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Universal non-thermal power-law distribution functions from the self-consistent evolution of collisionless electrostatic plasmas","authors":"Uddipan Banik, Amitava Bhattacharjee, Wrick Sengupta","doi":"arxiv-2408.07127","DOIUrl":"https://doi.org/arxiv-2408.07127","url":null,"abstract":"Distribution functions of collisionless systems are known to show non-thermal\u0000power law tails. Interestingly, collisionless plasmas in various physical\u0000scenarios, (e.g., the ion population of the solar wind) feature a $v^{-5}$ tail\u0000in the velocity ($v$) distribution, whose origin has been a long-standing\u0000mystery. We show this power law tail to be a natural outcome of the\u0000self-consistent collisionless relaxation of driven electrostatic plasmas. We\u0000perform a quasilinear analysis of the perturbed Vlasov-Poisson equations to\u0000show that the coarse-grained mean distribution function (DF), $f_0$, follows a\u0000quasilinear diffusion equation with a diffusion coefficient $D(v)$ that depends\u0000on $v$ through the plasma dielectric constant. If the plasma is isotropically\u0000forced on scales much larger than the Debye length with a white noise-like\u0000electric field, then $D(v)sim v^4$ for $sigma<v<omega_{mathrm{P}}/k$, with\u0000$sigma$ the thermal velocity, $omega_{mathrm{P}}$ the plasma frequency and\u0000$k$ the maximum wavenumber of the perturbation; the corresponding $f_0$, in the\u0000quasi-steady state, develops a $v^{-left(d+2right)}$ tail in $d$ dimensions\u0000($v^{-5}$ tail in 3D), while the energy ($E$) distribution develops an $E^{-2}$\u0000tail irrespective of the dimensionality of space. Any redness of the noise only\u0000alters the scaling in the high $v$ end. Non-resonant particles moving slower\u0000than the phase-velocity of the plasma waves ($omega_{mathrm{P}}/k$)\u0000experience a Debye-screened electric field, and significantly less (power law\u0000suppressed) acceleration than the near-resonant particles. Thus, a Maxwellian\u0000DF develops a power law tail. The Maxwellian core ($v<sigma$) eventually also\u0000heats up, but over a much longer timescale than that over which the tail forms.\u0000We definitively show that self-consistency (ignored in test-particle\u0000treatments) is crucial for the development of the universal $v^{-5}$ tail.","PeriodicalId":501423,"journal":{"name":"arXiv - PHYS - Space Physics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178258","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Recent advances in solar data-driven MHD simulations of the formation and evolution of CME flux ropes","authors":"Brigitte Schmieder, Jinhan Guo, Stefaan Poedts","doi":"arxiv-2408.06595","DOIUrl":"https://doi.org/arxiv-2408.06595","url":null,"abstract":"Filament eruptions and coronal mass ejections are physical phenomena related\u0000to magnetic flux ropes carrying electric current. A magnetic flux rope is a key\u0000structure for solar eruptions, and when it carries a southward magnetic field\u0000component when propagating to the Earth. It is the primary driver of strong\u0000geomagnetic storms. As a result, developing a numerical model capable of\u0000capturing the entire progression of a flux rope, from its inception to its\u0000eruptive phase, is crucial for forecasting adverse space weather. The existence\u0000of such flux ropes is revealed by the presence of sigmoids in active regions or\u0000hot channels by observations from space and ground instruments. After proposing\u0000cartoons in 2D, potential, linear, non-linear-force-free-field (NLFFF) and\u0000non-force-free-field (NFFF) magnetic extrapolations, 3D numerical\u0000magnetohydrodynamic (MHD) simulation models were developed, first in a static\u0000configuration and later dynamic data-driven MHD models using high resolution\u0000observed vector magnetograms. This paper reviews a few recent developments in\u0000data-driven mode, such as the time-dependent magneto-frictional (TMF) and\u0000thermodynamic magnetohydrodynamic (MHD) models. Hereafter, to demonstrate the\u0000capacity of these models to reveal the physics of observations, we present the\u0000results for three events explored in our group: 1. the eruptive X1.0 flare on\u000028 October 2021; 2. the filament eruption on 18 August 2022; and 3. the\u0000confined X2.2 flare on 6 September 2017. These case studies validate the\u0000ability of data-driven models to retrieve observations, including the formation\u0000and eruption of flux ropes, 3D magnetic reconnection, CME three-part structures\u0000and the failed eruption. Based on these results, we provide some arguments for\u0000the formation mechanisms of flux ropes, the physical nature of the CME leading\u0000front, and the constraints of failed eruptions.","PeriodicalId":501423,"journal":{"name":"arXiv - PHYS - Space Physics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178442","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Density-gradient-driven drift waves in the solar corona","authors":"Michaela Brchnelova, MJ Pueschel, Stefaan Poedts","doi":"arxiv-2408.06696","DOIUrl":"https://doi.org/arxiv-2408.06696","url":null,"abstract":"It has been suggested that under solar coronal conditions, drift waves may\u0000contribute to coronal heating. Specific properties of the drift waves to be\u0000expected in the solar corona have, however, not yet been determined using more\u0000advanced numerical models. We investigate the linear properties of\u0000density-gradient-driven drift waves in the solar coronal plasma using\u0000gyrokinetic ion-electron simulations with the gyrokinetic code GENE, solving\u0000the Vlasov-Maxwell equations in five dimensions assuming a simple slab\u0000geometry. We determine the frequencies and growth rates of the coronal density\u0000gradient-driven drift waves with changing plasma parameters, such as the\u0000electron b{eta} , the density gradient, the magnetic shear and additional\u0000temperature gradients. To investigate the influence of the finite Larmor radius\u0000effect on the growth and structure of the modes, we also compare the\u0000gyrokinetic simulation results to those obtained from drift-kinetics. In most\u0000of the investigated conditions, the drift wave has positive growth rates that\u0000increase with increasing density gradient and decreasing b{eta} . In the case\u0000of increasing magnetic shear, we find that from a certain point, the growth\u0000rate reaches a plateau. Depending on the considered reference environment, the\u0000frequencies and growth rates of these waves lie on the order of 0.1 mHz to 1\u0000Hz. These values correspond to the observed solar wind density fluctuations\u0000near the Sun detected by WISPR, currently of unexplained origin. As a next\u0000step, nonlinear simulations are required to determine the expected fluctuation\u0000amplitudes and the plasma heating resulting from this mechanism.","PeriodicalId":501423,"journal":{"name":"arXiv - PHYS - Space Physics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178443","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Non-Maxwellian Ion Distribution in the Equatorial and Auroral Electrojets","authors":"Rattanakorn Koontaweepunya, Yakov S. Dimant, Meers M. Oppenheim","doi":"arxiv-2408.06339","DOIUrl":"https://doi.org/arxiv-2408.06339","url":null,"abstract":"Strong electric fields in the auroral and equatorial electrojets can distort\u0000the background ion distribution function away from Maxwellian. We developed a\u0000collisional plasma kinetic model using the Boltzmann equation and a simple BGK\u0000collision operator which predicts a relatively simple relationship between the\u0000intensity of the background electric field and the resulting ion distribution\u0000function. To test the model, we perform 3-D plasma particle-in-cell simulations\u0000and compare the results to the model. The simulation applies an elastic\u0000collision operator assuming a constant ion-neutral collision rate. These\u0000simulations show less ion heating in the Pedersen direction than the analytic\u0000model but show similar overall heating. The model overestimates the heating in\u0000the Pedersen direction because the simple BGK operator includes no angular\u0000collisional scattering in the ion velocity space. On the other hand, the\u0000fully-kinetic particle-in-cell code is able to capture the physics of ion\u0000scattering in 3-D and therefore heats ions more isotropically. Although the\u0000simple BGK analytic theory does not precisely model the non-Maxwellian ion\u0000distribution function, it does capture the overall momentum and energy flows\u0000and therefore can provide the basis of further analysis of E-region wave\u0000evolution.","PeriodicalId":501423,"journal":{"name":"arXiv - PHYS - Space Physics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142178257","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"On the distribution of the the near-solar bound dust grains detected with Parker Solar Probe","authors":"Samuel Kočiščák, Audun Theodorsen, Ingrid Mann","doi":"arxiv-2408.05031","DOIUrl":"https://doi.org/arxiv-2408.05031","url":null,"abstract":"Parker Solar Probe (PSP) counts dust impacts in the near-solar region, but\u0000modelling effort is needed to understand the dust population's properties. We\u0000aim to constrain the dust cloud's properties based on the flux observed by PSP.\u0000We develop a forward-model for the bound dust detection rates using the\u0000formalism of 6D phase space distribution of the dust. We apply the model to the\u0000location table of different PSP's solar encounter groups. We explain some of\u0000the near-perihelion features observed in the data as well as the broader\u0000characteristic of the dust flux between 0.15 AU and 0.5 AU. We compare the\u0000measurements of PSP to the measurements of Solar Orbiter (SolO) near 1 AU to\u0000expose the differences between the two spacecraft. We found that the dust flux\u0000observed by PSP between 0.15 AU and 0.5 AU in post-perihelia can be explained\u0000by dust on bound orbits and is consistent with a broad range of orbital\u0000parameters, including dust on circular orbits. However, the dust number density\u0000as a function of the heliocentric distance and the scaling of detection\u0000efficiency with the relative speed are important to explain the observed flux\u0000variation. The data suggest that the slope of differential mass distribution\u0000${delta}$ is between 0.14 and 0.49. The near-perihelion observations, however,\u0000show the flux maxima, which are inconsistent with the circular dust model, and\u0000additional effects may play a role. We found indication that the sunward side\u0000of PSP is less sensitive to the dust impacts, compared to the other PSP's\u0000surfaces. Conclusions. We show that the dust flux on PSP can be explained by\u0000non-circular bound dust and the detection capabilities of PSP. The scaling of\u0000flux with the impact speed is especially important, and shallower than\u0000previously assumed.","PeriodicalId":501423,"journal":{"name":"arXiv - PHYS - Space Physics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141946758","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"EclipseNETs: a differentiable description of irregular eclipse conditions","authors":"Giacomo Acciarini, Francesco Biscani, Dario Izzo","doi":"arxiv-2408.05387","DOIUrl":"https://doi.org/arxiv-2408.05387","url":null,"abstract":"In the field of spaceflight mechanics and astrodynamics, determining eclipse\u0000regions is a frequent and critical challenge. This determination impacts\u0000various factors, including the acceleration induced by solar radiation\u0000pressure, the spacecraft power input, and its thermal state all of which must\u0000be accounted for in various phases of the mission design. This study leverages\u0000recent advances in neural image processing to develop fully differentiable\u0000models of eclipse regions for highly irregular celestial bodies. By utilizing\u0000test cases involving Solar System bodies previously visited by spacecraft, such\u0000as 433 Eros, 25143 Itokawa, 67P/Churyumov--Gerasimenko, and 101955 Bennu, we\u0000propose and study an implicit neural architecture defining the shape of the\u0000eclipse cone based on the Sun's direction. Employing periodic activation\u0000functions, we achieve high precision in modeling eclipse conditions.\u0000Furthermore, we discuss the potential applications of these differentiable\u0000models in spaceflight mechanics computations.","PeriodicalId":501423,"journal":{"name":"arXiv - PHYS - Space Physics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142223610","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Extreme heating of minor ions in imbalanced solar-wind turbulence","authors":"Michael F. Zhang, Matthew W. Kunz, Jonathan Squire, Kristopher G. Klein","doi":"arxiv-2408.04703","DOIUrl":"https://doi.org/arxiv-2408.04703","url":null,"abstract":"Minor ions in the solar corona are heated to extreme temperatures, far in\u0000excess of those of the electrons and protons that comprise the bulk of the\u0000plasma. These highly non-thermal distributions make minor ions sensitive probes\u0000of the underlying collisionless heating processes, which are crucial to coronal\u0000heating and the creation of the solar wind. The recent discovery of the\u0000\"helicity barrier\" offers a mechanism where imbalanced Alfv'enic turbulence in\u0000low-beta plasmas preferentially heats protons over electrons, generating\u0000high-frequency, proton-cyclotron-resonant fluctuations. We use the\u0000hybrid-kinetic particle-in-cell code, Pegasus++, to drive imbalanced Alfv'enic\u0000turbulence in a 3D low-beta plasma with additional passive ion species,\u0000He$^{2+}$ and O$^{5+}$. A helicity barrier naturally develops, followed by\u0000clear phase-space signatures of oblique ion-cyclotron-wave heating and\u0000Landau-resonant heating from the imbalanced Alfv'enic fluctuations. The former\u0000results in characteristically arced ion velocity distribution functions, whose\u0000non-bi-Maxwellian features are shown by linear ALPS calculations to be critical\u0000to the heating process. Additional features include a steep transition-range\u0000electromagnetic spectrum, the presence of ion-cyclotron waves propagating in\u0000the direction of imbalance, significantly enhanced proton-to-electron heating\u0000ratios, anisotropic ion temperatures that are significantly more perpendicular\u0000with respect to magnetic field, and extreme heating of heavier species in a\u0000manner consistent with empirically derived mass scalings informed by\u0000measurements. None of these features are realized in an otherwise equivalent\u0000simulation of balanced turbulence. If seen simultaneously in the fast solar\u0000wind, these signatures of the helicity barrier would testify to the necessity\u0000of incorporating turbulence imbalance in a complete theory for the evolution of\u0000the solar wind.","PeriodicalId":501423,"journal":{"name":"arXiv - PHYS - Space Physics","volume":null,"pages":null},"PeriodicalIF":0.0,"publicationDate":"2024-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141946756","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}