arXiv - PHYS - High Energy Astrophysical Phenomena最新文献

{"title":"Asking Fast Radio Bursts (FRBs) for More than Reionization History","authors":"Abinash Kumar Shaw, Raghunath Ghara, Paz Beniamini, Saleem Zaroubi, Pawan Kumar","doi":"arxiv-2409.03255","DOIUrl":"https://doi.org/arxiv-2409.03255","url":null,"abstract":"We propose different estimators to probe the epoch of reionization (EoR)\u0000intergalactic medium (IGM) using the dispersion measure (${rm DM}$) of the\u0000FRBs. We consider three different reionization histories which we can\u0000distinguish with a total of $lesssim 1000$ ${rm DM}$ measurements during EoR\u0000if their redshifts are known. We note that the redshift derivatives of ${rm\u0000DM}$ are also directly sensitive to the reionization history. The major point\u0000of this work is exploring the variance in the ${rm DM}$ measurements and the\u0000information encoded in them. We find that the all-sky average $overline{{rm\u0000DM}}(z)$ gets biased from the LoS fluctuations in the ${rm DM}$ measurements\u0000introduced by the ionization of IGM during EoR. We find that the ratio\u0000$sigma_{rm DM}/overline{{rm DM}}$ depends directly on the ionization bubble\u0000sizes as well as the reionization history. On the other hand, we also find that\u0000angular variance (coined as $structure$ $function$) of ${rm DM}$ encodes the\u0000information about the duration of reionization and the typical bubble sizes as\u0000well. We establish the usefulness of variances in ${rm DM}$ using toy models\u0000of reionization and later verify it with the realistic reionization\u0000simulations.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"5 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206588","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":"A splitting method for numerical relativistic magnetohydrodynamics","authors":"Serguei Komissarov, David Phillips","doi":"arxiv-2409.03637","DOIUrl":"https://doi.org/arxiv-2409.03637","url":null,"abstract":"We describe a novel splitting approach to numerical relativistic\u0000magnetohydrodynamics (RMHD) designed to expand its applicability to the domain\u0000of ultra-high magnetisation (high-$sigma$). In this approach, the\u0000electromagnetic field is split into the force-free component and its\u0000perturbation due to the plasma inertia. Accordingly, the system of RMHD\u0000equations is extended to include the subsystem of force-free degenerate\u0000electrodynamics and the subsystem governing the plasma dynamics and the\u0000perturbation of the force-free field. The combined system of conservation laws\u0000is integrated simultaneously, to which aim various numerical techniques can be\u0000used, and the force-free field is recombined with its perturbation at the end\u0000of every timestep. To explore the potential of this splitting approach, we\u0000combined it with a 3rd-order WENO method, and carried out a variety of 1D and\u00002D test simulations. The simulations confirm the robustness of the splitting\u0000method in the high-$sigma$ regime, and also show that it remains accurate in\u0000the low-$sigma$ regime, all the way down to $sigma$ = 0. Thus, the method can\u0000be used for simulating complex astrophysical flows involving a wide range of\u0000physical parameters. The numerical resistivity of the code obeys a simple\u0000ansatz and allows fast magnetic reconnection in the plasmoid-dominated regime.\u0000The results of simulations involving thin and long current sheets agree very\u0000well with the theory of resistive magnetic reconnection.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"74 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206583","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":"Diversity in hydrogen-rich envelope mass of type II supernovae (II): SN 2023ixf as explosion of partially-stripped intermediate massive star","authors":"Qiliang Fang, Takashi J. Moriya, Lucía Ferrari, Keiichi Maeda, Gaston Folatelli, Keila Y. Ertini, Hanindyo Kuncarayakti, Jennifer E. Andrews, Tatsuya Matsumoto","doi":"arxiv-2409.03540","DOIUrl":"https://doi.org/arxiv-2409.03540","url":null,"abstract":"SN 2023ixf is one of the most well-observed core-collapse supernova in recent\u0000decades, yet there is inconsistency in the inferred zero-age-main-sequence\u0000(ZAMS) mass $M_{rm ZAMS}$ of its progenitor. Direct observations of the pre-SN\u0000red supergiant (RSG) estimate $M_{rm ZAMS}$ spanning widely from 11 to 18\u0000$M_{rm odot}$. Additional constraints, including host environment and the\u0000pulsation of its progenitor RSG, suggest a massive progenitor with $M_{rm\u0000ZAMS}$ > 17 $M_{rm odot}$. However, the analysis of the properties of\u0000supernova, from light curve modeling to late phase spectroscopy, favor a\u0000relatively low mass scenario ($M_{rm ZAMS}$ < 15 $M_{rm odot}$). In this\u0000work, we conduct systematic analysis of SN 2023ixf, from the RSG progenitor,\u0000plateau phase light curve to late phase spectroscopy. Using MESA+STELLA to\u0000simulate the RSG progenitor and their explosions, we find that, despite the\u0000ZAMS mass of the RSG models being varied from 12.0 to 17.5 $M_{rm odot}$,\u0000they can produce light curves that well match with SN 2023ixf if the envelope\u0000mass and the explosion energy are allowed to vary. Using late phase\u0000spectroscopy as independent measurement, the oxygen emission line [O I]\u0000suggests the ZAMS is intermediate massive (~16.0 $M_{rm odot}$), and the\u0000relatively weak H$alpha$ emission line indicates the hydrogen envelope has\u0000been partially removed before the explosion. By incorporating the velocity\u0000structure derived from the light curve modeling into an axisymmetric model, we\u0000successfully generated [O I] line profiles that are consistent with the [O I]\u0000line observed in late phase spectroscopy of SN 2023ixf. Bringing these analyses\u0000together, we conclude that SN 2023ixf is the aspherical explosion of an\u0000intermediate massive star ($M_{rm ZAMS}$ = 15-16 $M_{rm odot}$) with the\u0000hydrogen envelope being partially stripped to 4-5 $M_{rm odot}$ prior to its\u0000explosion.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"45 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206613","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":"Are BAL outflows powered by radiation pressure on dust?","authors":"W. Ishibashi, A. C. Fabian, P. C. Hewett","doi":"arxiv-2409.03842","DOIUrl":"https://doi.org/arxiv-2409.03842","url":null,"abstract":"Broad absorption line (BAL) outflows are commonly detected in active galactic\u0000nuclei (AGN), but their driving mechanism remains poorly constrained. Here we\u0000investigate whether radiation pressure on dust can adequately explain the BAL\u0000phenomenon observed in quasars. In the framework of our AGN radiative dusty\u0000feedback scenario, we show that dust-driven outflows can reach BAL wind-like\u0000velocities ($v sim 10^4$ km/s) on galactic scales ($r lesssim 1$ kpc). This\u0000is consistent with recent observations indicating that BAL acceleration\u0000typically occurs on scales of $sim 10$ pc, and that the majority of BAL\u0000outflows are located at galactocentric radii greater than $sim 100$ pc. We\u0000derive the outflow radial velocity profile and compute the associated outflow\u0000momentum rate and kinetic power, which are found to be in agreement with the\u0000outflow energetics measured in BAL quasars. Therefore radiation pressure on\u0000dust may account for the observed BAL outflow dynamics and energetics.\u0000Furthermore, we consider BAL clouds/clumps (leading to a clumpy BAL flow\u0000characterised by a wide range of outflowing velocities), and we analyse how the\u0000resulting covering factors affect the shape of the absorption line profiles. We\u0000conclude that dust-driven BAL outflows may provide a significant contribution\u0000to AGN feedback on galactic scales.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"30 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206582","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":"A simple model of dust extinction in gamma-ray burst host galaxies","authors":"N. A. Rakotondrainibe, V. Buat, D. Turpin, D. Dornic, E. LeFloc'h, S. D. Vergani, S. Basa","doi":"arxiv-2409.03570","DOIUrl":"https://doi.org/arxiv-2409.03570","url":null,"abstract":"Gamma-ray burst (GRB) afterglows are powerful probes for studying the\u0000different properties of their host galaxies (e.g., the interstellar dust) at\u0000all redshifts. By fitting their spectral energy distribution (SED) over a large\u0000range of wavelengths, we can gain direct insights into the properties of the\u0000interstellar dust by studying the extinction curves. Unlike the dust extinction\u0000templates, such as the average Milky Way (MW) or the Small and Large Magellanic\u0000Cloud (SMC and LMC), the extinction curves of galaxies outside the Local Group\u0000exhibit deviation from these laws. Altogether, X-ray and gamma-ray satellites\u0000as well as ground-based telescopes, such as Neil Gehrels Swift Observatory\u0000(Swift) and Gamma-Ray Optical and Near-Infrared Detector (GROND), provide\u0000measurements of the afterglows from the X-ray to the NIR, which can be used to\u0000extract information on dust extinction curves along their lines of sight. The\u0000study presented in this paper undertakes such a photometric study, comprising a\u0000preparatory work for the SVOM mission and its ground-based follow-up telescope\u0000COLIBRI. We propose a simple parameterization of the dust extinction curve of\u0000GRB host galaxies. Our model is based on a power law form with the addition of\u0000a Loretzian-like Drude profile with two parameters: the extinction slope,\u0000$gamma$, and the 2175 $AA$ bump amplitude, $E_rm{b}$. Using the seven GROND\u0000filter bands, we tested our dust extinction model and explored the parameter\u0000space in extinction and redshift by fitting SEDs of simplified simulations of\u0000GRB afterglow spectra based on different extinction curve templates. From a\u0000final sample of 10 real Swift/GROND extinguished GRBs, we determined the\u0000quantities of the dust extinction in their host and measured their extinction\u0000curves. The measured average extinction curve is equivalent to a\u0000quasi-featureless in-between SMC-LMC template.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206591","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":"Indication of rapid magnetic field decay in X-ray Dim Isolated Neutron Star RX J0720.4-3125","authors":"Andrei P. Igoshev, Sergei B. Popov","doi":"arxiv-2409.03573","DOIUrl":"https://doi.org/arxiv-2409.03573","url":null,"abstract":"Magnetic field evolution of neutron stars is a long-standing debate. The rate\u0000of magnetic field decay for isolated, non-accreting neutron stars can be\u0000quantified by measuring the negative second derivative of the spin period.\u0000Alternatively, this rate can be estimated by observing an excess of thermal\u0000emission with respect to the standard cooling without additional heating\u0000mechanisms involved. One of the nearby cooling isolated neutron stars -- RX\u0000J0720.4-3125, -- offers a unique opportunity to probe the field decay as for\u0000this source there are independent measurements of the surface X-ray luminosity,\u0000the second spin period derivative, and magnetic field. We demonstrate that the\u0000evolution rate of the spin period derivative is in correspondence with the rate\u0000of dissipation of magnetic energy of the dipolar field if a significant part of\u0000the released energy is emitted in X-rays. The instantaneous time scale for the\u0000magnetic field decay is $sim 10^4$ years.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"71 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206586","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":"Chandra Discovery of a Candidate Hyper-Luminous X-ray Source in MCG+11-11-032","authors":"Adi Foord, Francesca Civano, Julia M. Comerford, Martin Elvis, Giuseppina Fabbiano, Tingting Liu, Elisabeta Lusso, Stefano Marchesi, Mar Mezcua, Francisco Muller-Sanchez, Rebecca Nevin, Kristina Nyland","doi":"arxiv-2409.03839","DOIUrl":"https://doi.org/arxiv-2409.03839","url":null,"abstract":"We present a multi-wavelength analysis of MCG+11-11-032, a nearby AGN with\u0000the unique classification of both a binary and a dual AGN candidate. With new\u0000Chandra observations we aim to resolve any dual AGN system via imaging data,\u0000and search for signs of a binary AGN via analysis of the X-ray spectrum.\u0000Analyzing the Chandra spectrum, we find no evidence of previously suggested\u0000double-peaked Fe K$alpha$ lines; the spectrum is instead best fit by an\u0000absorbed powerlaw with a single Fe K$alpha$ line, as well as an additional\u0000line centered at $approx$7.5 keV. The Chandra observation reveals faint, soft,\u0000and extended X-ray emission, possibly linked to low-level nuclear outflows.\u0000Further analysis shows evidence for a compact, hard source -- MCG+11-11-032 X2\u0000-- located 3.27'' from the primary AGN. Modeling MCG+11-11-032 X2 as a compact\u0000source, we find that it is relatively luminous ($L_{text{2$-$10 keV}} =\u00001.52_{-0.48}^{+0.96}times 10^{41}$ erg s$^{-1}$), and the location is\u0000coincident with an compact and off-nuclear source resolved in Hubble Space\u0000Telescope infrared (F105W) and ultraviolet (F621M, F547M) bands. Pairing our\u0000X-ray results with a 144 MHz radio detection at the host galaxy location, we\u0000observe X-ray and radio properties similar to those of ESO 243-49 HLX-1,\u0000suggesting that MCG+11-11-032 X2 may be a hyper-luminous X-ray source. This\u0000detection with Chandra highlights the importance of a high-resolution X-ray\u0000imager, and how previous binary AGN candidates detected with large-aperture\u0000instruments benefit from high-resolution follow-up. Future spatially resolved\u0000optical spectra, and deeper X-ray observations, can better constrain the origin\u0000of MCG+11-11-032 X2.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"2 6 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206565","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":"Prospects for Revealing Intermediate-Mass Black Holes in NGC 1399 using SKA","authors":"B. Karimi, P. Barmby, S. Abbassi","doi":"arxiv-2409.02893","DOIUrl":"https://doi.org/arxiv-2409.02893","url":null,"abstract":"This study investigates the detectability of intermediate-mass black holes\u0000(IMBHs) within the mass range $10^2-10^5$ solar masses in the globular star\u0000clusters of NGC 1399 at a frequency of 300.00 MHz. Employing the theoretical\u0000Bondi accretion model and the empirical fundamental plane of black hole\u0000accretion, we estimate IMBH masses based on bolometric luminosity and\u0000X-ray/radio luminosities, respectively. By simulating a 3-hour observation of\u000077 globular cluster candidates using the Square Kilometer Array, we identify\u0000radio detection benchmarks indicative of accretion onto IMBHs. Our results show\u0000that IMBHs inside the globular star clusters located in NGC 1399 are indeed\u0000detectable, with the Bondi accretion model providing IMBH mass estimates\u0000ranging from $2.93 times 10^{3.0pm 0.39}$ to $7.43 times 10^{4.0 pm 0.39}$\u0000solar masses, and the empirical fundamental-plane relation suggesting IMBH mass\u0000estimation with $3.41times 10^{5.0 pm 0.96}$ solar masses. These findings\u0000highlight the presence and detectability of IMBHs in globular clusters,\u0000offering insights into their role as precursors to supermassive black holes and\u0000enriching our understanding of black hole formation and evolution in\u0000astrophysical environments.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206614","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":"Theoretical modelling of the exceptional GRB 221009A afterglow","authors":"L. Foffano, M. Tavani, G. Piano","doi":"arxiv-2409.02859","DOIUrl":"https://doi.org/arxiv-2409.02859","url":null,"abstract":"The extraordinary gamma-ray burst GRB 221009A provides a great opportunity to\u0000investigate the enigmatic origin and evolution of GRBs. However, the complexity\u0000of the observations associated with this GRB provides significant challenges to\u0000develop a theoretical modeling in a coherent framework. In this paper, we\u0000present a theoretical interpretation of the GRB 221009A afterglow within the\u0000relativistic fireball scenario, aiming to describe the broad-band dataset with\u0000a consistent model evolution. We find that the adiabatic fireball evolution in\u0000the slow-cooling regime provides a viable scenario in good agreement with\u0000observations. Crucial to our analysis is the set of simultaneous GeV and TeV\u0000gamma-ray data obtained by AGILE and LHAASO during the early afterglow phases.\u0000Having successfully modelled as inverse Compton emission the high-energy\u0000spectral and lightcurve properties of the afterglow up to $10^4$ s, we extend\u0000our model to later times when also optical and X-ray data are available. This\u0000approach results in a coherent physical framework that successfully describes\u0000all observed properties of the afterglow up to very late times, approximately\u0000$10^6$ s. Our model requires time-variable microphysical parameters, with a\u0000moderately increasing efficiency $varepsilon_e$ of a few percent for\u0000transferring the shock energy to radiating particles, and a decreasing\u0000efficiency for magnetic field generation $varepsilon_B$ in the range $10^{-5}$\u0000to $10^{-7}$. Fitting the detailed multi-frequency spectral data across the\u0000afterglow provides a unique test of our model.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"3 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206589","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":"The vela supernova remnant: The unique morphological features of jittering jets","authors":"Noam SokerTechnion, Israel, Dmitry ShishkinTechnion, Israel","doi":"arxiv-2409.02626","DOIUrl":"https://doi.org/arxiv-2409.02626","url":null,"abstract":"We identify an S-shaped main-jet axis in the Vela core-collapse supernova\u0000(CCSN) remnant (CCSNR) that we attribute to a pair of precessing jets, one of\u0000the tens of pairs of jets that exploded the progenitor of Vela according to the\u0000jittering jets explosion mechanism (JJEM). A main-jet axis is a symmetry axis\u0000across the CCSNR and through the center. We identify the S-shaped main-jet axis\u0000by the high abundance of ejecta elements, oxygen, neon, and magnesium. We bring\u0000the number of identified pairs of clumps and ears in Vela to seven, two pairs\u0000shaped by the pair of precessing jets that formed the main-jet axis. The pairs\u0000and the main-jet axis form the point-symmetric wind-rose structure of Vela. The\u0000other five pairs of clumps/ears do not have signatures near the center, only on\u0000two opposite sides of the CCSNR. We discuss different possible jet-less shaping\u0000mechanisms to form such a point-symmetric morphology and dismiss these\u0000processes because they cannot explain the point-symmetric morphology of Vela,\u0000the S-shaped high ejecta abundance pattern, and the enormous energy to shape\u0000the S-shaped structure. Our findings strongly support the JJEM and further\u0000severely challenge the neutrino-driven explosion mechanism.","PeriodicalId":501343,"journal":{"name":"arXiv - PHYS - High Energy Astrophysical Phenomena","volume":"10 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142206590","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}