Astrophysical Journal Letters最新文献_第8页

Bursty Star Formation Naturally Explains the Abundance of Bright Galaxies at Cosmic Dawn 爆炸恒星的形成自然地解释了宇宙黎明中明亮星系的丰富

1区物理与天体物理

Astrophysical Journal Letters Pub Date : 2023-10-01 DOI: 10.3847/2041-8213/acf85a

Guochao Sun, Claude-André Faucher-Giguère, Christopher C. Hayward, Xuejian Shen, Andrew Wetzel, Rachel K. Cochrane

{"title":"Bursty Star Formation Naturally Explains the Abundance of Bright Galaxies at Cosmic Dawn","authors":"Guochao Sun, Claude-André Faucher-Giguère, Christopher C. Hayward, Xuejian Shen, Andrew Wetzel, Rachel K. Cochrane","doi":"10.3847/2041-8213/acf85a","DOIUrl":"https://doi.org/10.3847/2041-8213/acf85a","url":null,"abstract":"Abstract Recent discoveries of a significant population of bright galaxies at cosmic dawn <?CDATA $left(zgtrsim 10right)$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:mfenced close=\")\" open=\"(\"> <mml:mrow> <mml:mi>z</mml:mi> <mml:mo>≳</mml:mo> <mml:mn>10</mml:mn> </mml:mrow> </mml:mfenced> </mml:math> have enabled critical tests of cosmological galaxy formation models. In particular, the bright end of the galaxys’ UV luminosity functions (UVLFs) appear higher than predicted by many models. Using approximately 25,000 galaxy snapshots at 8 ≤ z ≤ 12 in a suite of FIRE-2 cosmological “zoom-in” simulations from the Feedback in Realistic Environments (FIRE) project, we show that the observed abundance of UV-bright galaxies at cosmic dawn is reproduced in these simulations with a multichannel implementation of standard stellar feedback processes, without any fine-tuning. Notably, we find no need to invoke previously suggested modifications, such as a nonstandard cosmology, a top-heavy stellar initial mass function, or a strongly enhanced star formation efficiency. We contrast the UVLFs predicted by bursty star formation in these original simulations to those derived from star formation histories (SFHs) smoothed over prescribed timescales (e.g., 100 Myr). The comparison demonstrates that the strongly time-variable SFHs predicted by the FIRE simulations play a key role in correctly reproducing the observed, bright-end UVLFs at cosmic dawn: the bursty SFHs induce order-or-magnitude changes in the abundance of UV-bright ( M UV ≲ −20) galaxies at z ≳ 10. The predicted bright-end UVLFs are consistent with both the spectroscopically confirmed population and the photometrically selected candidates. We also find good agreement between the predicted and observationally inferred integrated UV luminosity densities, which evolve more weakly with redshift in FIRE than suggested by some other models.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"30 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134933823","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 1

On the Subparsec-scale Core Composition of FR 0 Radio Galaxies fr0射电星系亚秒差距尺度核心组成研究

1区物理与天体物理

Astrophysical Journal Letters Pub Date : 2023-10-01 DOI: 10.3847/2041-8213/acf83c

Margot Boughelilba, Anita Reimer

{"title":"On the Subparsec-scale Core Composition of FR 0 Radio Galaxies","authors":"Margot Boughelilba, Anita Reimer","doi":"10.3847/2041-8213/acf83c","DOIUrl":"https://doi.org/10.3847/2041-8213/acf83c","url":null,"abstract":"Although Fanaroff-Riley (FR) type 0 radio galaxies are known to be the most numerous jet population in the local Universe, they are much less explored than the well-established class of FR I and FR II galaxies due to their intrinsic weakness. Observationally, their nuclear radio, optical and X-ray properties are comparable to the nuclear environment of FR Is. The recent detection of two FR 0s in the high-energy band suggests that like in FR Is, charged particles are accelerated there to energies that enable gamma-ray production. Up to now, only the lack of extended radio emission from FR 0s distinguishes them from FR Is. By comparing the spectral energy distribution of FR 0s with that of FR Is and in particular with that of M87 as a well-studied reference source of the FR I population, we find the broadband spectrum of FR 0s exceptionally close to M87's quiet core emission. Relying on that similarity, we apply a lepto-hadronic jet-accretion flow model to FR 0s. This model is able to explain the broadband spectral energy distribution, with parameters close to particle-field equipartition and matching all observational constraints. In this framework, FR 0s are multi-messenger jet sources, with a nature and highly magnetized environment similar to that of the naked quiet core of FR Is.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"21 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134933874","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Turbulence Properties of Interplanetary Coronal Mass Ejections in the Inner Heliosphere: Dependence on Proton Beta and Flux Rope Structure 内日球层行星际日冕物质抛射的湍流特性:对质子β和通量绳结构的依赖

1区物理与天体物理

Astrophysical Journal Letters Pub Date : 2023-10-01 DOI: 10.3847/2041-8213/acfd1c

S. W. Good, O. K. Rantala, A.-S. M. Jylhä, C. H. K. Chen, C. Möstl, E. K. J. Kilpua

{"title":"Turbulence Properties of Interplanetary Coronal Mass Ejections in the Inner Heliosphere: Dependence on Proton Beta and Flux Rope Structure","authors":"S. W. Good, O. K. Rantala, A.-S. M. Jylhä, C. H. K. Chen, C. Möstl, E. K. J. Kilpua","doi":"10.3847/2041-8213/acfd1c","DOIUrl":"https://doi.org/10.3847/2041-8213/acfd1c","url":null,"abstract":"Abstract Interplanetary coronal mass ejections (ICMEs) have low proton beta across a broad range of heliocentric distances and a magnetic flux rope structure at large scales, making them a unique environment for studying solar wind fluctuations. Power spectra of magnetic field fluctuations in 28 ICMEs observed between 0.25 and 0.95 au by Solar Orbiter and Parker Solar Probe have been examined. At large scales, the spectra were dominated by power contained in the flux ropes. Subtraction of the background flux rope fields increased the mean spectral index from −5/3 to −3/2 at kd i ≤ 10 −3 . Rope subtraction also revealed shorter correlation lengths in the magnetic field. The spectral index was typically near −5/3 in the inertial range at all radial distances regardless of rope subtraction and steepened to values consistently below −3 with transition to kinetic scales. The high-frequency break point terminating the inertial range evolved approximately linearly with radial distance and was closer in scale to the proton inertial length than the proton gyroscale, as expected for plasma at low proton beta. Magnetic compressibility at inertial scales did not show any significant correlation with radial distance, in contrast to the solar wind generally. In ICMEs, the distinctive spectral properties at injection scales appear mostly determined by the global flux rope structure while transition-kinetic properties are more influenced by the low proton beta; the intervening inertial range appears independent of both ICME features, indicative of a system-independent scaling of the turbulence.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"26 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135762656","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 1

PSR J1953+1844 Probably Being the Descendant of an Ultracompact X-Ray Binary PSR J1953+1844可能是超紧凑x射线双星的后代

1区物理与天体物理

Astrophysical Journal Letters Pub Date : 2023-10-01 DOI: 10.3847/2041-8213/acfe6e

Z. L. Yang, J. L. Han, W. C. Jing, W. Q. Su

引用次数: 0

Probing Reflection from Aerosols with the Near-infrared Dayside Spectrum of WASP-80b 利用WASP-80b近红外日侧光谱探测气溶胶反射

1区物理与天体物理

Astrophysical Journal Letters Pub Date : 2023-10-01 DOI: 10.3847/2041-8213/acfee9

Bob Jacobs, Jean-Michel Désert, Peter Gao, Caroline V. Morley, Jacob Arcangeli, Saugata Barat, Mark S. Marley, Julianne I. Moses, Jonathan J. Fortney, Jacob L. Bean, Kevin B. Stevenson, Vatsal Panwar

{"title":"Probing Reflection from Aerosols with the Near-infrared Dayside Spectrum of WASP-80b","authors":"Bob Jacobs, Jean-Michel Désert, Peter Gao, Caroline V. Morley, Jacob Arcangeli, Saugata Barat, Mark S. Marley, Julianne I. Moses, Jonathan J. Fortney, Jacob L. Bean, Kevin B. Stevenson, Vatsal Panwar","doi":"10.3847/2041-8213/acfee9","DOIUrl":"https://doi.org/10.3847/2041-8213/acfee9","url":null,"abstract":"Abstract The presence of aerosols is intimately linked to the global energy budget and the composition of a planet’s atmosphere. Their ability to reflect incoming light prevents energy from being deposited into the atmosphere, and they shape the spectra of exoplanets. We observed five near-infrared secondary eclipses of WASP-80b with the Wide Field Camera 3 (WFC3) aboard the Hubble Space Telescope to provide constraints on the presence and properties of atmospheric aerosols. We detect a broadband eclipse depth of 34 ± 10 ppm for WASP-80b. We detect a higher planetary flux than expected from thermal emission alone at 1.6 σ , which hints toward the presence of reflecting aerosols on this planet’s dayside, indicating a geometric albedo of A g < 0.33 at 3 σ . We paired the WFC3 data with Spitzer data and explored multiple atmospheric models with and without aerosols to interpret this spectrum. Albeit consistent with a clear dayside atmosphere, we found a slight preference for near-solar metallicities and for dayside clouds over hazes. We exclude soot haze formation rates higher than 10 −10.7 g cm −2 s −1 and tholin formation rates higher than 10 −12.0 g cm −2 s −1 at 3 σ . We applied the same atmospheric models to a previously published WFC3/Spitzer transmission spectrum for this planet and found weak haze formation. A single soot haze formation rate best fits both the dayside and the transmission spectra simultaneously. However, we emphasize that no models provide satisfactory fits in terms of the chi-square of both spectra simultaneously, indicating longitudinal dissimilarity in the atmosphere’s aerosol composition.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"160 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135963551","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Carbon-bearing Molecules in a Possible Hycean Atmosphere 可能存在的海洋大气中的含碳分子

1区物理与天体物理

Astrophysical Journal Letters Pub Date : 2023-10-01 DOI: 10.3847/2041-8213/acf577

Nikku Madhusudhan, Subhajit Sarkar, Savvas Constantinou, Måns Holmberg, Anjali A. A. Piette, Julianne I. Moses

{"title":"Carbon-bearing Molecules in a Possible Hycean Atmosphere","authors":"Nikku Madhusudhan, Subhajit Sarkar, Savvas Constantinou, Måns Holmberg, Anjali A. A. Piette, Julianne I. Moses","doi":"10.3847/2041-8213/acf577","DOIUrl":"https://doi.org/10.3847/2041-8213/acf577","url":null,"abstract":"Abstract The search for habitable environments and biomarkers in exoplanetary atmospheres is the holy grail of exoplanet science. The detection of atmospheric signatures of habitable Earth-like exoplanets is challenging owing to their small planet–star size contrast and thin atmospheres with high mean molecular weight. Recently, a new class of habitable exoplanets, called Hycean worlds, has been proposed, defined as temperate ocean-covered worlds with H 2 -rich atmospheres. Their large sizes and extended atmospheres, compared to rocky planets of the same mass, make Hycean worlds significantly more accessible to atmospheric spectroscopy with JWST. Here we report a transmission spectrum of the candidate Hycean world K2-18 b, observed with the JWST NIRISS and NIRSpec instruments in the 0.9–5.2 μ m range. The spectrum reveals strong detections of methane (CH 4 ) and carbon dioxide (CO 2 ) at 5 σ and 3 σ confidence, respectively, with high volume mixing ratios of ∼1% each in a H 2 -rich atmosphere. The abundant CH 4 and CO 2 , along with the nondetection of ammonia (NH 3 ), are consistent with chemical predictions for an ocean under a temperate H 2 -rich atmosphere on K2-18 b. The spectrum also suggests potential signs of dimethyl sulfide (DMS), which has been predicted to be an observable biomarker in Hycean worlds, motivating considerations of possible biological activity on the planet. The detection of CH 4 resolves the long-standing missing methane problem for temperate exoplanets and the degeneracy in the atmospheric composition of K2-18 b from previous observations. We discuss possible implications of the findings, open questions, and future observations to explore this new regime in the search for life elsewhere.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"12 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135996810","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 7

Multipoint Detection of GRB221009A’s Propagation through the Heliosphere GRB221009A通过日球层传播的多点探测

1区物理与天体物理

Astrophysical Journal Letters Pub Date : 2023-10-01 DOI: 10.3847/2041-8213/acf933

Andrii Voshchepynets, Oleksiy V. Agapitov, Lynn Wilson, Vassilis Angelopoulos, Samer T. Alnussirat, Michael Balikhin, Myroslava Hlebena, Ihor Korol, Davin Larson, David Mitchell, Christopher Owen, Ali Rahmati

{"title":"Multipoint Detection of GRB221009A’s Propagation through the Heliosphere","authors":"Andrii Voshchepynets, Oleksiy V. Agapitov, Lynn Wilson, Vassilis Angelopoulos, Samer T. Alnussirat, Michael Balikhin, Myroslava Hlebena, Ihor Korol, Davin Larson, David Mitchell, Christopher Owen, Ali Rahmati","doi":"10.3847/2041-8213/acf933","DOIUrl":"https://doi.org/10.3847/2041-8213/acf933","url":null,"abstract":"Abstract We present the results of processing the effects of the powerful gamma-ray burst GRB221009A captured by the charged particle detectors (electrostatic analyzers and solid-state detectors) on board spacecraft at different points in the heliosphere on 2022 October 9. To follow the GRB221009A propagation through the heliosphere, we used the electron and proton flux measurements from solar missions Solar Orbiter and STEREO-A; Earth’s magnetosphere and solar wind missions THEMIS and Wind; meteorological satellites POES15, POES19, and MetOp3; and MAVEN—a NASA mission orbiting Mars. GRB221009A had a structure of four bursts: the less intense Pulse 1—the triggering impulse—was detected by gamma-ray observatories at T 0 = 13:16:59 UT (near the Earth); the most intense Pulses 2 and 3 were detected on board all the spacecraft from the list; and Pulse 4 was detected in more than 500 s after Pulse 1. Due to their different scientific objectives, the spacecraft, whose data were used in this study, were separated by more than 1 au (Solar Orbiter and MAVEN). This enabled the tracking of GRB221009A as it was propagating across the heliosphere. STEREO-A was the first to register Pulse 2 and 3 of the GRB, almost 100 s before their detection by spacecraft in the vicinity of Earth. MAVEN detected GRB221009A Pulses 2, 3, and 4 at the orbit of Mars about 237 s after their detection near Earth. By processing the observed time delays, we show that the source location of the GRB221009A was at R.A. 288.°5, decl. 18.°5 ± 2° (J2000).","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"60 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134937019","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A Single Ejection Model of the DART/Dimorphos Debris Trail DART/二形态碎片轨迹的单次弹射模型

1区物理与天体物理

Astrophysical Journal Letters Pub Date : 2023-10-01 DOI: 10.3847/2041-8213/acfd1d

Yoonyoung Kim, David Jewitt

引用次数: 0

An ALMA-resolved View of 7000 au Protostellar Gas Ring around the Class I Source CrA-IRS 2 as a Possible Sign of Magnetic Flux Advection 围绕I类源CrA-IRS 2的7000 au原恒星气体环的alma分辨率视图，作为磁通平流的可能标志

1区物理与天体物理

Astrophysical Journal Letters Pub Date : 2023-10-01 DOI: 10.3847/2041-8213/acfca9

Kazuki Tokuda, Naofumi Fukaya, Kengo Tachihara, Mitsuki Omura, Naoto Harada, Shingo Nozaki, Ayumu Shoshi, Masahiro N. Machida

{"title":"An ALMA-resolved View of 7000 au Protostellar Gas Ring around the Class I Source CrA-IRS 2 as a Possible Sign of Magnetic Flux Advection","authors":"Kazuki Tokuda, Naofumi Fukaya, Kengo Tachihara, Mitsuki Omura, Naoto Harada, Shingo Nozaki, Ayumu Shoshi, Masahiro N. Machida","doi":"10.3847/2041-8213/acfca9","DOIUrl":"https://doi.org/10.3847/2041-8213/acfca9","url":null,"abstract":"Abstract Transferring a significant fraction of the magnetic flux from a dense cloud core is essential in the star formation process. A ringlike structure produced by magnetic flux loss has been predicted theoretically, but no observational identification has been presented. We have performed ALMA observations of the Class I protostar IRS 2 in the Corona Australis star-forming region and resolved a distinctive gas ring in the C 18 O ( J = 2–1) line emission. The center of this gas ring is ∼5000 au away from the protostar, with a diameter of ∼7000 au. The radial velocity of the gas is ≲ 1 km s −1 blueshifted from that of the protostar, with a possible expanding feature judged from the velocity-field (moment 1) map and position–velocity diagram. These features are either observationally new or have been discovered but not discussed in depth because they are difficult to explain by well-studied protostellar phenomena such as molecular outflows and accretion streamers. A plausible interpretation is a magnetic wall created by the advection of magnetic flux, which is theoretically expected in the Class 0/I phase during star formation as a removal mechanism of magnetic flux. Similar structures reported in the other young stellar sources could likely be candidates formed by the same mechanism, encouraging us to revisit the issue of magnetic flux transport in the early stages of star formation from an observational perspective.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"34 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135607004","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Metallicity and Spectral Evolution of WASP 39b: The Limited Role of Hydrodynamic Escape WASP 39b的金属丰度和光谱演化:流体动力学逃逸的有限作用

1区物理与天体物理

Astrophysical Journal Letters Pub Date : 2023-10-01 DOI: 10.3847/2041-8213/acfaec

Amy J. Louca, Yamila Miguel, Daria Kubyshkina

{"title":"Metallicity and Spectral Evolution of WASP 39b: The Limited Role of Hydrodynamic Escape","authors":"Amy J. Louca, Yamila Miguel, Daria Kubyshkina","doi":"10.3847/2041-8213/acfaec","DOIUrl":"https://doi.org/10.3847/2041-8213/acfaec","url":null,"abstract":"Abstract The recent observations on WASP-39 b by JWST have revealed hints of high metallicity within the atmosphere compared to its host star. There are various theories on how these high metallic atmospheres emerge. In this study, we closely investigate the impact of extreme escape in the form of hydrodynamic escape to see its impact on atmospheric metallicity and spectral features such as CH 4 , CO 2 and SO 2 . We perform a grid simulation, with an adapted version of MESA that includes hydrodynamic escape to fully evolve planets with similar masses and radii to the currently observed WASP-39 b estimates. By making use of (photo)chemical kinetics and radiative transfer codes, we evaluate the transmission spectra at various time intervals throughout the simulation. Our results indicate that the massive size of WASP-39 b limits the metal enhancement to a maximum of ∼1.23× the initial metallicity. When incorporating metal drag, this enhancement factor is repressed to an even greater degree, resulting in an enrichment of at most ∼0.4%. As a consequence, when assuming an initial solar metallicity, metal-enriched spectral features like SO 2 are still missing after ∼9 Gyr into the simulation. This paper, thus, demonstrates that hydrodynamic escape cannot be the primary process behind the high metallicity observed in the atmosphere of WASP-39 b, suggesting instead that a metal-enhanced atmosphere was established during its formation.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"129 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135655570","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0