Astronomy Reports最新文献_第2页

Effect of the Pseudo Mean Motion on the Dynamics of Perturbed Elliptic Restricted Three-Body Problem

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-08 DOI: 10.1134/S1063772924700768

Bhavneet Kaur, Sapna Kumari Meena, Ram Krishan Sharma, Rajiv Aggarwal

引用次数: 0

Proton Fluxes of Solar-Type Stars with Planetary Systems

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-08 DOI: 10.1134/S1063772924700823

I. S. Savanov

{"title":"Proton Fluxes of Solar-Type Stars with Planetary Systems","authors":"I. S. Savanov","doi":"10.1134/S1063772924700823","DOIUrl":"10.1134/S1063772924700823","url":null,"abstract":"The previously developed method for estimating of the parameters of proton fluxes from flare energies for the Sun has been applied to data on the flare activity of solar-type stars. The obtained results will be used to estimate the radiation situation in a stellar system containing exoplanets. In our analysis, we have used catalog data on flares of solar-type stars obtained from observations with Kepler telescope. The empirical relations between the energy of X-ray flares and the proton flux for the Sun have been extended to the case of stellar flares, similar to what has been done previously in the case of coronal mass ejections (CMEs). The used method has had limitations caused by the extension of the solar analogy to other stars as well as the uncertainties that have arisen when applying scaling methods. It has been found that the characteristic values of the proton flux for solar-type stars can be one order of magnitude higher than the estimates for the Sun. Prospects for the development of alternative methods for estimating proton fluxes in the vicinity of stars of late spectral types have been discussed (for example, by studying the behavior of Si IV and He II emission lines in the far ultraviolet range).","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 9","pages":"934 - 937"},"PeriodicalIF":1.1,"publicationDate":"2024-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1134/S1063772924700823.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142790388","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Impact of Star Flare Activity on the Structure of the Hydrogen–Helium Upper Atmosphere of Hot Jupiter

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-08 DOI: 10.1134/S1063772924700793

A. G. Zhilkin, Y. G. Gladysheva, V. I. Shematovich, G. N. Tsurikov, D. V. Bisikalo

{"title":"Impact of Star Flare Activity on the Structure of the Hydrogen–Helium Upper Atmosphere of Hot Jupiter","authors":"A. G. Zhilkin, Y. G. Gladysheva, V. I. Shematovich, G. N. Tsurikov, D. V. Bisikalo","doi":"10.1134/S1063772924700793","DOIUrl":"10.1134/S1063772924700793","url":null,"abstract":"In the paper, the impact of a stellar flare on the upper atmosphere of hot Jupiter has been studied using 1D aeronomic model. The atmosphere has been assumed to have a hydrogen–helium chemical composition, and calculations have been carried out for hot Jupiter HD 209458b. We have examined single and repeated flares, in which the flux of hard UV radiation has increased by 10, 100, and 1000 times compared to the quiescent state of the star. The active phase of the dynamic response of the atmosphere has lasted 12–15 h after the flare, and the characteristic period of relaxation to the initial state has been about a day. From the obtained results, it follows that the flare activity of solar-type stars has not had a significant effect on the evolution of the planetary atmospheres of hot Jupiters. However, the interpretation of transit observations of the disturbed atmospheres of hot Jupiters will make it possible to separate from each other the observational effects associated with the interaction of stellar flares and coronal mass ejections with the upper atmospheres and envelopes of these planets. This will make it possible to determine more accurately the parameters of the stellar wind and coronal mass ejections of solar-type parent stars.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 9","pages":"865 - 877"},"PeriodicalIF":1.1,"publicationDate":"2024-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142790390","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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

[N/C] Value as an Indicator of the Red Giant Evolution: Observed Differences between Magnetic and Non-Magnetic Giants

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-08 DOI: 10.1134/S1063772924700811

L. S. Lyubimkov, D. B. Poklad

{"title":"[N/C] Value as an Indicator of the Red Giant Evolution: Observed Differences between Magnetic and Non-Magnetic Giants","authors":"L. S. Lyubimkov, D. B. Poklad","doi":"10.1134/S1063772924700811","DOIUrl":"10.1134/S1063772924700811","url":null,"abstract":"Data concerning the [N/C] value, one of the most sensitive indicators of stellar evolution, have been analyzed for 20 red giants with magnetic fields in comparison with similar data for seven non-magnetic giants. For the most giants in question, the [N/C] value has showed a dependence on age (t) and mass (M). In particular, the [N/C] value for the most of magnetic giants decreases from 1.2 to 0.9 when (log t) increases from 8.2 to 9.8 and (M) increases from 1 to 4 ({{M}_{ odot }}). For the most of magnetic giants, the [N/C] values have been shown to be lowered (up to 0.4 dex) as compared with non-magnetic giants with the same values of (t) or (M). Such differences in the [N/C] values between these two groups of stars have been supposed to be explained by different ways of stellar evolution of red giants with magnetic fields (on the main sequence (MS) stage, the fields could be strong) and giants without magnetic fields. In particular, the magnetic field can suppress the mixing process at the MS stage already and especially in the First Dredge-Up (FDU) phase, which leads to the [N/C] lowering in magnetic giants.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 9","pages":"925 - 933"},"PeriodicalIF":1.1,"publicationDate":"2024-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142790399","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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

V839 Cep—A New Quadruple Doubly Eclipsing System

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-12-08 DOI: 10.1134/S1063772924700781

I. M. Volkov, A. S. Volkova, L. A. Bagaev

{"title":"V839 Cep—A New Quadruple Doubly Eclipsing System","authors":"I. M. Volkov, A. S. Volkova, L. A. Bagaev","doi":"10.1134/S1063772924700781","DOIUrl":"10.1134/S1063772924700781","url":null,"abstract":"New high-precision photometric measurements of the eclipsing star V839 Cep ((P{{ = 9.96}^{d}}), ({{V}_{{{text{A}} + {text{B}}}}}{{ = 9.64}^{m}}), (e = 0.07), B6 V + B7 V), which is the A component of the visual double star J21035+5925AB, have established that component B is also an eclipsing variable ((P{{ = 4.075}^{d}}), B9 V + G8 V). For component A, the apsidal rotation rate was measured to be ({{dot {omega }}_{{{text{obs}}}}} = 0.027^circ )/year, which exceeds the theoretical value under the condition of synchronism ({{dot {omega }}_{{{text{theor}}}}} = 0.021^circ )/year. The physical parameters of the component stars of the eclipsing pair A were obtained: ({{T}_{1}} = 13{kern 1pt} {kern 1pt} 200 pm 300) K, ({{M}_{1}} = (3.7 pm 0.15){{M}_{ odot }}), ({{R}_{1}} = (2.57 pm 0.05){{R}_{ odot }}), ({{T}_{2}} = 11,900 pm 250) K, ({{M}_{2}} = (3.2 pm 0.15){{M}_{ odot }}), ({{R}_{2}} = (2.42 pm 0.05){kern 1pt} {{R}_{ odot }}), and components of the eclipsing pair B: ({{T}_{1}} = 10{kern 1pt} {kern 1pt} 600 pm 200) K, ({{M}_{1}} = (2.6 pm 0.2){{M}_{ odot }}), ({{R}_{1}} = (1.97 pm 0.05){{R}_{ odot }}), ({{T}_{2}} = 5540 pm 50) K, M2 = ((0.88 pm 0.05){{M}_{ odot }}), ({{R}_{2}} = (0.84 pm 0.05){{R}_{ odot }}). The age of the system is determined to be 70 Myr with solar chemical composition. The components of star A are pulsating variable stars of the slow (beta ) Cephei (SBC) type.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 9","pages":"886 - 905"},"PeriodicalIF":1.1,"publicationDate":"2024-12-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142790398","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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

Variations in the Radiation Intensity of Pulsar B0950+08: Nine Years of Monitoring at 110 MHz 脉冲星 B0950+08 辐射强度的变化：在 110 兆赫频率上的九年监测

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700707

T. V. Smirnova, M. O. Toropov, S. A. Tyul’bashev

{"title":"Variations in the Radiation Intensity of Pulsar B0950+08: Nine Years of Monitoring at 110 MHz","authors":"T. V. Smirnova, M. O. Toropov, S. A. Tyul’bashev","doi":"10.1134/S1063772924700707","DOIUrl":"10.1134/S1063772924700707","url":null,"abstract":"Variations in the radiation intensity of pulsar B0950+08 from 2014 to 2022 with scales from minutes to years were analyzed. The observations were obtained in daily survey using the Large Phased Array (LPA) radio telescope. The high variability of radiation is shown both from pulse to pulse and on scales greater than 3 min. The average value of the estimated amplitude of these variations in 3.2 min is 25 Jy, the modulation index is unity. The average relative amplitude of the interpulse (IP) is (2.00 pm 0.28% ) of the main pulse. In individual pulses, the amplitude of the interpulse may exceed the amplitude of the main pulse (MP), but this is a rare event. Radiation is observed in almost the entire period of the pulsar. For the first time, the relative amplitude of radiation between the main pulse and the interpulse (radiation bridge) was measured. When averaging for ~10 h, it varies from 0.8 to 1.31% with an average value of (1.04 pm 0.28% ). A high correlation between MP and IP amplitude variations both when averaging profiles over 3.2 min and when averaging over years was found. This correlation is due to refractive interstellar scintillation. The frequency scale of IP diffraction interstellar scintillation was measured for the first time, and that the spectral shapes for IP and MP were shown to be well correlated and have the same frequency scale. There are strong variations in the frequency scale of scintillation ({{f}_{{{text{dif}}}}}) from session to session (time interval from one day) on scales of 200–800 kHz. The refractive scale of scintillation of 1–2 days was determined. A modulation of radiation with a characteristic scale of ~130 days, which, apparently, is also associated with refractive scintillation, was found.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 8","pages":"828 - 837"},"PeriodicalIF":1.1,"publicationDate":"2024-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142518833","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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

Non-Thermal Processes of Nitric Oxide Formation during Precipitation of Auroral Electrons into the Upper Atmospheres of Terrestrial Planets 极光电子沉降到地球星高层大气期间一氧化氮的非热形成过程

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700744

V. Shematovich, D. Bisikalo, G. Tsurikov, A. Zhilkin

{"title":"Non-Thermal Processes of Nitric Oxide Formation during Precipitation of Auroral Electrons into the Upper Atmospheres of Terrestrial Planets","authors":"V. Shematovich, D. Bisikalo, G. Tsurikov, A. Zhilkin","doi":"10.1134/S1063772924700744","DOIUrl":"10.1134/S1063772924700744","url":null,"abstract":"Nitric oxide is a potential biomarker in the N2–O2 atmospheres of terrestrial exoplanets, which can be detected by space missions, including the planned launch of the Russian Spektr-UV observatory. From observations of the Earth’s thermosphere in the polar regions, it is known that important sources of formation of this molecule are the precipitation of high-energy electrons into the planet’s atmosphere, as well as the non-thermal processes accompanying them. In this paper, we study the non-thermal processes of nitric oxide formation in the polar regions of the Earth’s upper atmosphere, as well as the atmospheres of exoplanets located in the potential habitable zone of active stars. For this purpose the following models are developed: a numerical kinetic Monte Carlo model of the interaction of energetic electrons with atmospheric gas, a kinetic Monte Carlo model of the interaction of suprathermal N(4S) atoms formed as a result of dissociation of N2 molecules by electron impact with the surrounding gas; a model of odd nitrogen chemistry with molecular and eddy diffusion. Based on results of calculations, it is confirmed that the process of dissociation of N2 by an electron impact during the interaction of the stellar wind with the atmosphere of the planet is an important source of suprathermal N atoms, which contribute to a significant increase in the non-thermal formation of NO in the N2–O2 atmospheres of terrestrial planets (both locally, in the case of a planet’s own magnetic field, and throughout the whole planet’s surface, in case of its absence). Since the column concentration of NO during flares becomes larger, therefore, the chances of detecting of nitric oxide biomarker in the atmospheres of the terrestrial-type exoplanets located in the potential habitable zone of active stars are also become larger.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 8","pages":"843 - 864"},"PeriodicalIF":1.1,"publicationDate":"2024-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142518948","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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

Analysis of Gradient Profiles and Morphology of the Vela Jr. Supernova Remnant 小维拉超新星残留物的梯度剖面和形态分析

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700690

S. A. Pronicheva, A. F. Iyudin

{"title":"Analysis of Gradient Profiles and Morphology of the Vela Jr. Supernova Remnant","authors":"S. A. Pronicheva, A. F. Iyudin","doi":"10.1134/S1063772924700690","DOIUrl":"10.1134/S1063772924700690","url":null,"abstract":"We present the study of gradient profiles of the Vela Jr. northwestern rim in X-ray emission and the morphology of this supernova remnant in various spectral ranges of electromagnetic radiation to estimate the distance to the object and its age. This work involves radiation intensity spatial distributions for the northwestern rim of the supernova remnant RX J0852.0–4622 in the X-ray energy range, 1000.0–2000.0 eV, obtained from measurements of the EPIC-pn camera of the XMM-Newton space observatory for four consecutive time intervals. From the calculated shifts over the period from 2004 to 2018 of the X-ray intensity profiles along the northwestern rim of Vela Jr., limits were obtained on the angular expansion rate of the shock wave of this remnant’s region into a cloud of gas, probably hydrogen: minimum speed (V_{theta }^{{{text{max}}}}) = 0.29('' ) ± 0.04('' ) year–1 and maximum (V_{theta }^{{60}}) = 0.82('' ) ± 0.11('' ) year–1. The hydrogen cloud with which the supernova shock wave interacts along the northwestern rim of Vela Jr. is very inhomogeneous. The upper limits for the age of the remnant and the distance to it based on the cloud density estimate are 1920 years and 450 pc, respectively. More stringent restrictions on such parameters of RX J0852.0–4622 as its age and distance to it were obtained by analyzing the remnant’s two-ring morphology based on its images in ultraviolet, X-ray, radio and gamma rays: 1190 ± 250 years and 280 ± 60 pc.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 8","pages":"818 - 827"},"PeriodicalIF":1.1,"publicationDate":"2024-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142518949","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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

Relative Distances and Peculiar Velocities of 140 Groups and Clusters of Galaxies at Low Redshifts: the Hubble Diagram 低红移下 140 个星系群和星系团的相对距离和奇异速度：哈勃图

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700756

F. G. Kopylova, A. I. Kopylov

{"title":"Relative Distances and Peculiar Velocities of 140 Groups and Clusters of Galaxies at Low Redshifts: the Hubble Diagram","authors":"F. G. Kopylova, A. I. Kopylov","doi":"10.1134/S1063772924700756","DOIUrl":"10.1134/S1063772924700756","url":null,"abstract":"To determine the relative distances and peculiar velocities of 140 groups and clusters of galaxies at low redshifts (z < 0.12), we used the fundamental plane (FP) of early-type galaxies (from the Sloan Digital Sky Survey (SDSS) data). We constructed the Hubble diagram for the relative distances of galaxy groups/clusters versus their radial velocities in the cosmic microwave background (CMB) reference frame in the flat Λ cold dark matter (ΛLCDM) model (Ωm = 0.3 and H0 = 70 km s–1 Mpc–1). We have found that the standard logarithmic deviation for groups and clusters of galaxies on the Hubble diagram (minus peculiar velocities) is ±0.0173 (N = 140), which corresponds to a deviation of 70 ± 2.8 km s–1 Mpc–1 in the Hubble constant. For a sample of galaxy systems (N = 63), the X-ray luminosity of which is in an interval of (0.151‒4) × 1044 erg/s, this quantity turned out to be 70 ± 2.1 km s–1 Mpc–1. The root-mean-square deviations of peculiar velocities with quadratic accounting for errors are ({{langle V_{{{text{pec}}}}^{2}rangle }^{{1/2}}}) = 714 ± 7 and 600 ± 7 km/s, respectively. For five large superclusters of galaxies from the SDSS region, the average peculiar velocity relative to the CMB reference frame is +240 ± 250 km/s. We detected no outflow of galaxy systems from the void (Giant Void; α ≈ 13h, δ ≈ 40°, and z ≈ 0.107) formed by groups and clusters of galaxies.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 8","pages":"761 - 770"},"PeriodicalIF":1.1,"publicationDate":"2024-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142518646","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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 Survey of High-Mass Star Forming Regions in the Line of Singly Deuterated Ammonia NH2D 单氘化氨 NH2D 线高质量恒星形成区调查

IF 1.1 4区物理与天体物理

Astronomy Reports Pub Date : 2024-10-25 DOI: 10.1134/S1063772924700719

E. A. Trofimova, I. I. Zinchenko, P. M. Zemlyanukha, M. Thomasson

{"title":"A Survey of High-Mass Star Forming Regions in the Line of Singly Deuterated Ammonia NH2D","authors":"E. A. Trofimova, I. I. Zinchenko, P. M. Zemlyanukha, M. Thomasson","doi":"10.1134/S1063772924700719","DOIUrl":"10.1134/S1063772924700719","url":null,"abstract":"The present survey represents a continuation of our study of high mass star forming regions in the lines of deuterated molecules, the first results of which were published in [1]. This paper present the results of observations of 50 objects in the line of ortho modification of singly deuterated ammonia NH2D (1_{{11}}^{s}{-} 1_{{01}}^{a}) at a frequency of 85.9 GHz, carried out using the 20-m radio telescope of the Onsala Space Observatory (Sweden). This line is detected in 29 sources. The analysis of obtained data, as well as the fact that the gas density in the investigated sources, according to independent estimates, is significantly lower than the critical density for this NH2D transition, indicate non-LTE excitation of NH2D. Based on non-LTE modeling, estimates of the relative content of the NH2D molecule and the degree of deuterium enrichment were obtain, and the dependencies of these parameters on temperature and velocity dispersion were analyzed with and without taking into account detection limits assuming the same gas density in all sources. An anti-correlation between the NH2D relative abundances and the kinetic temperature is revealed in a temperature range of 15–50 K. At the same time, a significant decrease in the ratio of the NH2D/NH3 abundances with increasing temperature, predicted by the available chemical models, is not observed under the adopted assumptions. An anti-correlation was also revealed between the relative content of the main isotopologue of ammonia NH(_{3}) and the velocity dispersion, while no statistically significant correlation with the kinetic temperature of sources in the same temperature range was found.","PeriodicalId":55440,"journal":{"name":"Astronomy Reports","volume":"68 8","pages":"771 - 789"},"PeriodicalIF":1.1,"publicationDate":"2024-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142518647","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"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