New Astronomy最新文献

{"title":"In-depth analysis of the light curve and first orbital period of contact binary GM Dra","authors":"M.F. Yıldırım","doi":"10.1016/j.newast.2025.102445","DOIUrl":"10.1016/j.newast.2025.102445","url":null,"abstract":"<div><div>This study presents the light curve (LC) analysis of the GM Dra eclipsing binary (using data from TESS, SuperWASP, KWS(<span><math><msub><mrow><mi>I</mi></mrow><mrow><mi>c</mi></mrow></msub></math></span>), Hipparcos, and ASAS-SN), along with a detailed investigation of its orbital period (OP) for the first time. Photometric data obtained from five different databases were used to simultaneously analyze the system’s LC and radial velocity (RV). The LC modeling results for GM Dra reveal the object stars’ masses and radii as follows: <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>28</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>01</mn></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, <span><math><mrow><msub><mrow><mi>M</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>34</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>02</mn></mrow></math></span> M<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>1</mn></mrow></msub><mo>=</mo><mn>0</mn><mo>.</mo><mn>64</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>01</mn></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>, and <span><math><mrow><msub><mrow><mi>R</mi></mrow><mrow><mn>2</mn></mrow></msub><mo>=</mo><mn>1</mn><mo>.</mo><mn>27</mn><mo>±</mo><mn>0</mn><mo>.</mo><mn>02</mn></mrow></math></span> R<span><math><msub><mrow></mrow><mrow><mo>⊙</mo></mrow></msub></math></span>. A total of 108 eclipse times (ETs) were calculated on the basis of TESS and SuperWASP observations. These ETs are of great significance in determining the OP change. The OP of the GM Dra has been analyzed based on long-term observations, revealing that the OP of GM Dra is decreasing by 0.051 s per year. A sinusoidal variation in the period change was also identified, which may be attributed to the presence of a potential third object or magnetic activity. These findings provide significant insights into the evolutionary status (the positions of the system in the Hertzsprung–Russell (HR) diagram and logM<span><math><msub><mrow></mrow><mrow><mi>t</mi><mi>o</mi><mi>t</mi><mo>.</mo></mrow></msub></math></span>–logJ diagram were discussed) of GM Dra and the dynamics of the binary system.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102445"},"PeriodicalIF":1.9,"publicationDate":"2025-06-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144480598","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}

{"title":"Multi-point observation of a CME on August 16, 2020","authors":"Marcel Nogueira de Oliveira ,&nbsp;Carlos E. Navia ,&nbsp;Andre Asevedo Nepomuceno","doi":"10.1016/j.newast.2025.102446","DOIUrl":"10.1016/j.newast.2025.102446","url":null,"abstract":"<div><div>On August 16, 2020, at 17:12 UT, a long-duration B1.2-class flare erupted from a filament in the southeastern hemisphere, originating from an active region at <span><math><mrow><mn>32</mn><mo>°</mo></mrow></math></span>S, <span><math><mrow><mn>26</mn><mo>°</mo></mrow></math></span>E, near a large equatorial coronal hole (CH). According to LASCO coronagraph images from the L1 point, the associated CME erupted with a principal angle (PA) of approximately <span><math><mrow><mn>99</mn><mo>°</mo></mrow></math></span>, close to the ecliptic plane, and at a speed of 437 km/s. Consequently, the Lorentz force between the CH’s magnetic field and the CME deflected the CME about <span><math><mrow><mn>30</mn><mo>°</mo></mrow></math></span> northward. NOAA’s CME propagation models predicted a possible impact on Earth on August 19 around 22:00 UT. However, no signs of the CME were detected at Earth. Meanwhile, STEREO-A observed a disturbance in the solar wind around 19:00 UT, consistent with a CME impact. Considering that the magnetic field and solar wind plasma move together (i.e., under the frozen-in flux condition), and due to the Sun’s rotation, parcels of solar wind plasma spiral outward from the Sun (forming the Parker spiral). The solar wind spiral motion dragged the CME, deflecting it approximately <span><math><mrow><mn>30</mn><mo>°</mo></mrow></math></span> eastward during its propagation to 1 AU, ultimately directing it toward STEREO-A’s location. Furthermore, remote-tracking observations from the two broadband visible-light refracting camera systems (HI-1 and HI-2) aboard STEREO-A captured the CME in J-plot images, tracking it from its eruption to its impact. Additionally, the bi-directional flow of suprathermal electrons observed by STEREO-A during the first 12 h of August 19, 2020, indicates that the CME crossed a high-speed stream (HSS) sector. An isotropic flux of suprathermal electrons observed around 19:00 UT further confirms the CME’s impact in STEREO-A’s vicinity.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102446"},"PeriodicalIF":1.9,"publicationDate":"2025-06-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144480597","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}

{"title":"uvby−Hβ Photoelectric photometry of 65 A/F-type candidate stars in the Kepler field: Observations, stellar parameters and variability analysis","authors":"L. Fox-Machado ,&nbsp;J.H. Peña ,&nbsp;B. Smalley","doi":"10.1016/j.newast.2025.102436","DOIUrl":"10.1016/j.newast.2025.102436","url":null,"abstract":"<div><div>We present the results of <span><math><mrow><mi>u</mi><mi>v</mi><mi>b</mi><mi>y</mi><mo>−</mo><msub><mrow><mi>H</mi></mrow><mrow><mi>β</mi></mrow></msub><mspace></mspace></mrow></math></span> photoelectric photometry for 65 stars in the Kepler field, focusing on the study of <span><math><mi>δ</mi></math></span> Scuti, <span><math><mi>γ</mi></math></span> Doradus, and hybrid-type stars. The observing procedures and methodology used to derive the Strömgren indices and colors <span><math><mi>V</mi></math></span>, <span><math><mrow><mo>(</mo><mi>b</mi><mo>−</mo><mi>y</mi><mo>)</mo></mrow></math></span>, <span><math><msub><mrow><mi>m</mi></mrow><mrow><mn>1</mn></mrow></msub></math></span>, <span><math><msub><mrow><mi>c</mi></mrow><mrow><mn>1</mn></mrow></msub></math></span>, and <span><math><msub><mrow><mi>H</mi></mrow><mrow><mi>β</mi></mrow></msub></math></span> are described in detail. We identify dwarfs and giants within the sample and report their physical parameters. For 47 stars, <span><math><msub><mrow><mi>T</mi></mrow><mrow><mi>eff</mi></mrow></msub></math></span> and <span><math><mrow><mo>log</mo><mspace></mspace><mi>g</mi><mspace></mspace></mrow></math></span> determined from our indices were previously reported by Uytterhoeven et al. (2011), while for the remaining stars, these parameters are provided in this work. Additionally, we revisit the variability classifications of these stars by analyzing all available Kepler and TESS light curves and confirm most of the pulsation classifications assigned in previous studies.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102436"},"PeriodicalIF":1.9,"publicationDate":"2025-06-18","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144364962","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}

{"title":"Warped accretion disk with power-law models for viscosities","authors":"F.S. Mohseni,&nbsp;A. Khosravi","doi":"10.1016/j.newast.2025.102447","DOIUrl":"10.1016/j.newast.2025.102447","url":null,"abstract":"<div><div>In this paper, we investigate a thin accretion disk that is warped due to the Black hole spin using numerical methods. We assume that the two viscosity coefficients vary with radius according to a power-law model, each with different power indices. Additionally, we consider the contribution of the inner disk by applying the appropriate boundary condition. Our results indicate that the alignment of the disk is influenced by the power indices of the viscosities (n and α₁). Specifically, the vertical viscosity index is more influential than the azimuthal viscosity index. An increase in the vertical viscosity index leads to greater misalignment of the disk concerning the spin axis of the black hole. These findings suggest that, contrary to previous studies, the inner regions of the disk can remain tilted relative to the rotation axis of the black hole, even for rotating black holes with a larger Kerr parameter, specifically, <em>a</em> = 0.3. Our results help explain the observed quasi-periodic oscillation features in X-ray emissions and the Fe Kα line, which may arise from the precession of a warped inner accretion disk. This research could be valuable for exploring regions of strong gravitational fields.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102447"},"PeriodicalIF":1.9,"publicationDate":"2025-06-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144470835","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}

{"title":"Detection of CRSF in Cep X-4 at a low luminosity level","authors":"Kinjal Roy ,&nbsp;Rahul Sharma","doi":"10.1016/j.newast.2025.102435","DOIUrl":"10.1016/j.newast.2025.102435","url":null,"abstract":"<div><div>The BeXRP <!--> <em>Cep X-4</em> underwent a type II outburst during July 2023, during which <!--> <em>NuSTAR</em> made two observations of the source. In this paper, we present the spectral and timing analysis of <!--> <em>Cep X-4</em> during this outburst. Pulsations were detected from the source at the neutron star spin period of <span><math><mo>∼</mo></math></span> 66 s from both observations. We detected a CRSF feature at an energy of <span><math><mrow><mn>27</mn><mo>.</mo><msubsup><mrow><mn>3</mn></mrow><mrow><mo>−</mo><mn>1</mn><mo>.</mo><mn>0</mn></mrow><mrow><mo>+</mo><mn>1</mn><mo>.</mo><mn>5</mn></mrow></msubsup></mrow></math></span> keV in the spectrum of <!--> <em>Cep X-4</em> during the first observation. In the second observation conducted a day later when the source luminosity dropped by a factor of five, no CRSF could be detected significantly. A positive correlation between CRSF energy and luminosity was observed using data from multiple outbursts since 1998. The collisionless shock model provides a good fit to the observed variations of cyclotron line energy with luminosity, giving a surface magnetic field strength of <span><math><mrow><mo>∼</mo><mn>2</mn><mo>.</mo><mn>6</mn><mo>×</mo></mrow></math></span> <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>12</mn></mrow></msup></mrow></math></span> G.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102435"},"PeriodicalIF":1.9,"publicationDate":"2025-06-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144312619","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}

{"title":"Star formation rate estimations of a mid-infrared sample of X-ray selected nearby Active Galactic Nuclei","authors":"Angel Castro ,&nbsp;Takamitsu Miyaji ,&nbsp;Liliana Altamirano-Dévora ,&nbsp;Peter Boorman ,&nbsp;Kohei Ichikawa ,&nbsp;Matthew Malkan ,&nbsp;Héctor Aceves ,&nbsp;Yoshihiro Ueda ,&nbsp;Erika Castillo ,&nbsp;Mauricio Elías-Chavez ,&nbsp;Irene Cruz-González ,&nbsp;Martín Herrera-Endoqui ,&nbsp;Takao Nakagawa","doi":"10.1016/j.newast.2025.102433","DOIUrl":"10.1016/j.newast.2025.102433","url":null,"abstract":"<div><div>We investigate the activity of active galactic nuclei and the circumnuclear star formation properties in a nearby (<span><math><mrow><mi>z</mi><mo>≤</mo><mn>0</mn><mo>.</mo><mn>1</mn></mrow></math></span>) sample of 125 hard X-ray (14–195 keV) selected active Galactic Nuclei (AGN) from the <em>Swift</em>/BAT 70-month survey catalogue. Using the 11.3 <span><math><mrow><mi>μ</mi><mi>m</mi></mrow></math></span> polycyclic aromatic hydrocarbon (PAH) emission feature measured with the <em>Spitzer</em>/IRS instrument as a proxy for recent star formation, we examine the relationship between AGN power and circumnuclear star formation rate (SFR). We explored the SFR properties of both type-1 and type-2 AGN populations within our sample. A positive correlation is found between hard X-ray luminosity (<span><math><msub><mrow><mi>L</mi></mrow><mrow><mi>X</mi></mrow></msub></math></span>) and SFR for our sample but not for type-2 AGN alone. In comparing type-1 and type-2 sources, we found no significant differences between our sample’s low- and high-luminosity populations. For a subset of 50 AGN, we also provide <em>AKARI</em>/IRC measurements of the 3.3 <span><math><mrow><mi>μ</mi><mi>m</mi></mrow></math></span> PAH emission feature, which were used to estimate SFR. Although some correlations are present, these samples’ two types of AGN cannot be clearly distinguished based solely on their luminosity or SFR properties as indicated by their PAH emission.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102433"},"PeriodicalIF":1.9,"publicationDate":"2025-06-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144221028","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}

{"title":"Mapping the reddening plane in the Galactic disk through interstellar extinction of open clusters","authors":"Y.C. Joshi","doi":"10.1016/j.newast.2025.102425","DOIUrl":"10.1016/j.newast.2025.102425","url":null,"abstract":"<div><div>As thousands of new open clusters in the Galaxy have recently been reported with reddening or extinction information, we map the distribution and properties of the MilkyWay’s interstellar material in the Galactic disk as traced by these open clusters. By analyzing the distribution of interstellar extinction for 6215 open clusters located at low Galactic latitude (<span><math><mrow><mrow><mo>|</mo><mi>b</mi><mo>|</mo></mrow><mo>≤</mo><mn>6</mn><mo>°</mo></mrow></math></span>), corresponding to the thin Galactic disk, we identify a reddening plane characterized by a dust layer whose thickness varies with Galactic longitude. By splitting the open clusters sample into several sub-regions of Galactic longitude, we observe that the reddening plane is not perfectly aligned with the formal Galactic plane, but instead varies sinusoidally around the Galactic mid-plane. The maximum and minimum interstellar absorption occur at approximately <span><math><mrow><mn>42</mn><mo>°</mo></mrow></math></span> and <span><math><mrow><mn>222</mn><mo>°</mo></mrow></math></span>, respectively, along the Galactic longitude. Our analysis reveals a noticeable north-south asymmetry in the distribution of interstellar absorption, with a higher proportion of interstellar material below the Galactic plane. We also find that the Sun is located <span><math><mrow><mn>15</mn><mo>.</mo><mn>7</mn><mo>±</mo><mn>7</mn><mo>.</mo><mn>3</mn></mrow></math></span> pc above the reddening plane. The scale height of the open clusters from the reddening plane is estimated to be <span><math><mrow><msub><mrow><mi>z</mi></mrow><mrow><mi>h</mi></mrow></msub><mo>=</mo><mn>87</mn><mo>.</mo><mn>3</mn><mo>±</mo><mn>1</mn><mo>.</mo><mn>8</mn></mrow></math></span> pc. The mean thickness of the absorbing material in the reddening plane, which represents the average extent of the dust layer responsible for interstellar extinction, is found to be about <span><math><mrow><mn>201</mn><mo>±</mo><mn>20</mn></mrow></math></span> pc. Our findings provide insights into the distribution of interstellar dust, its relationship with the Galactic thin disk, and its implications on the Galactic structure.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102425"},"PeriodicalIF":1.9,"publicationDate":"2025-06-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144221029","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}

{"title":"A study on the formation of field, binary or multiple stars: A 3D approach through dynamical system","authors":"Ashok Mondal ,&nbsp;Tanuka Chattopadhyay","doi":"10.1016/j.newast.2025.102424","DOIUrl":"10.1016/j.newast.2025.102424","url":null,"abstract":"<div><div>We have studied a three-dimensional model using the concept of double-well potential to find out what kind of stars can be formed from filamentary molecular clouds depending on their density. We have shown the effect of both rotation and magnetic fields in the process of star formation. It is found that thin filamentary MCs can lead to the formation of field stars, and this occurs even in a rapidly rotating cloud or in a magnetized rotating cloud. In absence of a magnetic field, binary stars form from a moderately dense structure, whereas in presence of a magnetic field isolated field stars may also form. For a moderately high dense structure, the nature of stars depends on the combined effect of rotation and magnetic field strength. High dense and compressed filamentary MCs are favorable to form stellar associations or more massive star clusters.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"120 ","pages":"Article 102424"},"PeriodicalIF":1.9,"publicationDate":"2025-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144184259","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}

{"title":"Potential optical astronomical sites in less developed countries","authors":"Pedro Augusto","doi":"10.1016/j.newast.2025.102434","DOIUrl":"10.1016/j.newast.2025.102434","url":null,"abstract":"<div><div>A “suitability index for astronomical sites” (SIAS) has been proposed to more easily select the best sites in the world as regards cloud cover, elevation, and artificial light. The SIAS brings new and great potential for countries with few resources, typically less developed countries (LDCs). However, it lacks crucial quantitative astronomical <em>seeing</em> information, quite expensive to gather (for this, we have developed a new technique and portable instrument to lower the costs of measuring the seeing). Good seeing exists on the up-wind edge of a mountain top with a greater than 1:3 slope angle towards laminar flow dominating winds (coastal sites or small islands). By inspecting with Google Earth the terrain and surrounding area of each SIAS-selected candidate site as regards the mountain height and slopes, the distance from the nearest sea/lake, and its mountainous neighborhood, we have shortlisted the best 13 sites for optical astronomy in eight LDCs.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"121 ","pages":"Article 102434"},"PeriodicalIF":1.9,"publicationDate":"2025-05-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144204529","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}

{"title":"On the logarithmic parameterization for the deceleration parameter in f(Q,C)-gravity","authors":"Andronikos Paliathanasis","doi":"10.1016/j.newast.2025.102426","DOIUrl":"10.1016/j.newast.2025.102426","url":null,"abstract":"<div><div>We show that the gravitational Lagrangian introduced in Bhoyar and Ingole, (2025) is nothing else than that of the power-law <span><math><mrow><mi>f</mi><mfenced><mrow><mi>Q</mi></mrow></mfenced><mo>=</mo><msup><mrow><mi>Q</mi></mrow><mrow><mi>n</mi></mrow></msup></mrow></math></span> theory and the boundary term <span><math><mi>C</mi></math></span> plays no role in this study.</div></div>","PeriodicalId":54727,"journal":{"name":"New Astronomy","volume":"120 ","pages":"Article 102426"},"PeriodicalIF":1.9,"publicationDate":"2025-05-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144146963","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}