Astrophysics最新文献

{"title":"The Digitized First Byurakan Survey Data Base. Late-Type Stars Candidates. New Confirmations. I","authors":"K. S. Gigoyan,&nbsp;K. K. Gigoyan,&nbsp;A. Sarkissian,&nbsp;G. R. Kostandyan,&nbsp;M. Meftah,&nbsp;S. Bekki","doi":"10.1007/s10511-024-09804-7","DOIUrl":"10.1007/s10511-024-09804-7","url":null,"abstract":"<p>The Digitized First Byurakan Survey (DFBS) is the digitized version of the First Byurakan Survey (FBS, or Markarian survey). The FBS was the first systematic survey of the extragalactic sky. This objective-prism survey was carried out in 1965-1980 by B.E.Markarian and his colleagues using the 1 m Schmidt telescope of the Byurakan Astrophysical Observatory and resulted in discovery of 1517 UVX-excess (Markarian) galaxies. FBS low-resolution spectral plates have been used for a long time to search and study faint Late-Type Stars (LTS, M-type and C stars) at high Galactic latitudes. A total of 18 lists of the FBS LTS were published between 1990 and 2016. We report newly confirmed C and M giants, and also large amount of M dwarfs based on the Gaia DR3 BP/RP low-resolution spectroscopic data base. Some of the newly confirmed M dwarfs presents binary systems. Some of them are new eclipsing binaries. In our previous studies of the DFBS spectral plates, all were presented as LTS candidates. Gaia high-accuracy astrometric and photometric data and Transiting Exoplanet Survey Satellite (TESS) data are used to characterize these new confirmed LTS. TESS phase-dependent light curves show rotational modulations and flares for many new M dwarfs. This confirmations of the large number of completely new objects represents a very significant extension in the census of M giants, faint N-type Asymptotic Giant Branch C stars, CH-type C giants at high Galactic latitudes, and M dwarfs in the solar vicinity. Some objects are located more than 7 kpc from the Galactic plane. Ultimately, we aim to present value-added catalog and update the FBS LTS catalog. Note that a large amount of the blue stellar objects with UVX-excess and numerous of emission line objects were also detected.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"470 - 484"},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139469222","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":"Mass Loss from the Atmosphere of the Planet WASP-193 b","authors":"I. S. Savanov","doi":"10.1007/s10511-024-09803-8","DOIUrl":"10.1007/s10511-024-09803-8","url":null,"abstract":"<p>Results are presented from an analysis of the manifestations of activity of the star WASP-193 of spectral class F9 with a super-neptune-type planet. The gaseous giant WASP-193 b with a mass 0.13 times Jupiter’s mass and almost one and a half times its radius. The planet has a low density ρ = 0.059±0.014 g/cm³ (Kepler 51 d is an analogous object; there are few other exoplanets of this type). The equilibrium temperature of the atmosphere of the planet is high at <i>T</i>_<i>eq</i> = 1254±31 K. The results of this study of the star’s activity are used to estimate the loss of matter by the atmosphere of the planet WASP-193 b using an approximation formula corresponding to a model with limited energy. Estimates of the flux of XUV-photons <i>F</i>_<i>XUV</i> were made using an analytical relationship relating <i>F</i>_<i>XUV</i> and the parameter <span>({text{log}}{R}_{HK}{prime})</span> for stars in classes F-M. Calculations showed that the loss of matter from the atmosphere of the exoplanet is quite high (even in the case of a low chromospheric activity of the parent star). The parameter <span>(dot{M})</span> ranges from 1.8∙10¹⁰ g/s to 4.3∙10¹¹ g/s, depending on the assumed level of the flux of XUV-photons (high and low activity). It is probable that the planet is losing its atmosphere intensively. WASP-193 b can be regarded as a high-priority candidate for observations using the JWST space mission (the transmission spectroscopy metric TSM for this object is about 600).</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"463 - 469"},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139471102","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":"Viscous Ricci Dark Energy Cosmological Models in Brans-Dicke Theory","authors":"M. Vijaya Santhi,&nbsp;T. Chinnappalanaidu,&nbsp;S. Srivani Madhu","doi":"10.1007/s10511-024-09810-9","DOIUrl":"10.1007/s10511-024-09810-9","url":null,"abstract":"<p>The whole article deals with the analysis of the cosmic model of Ruban’s space-time in the context of a bulk viscosity impact in the form of Ricci dark energy within the framework Brans-Dicke theory. We believe that outer space is filled with dark matter and viscous Ricci dark energy (VRDE) under the pressureless situation. The velocity and rate at which the Universe is expanding are presumed to be proportional to the coefficient of total bulk viscosity, is in the form, <span>({upxi }_{0}+{upxi }_{1}dot{a}/a+{upxi }_{2}ddot{a}/a,)</span> where <span>({upxi }_{0},{upxi }_{1})</span> and <span>({upxi }_{2})</span> are the constants. To solve the RDE model's field equations, we utilize the relation among the metric potentials and also the power-law relation among the average scale factor <i>a</i>(<i>t</i>) and scalar field ϕ. To examine the evolutionary dynamics of the Universe, we investigate the deceleration parameter <i>q</i>, jerk parameter <i>j</i>, EoS parameter <span>({upomega }_{de},)</span> Om(<i>z</i>) , stability of the obtained models through the square speed of the sound <span>({v}_{s}^{2},{upomega }_{de}-{omega }_{de}{prime})</span> plane, statefinder parameter planes (<i>r</i>, <i>s</i>) and (<i>q</i>, <i>r</i>) and presented via graphical representation. By the end of the discussion, VRDE model was found to be compatible with the present accelerated expansion of the Universe.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"559 - 589"},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139471051","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":"Structure of the Magnetic Field of the Star HD133880 (Si)","authors":"Yu. V. Glagolevskij","doi":"10.1007/s10511-024-09806-5","DOIUrl":"10.1007/s10511-024-09806-5","url":null,"abstract":"<p>The magnetic field of the star HD133880 is modeled assuming a magnetic field structure that is described by two theoretical magnetic dipoles. A comparison of this result with what was found previously using a representation of the phase dependence <i>Be</i>(Φ) employing a dipole+quadrupole+octupole expansion for the structure shows that this scheme leads only to a formal description of the phase dependence, while the terms in the expansion lack physical significance.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"503 - 515"},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139471291","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":"Periodicity of Flare Frequency of Active Flare Stars Detected by Tess","authors":"A. A. Akopian","doi":"10.1007/s10511-024-09807-4","DOIUrl":"10.1007/s10511-024-09807-4","url":null,"abstract":"<p>Data from the TESS orbital observatory are used to study the most active flare stars indicating 100 or more flares during the period from July 2018 through October 2020. The main objectives of this study were: (a) analysis of the light curves, determination of the axial rotation periods, and identification of physical features in individual stars, (b) determination of the parameters of the periodic/cyclical variability of the flare frequencies of flare stars owing to axial/orbital rotations. The corresponding periods of the flare frequency functions were obtained and compared with the axial rotation periods of the stars. The periods of the frequency functions of the flares turned out to be close to the axial rotation periods of the stars. Theoretical phase distributions of the flares are constructed and compared with analogous observations of the flares for the given period. For all the stars without exception, a comparison with the aid of the χ² criterion confirms the periodicity of the flare frequency. It is proposed that the distribution of spots over the longitude of flare stars can be represented by an angular von Mises distribution, for which the parameters are determined by the corresponding parameters of the flare frequency function. The binarity of the star CD-56 1032 is discussed in detail.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"516 - 531"},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139469135","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":"Photometric and Spectral Studies of the Group of Galactic Wolf-Rayet Stars. I. WN Sequence","authors":"L. N. Kondratyeva,&nbsp;I. V. Reva,&nbsp;E. K. Denissyuk,&nbsp;S. A. Shomshekova,&nbsp;G. K. Aimanova","doi":"10.1007/s10511-024-09805-6","DOIUrl":"10.1007/s10511-024-09805-6","url":null,"abstract":"<p>Photometric and spectral observations of 11 Wolf-Rayet stars of the WN sequence were made at the AFIF during 2021-2022. Estimates of the brightness of objects in BVRc filters and the absolute fluxes of radiation in emission lines in this group are obtained on the basis of these observations. Changes in the brightness over a range of 0^m.1-0^m.15 are recorded for the stars WR 120, WR 151, and WR 152 in the WR I stars. Changes in the emission fluxes are detected in the spectra of several objects: WR 120, WR 128, and WR 145.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"485 - 502"},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139469272","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 Search for New Dwarf Galaxies Outside the Nearby Groups","authors":"I. D. Karachentsev,&nbsp;V. E. Karachentseva,&nbsp;S. S. Kaisin,&nbsp;E. I. Kaisina","doi":"10.1007/s10511-024-09801-w","DOIUrl":"10.1007/s10511-024-09801-w","url":null,"abstract":"<p>We undertook a search for new nearby dwarf galaxies outside the known groups in the Local Volume using the data on DESI Legacy Imaging Surveys. In a wide sky area of ~5000 square degrees directed toward the Local Void, we found only 12 candidates to nearby low mass galaxies. Almost all of them are classified as irregular or transition type dwarfs. Additionally, we examined areas of the sky exposed with the Hyper Suprime Camera of the Subaru telescope (~700 square degrees) and found nine more candidates to nearby dwarfs. Finally, nine candidates to the Local Volume were selected by us from the Zaritsky’s SMUDG catalog that contains 7070 ultra-diffuse objects automatically detected in the whole area of the DESI surveys. We estimated a fraction of quiescent dSph galaxies in the general cosmic field to be less than 10 percent.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"441 - 451"},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139469209","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":"Transverse Gradients of Longitudinal Magnetic Field in Active Regions with Different Levels of Flare Productivity. I. Calculation Methods and Dynamics of Selected Parameters","authors":"Yu. A. Fursyak","doi":"10.1007/s10511-024-09808-3","DOIUrl":"10.1007/s10511-024-09808-3","url":null,"abstract":"<p>This paper is a study of the dynamics of the parameters describing the transverse component of the gradient of the longitudinal magnetic field ∇_⊥ <i>B</i>_<i>z</i> in active regions (AR) with different levels of flare productivity. Data obtained by the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) has been used to analyze 75 ARs in the 24-th cycle of solar activity. ∇_⊥ <i>B</i>_<i>z</i> has been calculated using two approaches, modern and classical. In each case the parameters describing the quantity ∇_⊥ <i>B</i>_<i>z</i> in the AR are determined. For the modern approach, this includes the average of ∇_⊥ <i>B</i>_<i>z</i> over the AR, &lt;∇_⊥ <i>B</i>_<i>z</i>&gt; and the average value of ∇_⊥ <i>B</i>_<i>z</i> in the neighborhood of the point with its maximum value, &lt;max ∇_⊥ <i>B</i>_<i>z</i>&gt;; for the classical approach, the maximum value of ∇_⊥ <i>B</i>_<i>z</i> between pairs of spots in the AR, &lt;max ∇_⊥ <i>B</i>_<i>z</i>&gt;. The dynamics of the chosen parameters are studied over the time of monitoring each of the regions of the analyzed sample. It is shown that: 1. the spread in values of ∇_⊥ <i>B</i>_<i>z</i> is small (for the overwhelming majority of studied regions it lies within a range of 0.08-0.12 G·km^-1) and differs little for regions with low and high flare activity. 2. The numerical values of the parameter max(∇_⊥ <i>B</i>_<i>z</i>) and its dynamics in the overwhelming majority of examined cases are greater in regions with a higher level of flare activity. 3. The numerical values of the parameter max(∇_⊥ <i>B</i>_<i>z</i>) and its dynamics are greater in regions with higher levels of flare activity. 4. In the AR NOAA 11283 a stable rise in the magnitude of max (∇_⊥ <i>B</i>_<i>z</i>)_<i>sp</i> was detected for approximately 19 h before the development of the first of a series of flares in high x-ray classes.</p>","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"66 4","pages":"532 - 549"},"PeriodicalIF":0.6,"publicationDate":"2024-01-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139469055","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":"Поперечные градиенты продольного магнитного поля в активных областях с разным уровнем вспышечной продуктивности. I. Методы вычисления и динамика выбранных параметров","authors":"Ю. А. Фурсяк","doi":"10.54503/0002-3051-2023.76.4-571","DOIUrl":"https://doi.org/10.54503/0002-3051-2023.76.4-571","url":null,"abstract":"Поступила 20 июля 2023 Принята к печати 28 ноября 2023 Задача исследования - изучение динамики параметров, описывающих поперечную составляющую градиента продольного магнитного поля z B   в активных областях (АО) с разным уровнем вспышечной продуктивности. Используя данные, полученные инструментом Helioseismic and Magnetic Imager (HMI) на борту Solar Dynamics Observatory (SDO), проанализированы 75 АО 24-го цикла солнечной активности. Для вычисления величины z B   применены два подхода - современный и классический. В каждом случае определены параметры, описывающие величину z B   в АО. Для современного подхода это средняя z B   по АО величина - z B   и средняя величина z B   в окрестности точки с максимальным его значением - max Bz , для классического подхода - максимальное значение z B   между парами пятен в АО - z sp max ( B )   . Изучена динамика выбранных параметров за время мониторинга каждой из областей анализируемой выборки. Показано, что: 1. Разброс значений величины z B   небольшой (для подавляющего большинства исследуемых областей находится в пределах 0.08-0.12 Гс км-1) и мало различается для областей с низкой и высокой вспышечной продуктивностью. 2. Численные значения параметра max ( ) z B   и его динамика в подавляющем большинстве рассмотренных случаев больше в областях с более высоким уровнем вспышечной продуктивности. 3. Численные значения параметра z sp max ( B )   и его динамика больше в областях с более высоким уровнем вспышечной продуктивности. 4. В АО NOAA 11283 зафиксирован стабильный рост величины z sp max ( B )   приблизительно за 19 ч до начала развития первой из серии вспышек высоких рентгеновских классов. Ключевые слова: Солнце: активные области: вспышечная активность: магнитное поле: градиенты магнитного поля․\u0000The aim of this work is to study the dynamics of parameters describing the transverse component of the longitudinal magnetic field gradient  Bz in active regions (ARs) with different levels of flare productivity. The data obtained by the Helioseismic and Magnetic Imager (HMI) instrument onboard the Solar Dynamics Observatory (SDO) was used to analyse 75 ARs of the 24th cycle of solar activity. To calculate the value of  Bz , two approaches are applied - modern and classical. In each case, the parameters describing the quantity  Bz in the AO are determined. For the modern approach, these are the  Bz AR-averaged value  Bz and the  Bz average value in the vicinity of the point with its maximum value max Bz , for the classical approach is the maximum value between pairs of spots in the AR max Bz sp . The dynamics of the selected parameters during the monitoring time of each of the ARs of the analyzed sample was studied. It is shown that: 1. The scatter of  Bz values is small (for the vast majority of the studied ARs it is within 0.08-0.12 G km-1) and differs little for ARs with low and high flare productivity. 2. Numerical values of the parameter max Bz and its dynamics in the","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"47 5","pages":""},"PeriodicalIF":0.5,"publicationDate":"2023-12-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138949464","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":"Novel Planetary Signatures From The Dark Universe","authors":"K. Zioutas, V. Anastassopoulos, A. Argiriou, G. Cantatore, S. Cetin, A. Gardikiotis, H. Haralambous, M. Karuza, A. Kryemadhi, M. Maroudas, A. Mastronikolis, C. Oikonomou, K. Ozbozduman, Y. Semertzidis, M. Tsagri, I. Tsagris","doi":"10.54503/0002-3051-2023.76.4-591","DOIUrl":"https://doi.org/10.54503/0002-3051-2023.76.4-591","url":null,"abstract":"\"Dunkle Materie\" (DM) came from unexpected cosmological observations. Nowadays within our solar system, diverse observations also defy conventional explanations, like the main physical process(es) underlying the heating of the different solar atmospheric layers. Streaming DM offers a viable common scenario following gravitational focusing by the solar system bodies. This fits as the underlying process behind the solar cycle, which was the first signature suggesting a planetary dependency. The challenge, since 1859, is to find a remote planetary impact, beyond the extremely feeble planetary tidal force. We stress the possible involvement of an external impact by some overlooked \"streaming invisible matter\", which reconciles all investigated mysterious observations mimicking a not extant remote planetary force. Unexpected planetary relationships exist for both the dynamic Sun and Earth, reflecting multiple signatures for streaming DM. The local reasoning à la Zwicky is also suggestive for searches including puzzling biomedical phenomena. Favourite DM candidates are anti-quark-nuggets, magnetic monopoles, dark photons, or the composite \"pearls\". Then, anomalies within the solar system are the manifestation of the dark Universe. The tentative streaming DM scenario enhances spatiotemporally the DM flux favouring conditions for direct DM detection or extracting energy from the not-so-invisible as anticipated dark sector.\u0000Понятие темной материи (DM) введено для объяснения неожиданных результатов космологических наблюдений. В настоящее время разные явления, наблюдаемые в нашей солнечной системе, также не поддаются традиционным объяснениям, например, основные физические процессы, лежащие в основе нагрева различных слоев солнечной атмосферы. Концепция потоков DM с их последующей гравитационной фокусировкой телами Солнечной системы предлагает жизнеспособный общий сценарий для понимания таких явлений. Возможно это основной процесс, ответственный за солнечные циклы, у которых были обнаружены первыe признаки зависимости от параметров планет. Уже в 1859г. была поставлена задача найти удаленное планетарное воздействие, отличное от чрезвычайно слабой планетарной приливной силы. Мы подчеркиваем возможную причастность внешнего воздействия неучтенного \"потока невидимой материи\", что согласуется со всеми загадочными наблюдениями, ранее исследованными с привлeчением несуществующей удаленной планетарной силы. Множество следов \"потоковой\" ТМ проявляются в разного рода неожиданных связах, как динамического Солнца, так и и Земли. В частности, рассуждение в духе Цвикки наводит на размышления о поиске загадочных биомедицинских явлений. Предпочтительными носителями ТМ являются - крупицы антикварковой материи, магнитные монополи, темные фотоны или составные \"жемчужины\". Таким образом, аномалии внутри Солнечной системы являются проявлениями темной Вселенной. Неявный сценарий потока темной материи расширяет пространственно- временное распределение темной материи, создавая лучши","PeriodicalId":479,"journal":{"name":"Astrophysics","volume":"43 20","pages":""},"PeriodicalIF":0.5,"publicationDate":"2023-12-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"138949626","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}