Pub Date : 2023-04-01DOI: 10.22201/ia.01851101p.2023.59.01.05
L. Santos, A. K. D. Almeida, P. Sousa-Silva, M. O. Terra, D. M. Sanchez, S. Aljbaae, A. Prado, F. Monteiro
In this article, equilibrium points and families of periodic orbits in the vicinity of the collinear equilibrium points of a binary asteroid system are investigated with respect to the angular velocity of the secondary body, the mass ratio of the system and the size of the secondary. We assume that the gravitational fields of the bodies are modeled considering the primary as a mass point and the secondary as a rotating mass dipole. This model allows to compute families of planar and halo periodic orbits that emanate from the equilibrium points L1 and L2. The stability and bifurcations of these families are analyzed and the results are compared with the results obtained with the restricted three-body problem (RTBP). The results provide an overview of the dynamical behavior in the vicinity of a binary asteroid system.
{"title":"NUMERICAL INVESTIGATIONS OF THE ORBITAL DYNAMICS AROUND A SYNCHRONOUS BINARY SYSTEM OF ASTEROIDS","authors":"L. Santos, A. K. D. Almeida, P. Sousa-Silva, M. O. Terra, D. M. Sanchez, S. Aljbaae, A. Prado, F. Monteiro","doi":"10.22201/ia.01851101p.2023.59.01.05","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.01.05","url":null,"abstract":"In this article, equilibrium points and families of periodic orbits in the vicinity of the collinear equilibrium points of a binary asteroid system are investigated with respect to the angular velocity of the secondary body, the mass ratio of the system and the size of the secondary. We assume that the gravitational fields of the bodies are modeled considering the primary as a mass point and the secondary as a rotating mass dipole. This model allows to compute families of planar and halo periodic orbits that emanate from the equilibrium points L1 and L2. The stability and bifurcations of these families are analyzed and the results are compared with the results obtained with the restricted three-body problem (RTBP). The results provide an overview of the dynamical behavior in the vicinity of a binary asteroid system.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2023-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48587787","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}
Pub Date : 2023-04-01DOI: 10.22201/ia.01851101p.2023.59.01.09
R. Michel, C. Barani, M. Martignoni, F. Acerbi, L. Altamirano-Dévora
The results of our study of the eclipsing binary systems AF LMi, CzeV188 and CRTS J073333.0+302556 based on new CCD B, V, RC, IC complete light curves, are here presented. The short periods of these systems are confirmed and revised. The light curves were modeled using the latest version of the WilsonDevinney code and, as a result, we found that AF LMi (G3+G9) and CzeV188 (K0+K1) are W UMa-type contact binary systems belonging to the W subclass, showing a shallow degree of fill-out with components in good thermal contact. CRTS J073333.0+302556 is a detached binary system composed by a late dwarf (K8) and an M6 dwarf spectral type components. The asymmetries of the light curves were accounted for with a spot on the surface of one of the component. The absolute elements of the three objects were estimated.
{"title":"PHOTOMETRIC STUDY OF TWO CONTACT BINARY SYSTEMS AND A DETACHED LATE DWARF + M DWARF COMPONENTS","authors":"R. Michel, C. Barani, M. Martignoni, F. Acerbi, L. Altamirano-Dévora","doi":"10.22201/ia.01851101p.2023.59.01.09","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.01.09","url":null,"abstract":"The results of our study of the eclipsing binary systems AF LMi, CzeV188 and CRTS J073333.0+302556 based on new CCD B, V, RC, IC complete light curves, are here presented. The short periods of these systems are confirmed and revised. The light curves were modeled using the latest version of the WilsonDevinney code and, as a result, we found that AF LMi (G3+G9) and CzeV188 (K0+K1) are W UMa-type contact binary systems belonging to the W subclass, showing a shallow degree of fill-out with components in good thermal contact. CRTS J073333.0+302556 is a detached binary system composed by a late dwarf (K8) and an M6 dwarf spectral type components. The asymmetries of the light curves were accounted for with a spot on the surface of one of the component. The absolute elements of the three objects were estimated.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2023-04-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"47449101","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}
Pub Date : 2023-01-31DOI: 10.22201/ia.01851101p.2023.59.01.10
V. Kudak, vS.Parimucha, V. Perig, Pavol Gajdoš
We present the photometric analysis of BVR and TESS light curves of three eclipsing binaries, together with their period changes considering archival data and new minima times from our and TESS observations. For the first time we detected wave-like variations with low-amplitude in O − C residua of RU UMi, which can be interpreted as a consequence of the light-time effect caused by the 3rd component with period 7370 days. The period increase detected in the VY UMi system corresponds to mass transfer from the secondary to the primary component. For the GSC 04364-00648 binary system we find quadratic changes on the O − C diagram, which correspond to a period decrease. We cannot make assumptions about their nature, mainly due to short time of observation and uneven coverage of O − C diagram. We also determined the absolute parameter of their components using the photometric solution and GAIA distances.
{"title":"PHOTOMETRIC ANALYSIS OF ECLIPSING BINARIES: VY UMI, RU UMI AND GSC 04364-00648","authors":"V. Kudak, vS.Parimucha, V. Perig, Pavol Gajdoš","doi":"10.22201/ia.01851101p.2023.59.01.10","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.01.10","url":null,"abstract":"We present the photometric analysis of BVR and TESS light curves of three eclipsing binaries, together with their period changes considering archival data and new minima times from our and TESS observations. For the first time we detected wave-like variations with low-amplitude in O − C residua of RU UMi, which can be interpreted as a consequence of the light-time effect caused by the 3rd component with period 7370 days. The period increase detected in the VY UMi system corresponds to mass transfer from the secondary to the primary component. For the GSC 04364-00648 binary system we find quadratic changes on the O − C diagram, which correspond to a period decrease. We cannot make assumptions about their nature, mainly due to short time of observation and uneven coverage of O − C diagram. We also determined the absolute parameter of their components using the photometric solution and GAIA distances.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"1 1","pages":""},"PeriodicalIF":1.0,"publicationDate":"2023-01-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"42861354","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}
Pub Date : 2022-11-09DOI: 10.22201/ia.01851101p.2023.59.01.08
L. Binette, Y. Krongold, S. Haro-Corzo, A. Humphrey, S. G. Morais
The temperature predicted by photoionization models for the narrow line region of Seyfert 2 galaxies is lower than the value inferred from the observed [OIII] λ4363Å/λ5007Å line ratio. We explore the possibility of considering a harder ionizing continuum than typically assumed. The spectral ionizing energy distribution, which can generate the observed λ4363Å/λ5007Å ratio, is characterized by a secondary continuum peak at 200 eV.
{"title":"OPTIMIZED SPECTRAL ENERGY DISTRIBUTION FOR SEYFERT GALAXIES","authors":"L. Binette, Y. Krongold, S. Haro-Corzo, A. Humphrey, S. G. Morais","doi":"10.22201/ia.01851101p.2023.59.01.08","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2023.59.01.08","url":null,"abstract":"The temperature predicted by photoionization models for the narrow line region of Seyfert 2 galaxies is lower than the value inferred from the observed [OIII] λ4363Å/λ5007Å line ratio. We explore the possibility of considering a harder ionizing continuum than typically assumed. The spectral ionizing energy distribution, which can generate the observed λ4363Å/λ5007Å ratio, is characterized by a secondary continuum peak at 200 eV.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-11-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"44732159","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}
Pub Date : 2022-10-01DOI: 10.22201/ia.01851101p.2022.58.02.01
B. Oostra, P. C. Vargas Muñoz
We present measurements of line core positions in UVES spectra of a sample of K-type stars, using the technique of bisector tracing. In all but two of these stars we detect an excess redshift of Ti I lines with respect to Fe I lines. We explain this invoking the temperature-dependence of the line depths. We conclude that the granulation curve is not unique but depends on the chemical species.
{"title":"THE DIFFERENTIAL REDSHIFT OF TITANIUM LINES IN K STARS","authors":"B. Oostra, P. C. Vargas Muñoz","doi":"10.22201/ia.01851101p.2022.58.02.01","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.01","url":null,"abstract":"We present measurements of line core positions in UVES spectra of a sample of K-type stars, using the technique of bisector tracing. In all but two of these stars we detect an excess redshift of Ti I lines with respect to Fe I lines. We explain this invoking the temperature-dependence of the line depths. We conclude that the granulation curve is not unique but depends on the chemical species.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":"46 5","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41293785","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}
Pub Date : 2022-10-01DOI: 10.22201/ia.01851101p.2022.58.02.18
A. Raga, J. Cantó, A. Noriega-Crespo
We present a model for the HII region and stellar wind bow shock formed by runaway O stars passing through the Galactic disk. We develop a quasi-analytic approach in which the absorption of stellar ionizing photons by the bow shock is considered. With these models we study the transition between a detached ionization front (leading the bow shock) and an ionization front trapped by the stellar wind bow shock. We find that for an O7 star one needs to have a stellar velocity of only a few km/s and an environmental density > 105 cm−3.
{"title":"THE HII REGIONS AND BOW SHOCKS AROUND RUNAWAY O STARS","authors":"A. Raga, J. Cantó, A. Noriega-Crespo","doi":"10.22201/ia.01851101p.2022.58.02.18","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.18","url":null,"abstract":"We present a model for the HII region and stellar wind bow shock formed by runaway O stars passing through the Galactic disk. We develop a quasi-analytic approach in which the absorption of stellar ionizing photons by the bow shock is considered. With these models we study the transition between a detached ionization front (leading the bow shock) and an ionization front trapped by the stellar wind bow shock. We find that for an O7 star one needs to have a stellar velocity of only a few km/s and an environmental density > 105 cm−3.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"41376592","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}
Pub Date : 2022-10-01DOI: 10.22201/ia.01851101p.2022.58.02.05
Robert H. Nelson
Radial velocity (RV) and light curve (LC) data for the overcontact binary V563 Lyr have been obtained and analysed with the 2003 version of the WilsonDevinney (WD) code with results K1 = 147.4 ± 2.1 km/s, K2 = 247.2 ± 1.1 km/s, RVγ = 22.5 ± 1.5 km/s, qsp = 0.596 ± 0.008, M1 = 2.49(4)M☉, M2 = 1.45(4)M☉, R1 = 2.23(2)R☉, R2 = 1.81(2)R☉. A third component was identified, with radial velocity RV3 = 18.8 ± 6.7 km/s. Inserting the derived parameters of the eclipsing pair into a Log (L)-Log (Teff) plot for each star using data from Yakut and Eggleton (2005) suggested that both stars are over-luminous and evolved to, and perhaps past, the terminal age main sequence (TAMS). The companion (star 3) has a spectral type of A0 ± 1 spectral subclass but cannot be gravitationally bound to the eclipsing pair, as its flux would dominate that of the pair, which was not observed. The companion must lie at some other distance.
{"title":"THE OVERCONTACT BINARY V563 LYRAE","authors":"Robert H. Nelson","doi":"10.22201/ia.01851101p.2022.58.02.05","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.05","url":null,"abstract":"Radial velocity (RV) and light curve (LC) data for the overcontact binary V563 Lyr have been obtained and analysed with the 2003 version of the WilsonDevinney (WD) code with results K1 = 147.4 ± 2.1 km/s, K2 = 247.2 ± 1.1 km/s, RVγ = 22.5 ± 1.5 km/s, qsp = 0.596 ± 0.008, M1 = 2.49(4)M☉, M2 = 1.45(4)M☉, R1 = 2.23(2)R☉, R2 = 1.81(2)R☉. A third component was identified, with radial velocity RV3 = 18.8 ± 6.7 km/s. Inserting the derived parameters of the eclipsing pair into a Log (L)-Log (Teff) plot for each star using data from Yakut and Eggleton (2005) suggested that both stars are over-luminous and evolved to, and perhaps past, the terminal age main sequence (TAMS). The companion (star 3) has a spectral type of A0 ± 1 spectral subclass but cannot be gravitationally bound to the eclipsing pair, as its flux would dominate that of the pair, which was not observed. The companion must lie at some other distance.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46731197","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}
Pub Date : 2022-10-01DOI: 10.22201/ia.01851101p.2022.58.02.06
C. Barani, M. Martignoni, F. Acerbi, R. Michel, H. Aceves, V. Popov
The first analysis of the light curves of contact binaries ROTSE J135349.8+305205 (CB1) and 1SWASP J150957.5-115308 (CB2) using the Wilson-Devinney code is presented. Both binary systems are of the A-subtype with a shallow fill-out (20.8% and 15.8% respectively) and a difference in temperatures between the components of < 200 K. A mass-ratio of 0.302 is found for CB1, while for CB2 the interesting value of 0.904 is found. The short periods, 0.246 d for CB1 and 0.229 d for CB2, and their spectral type K suggests that these systems are near the shortest period limit. The absolute elements are estimated using GAIA parallaxes. CB2 is found to be at the beginning of its evolution, while CB1 will approach the final evolutionary stage. The sum of the component masses of CB1 is 0.813 M☉, below the mass limit of 1.0 − 1.2 M☉ assumed for the known contact binary stars.
{"title":"PHOTOMETRIC ANALYSIS OF TWO K SPECTRAL TYPE CONTACT BINARY SYSTEMS","authors":"C. Barani, M. Martignoni, F. Acerbi, R. Michel, H. Aceves, V. Popov","doi":"10.22201/ia.01851101p.2022.58.02.06","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.06","url":null,"abstract":"The first analysis of the light curves of contact binaries ROTSE J135349.8+305205 (CB1) and 1SWASP J150957.5-115308 (CB2) using the Wilson-Devinney code is presented. Both binary systems are of the A-subtype with a shallow fill-out (20.8% and 15.8% respectively) and a difference in temperatures between the components of < 200 K. A mass-ratio of 0.302 is found for CB1, while for CB2 the interesting value of 0.904 is found. The short periods, 0.246 d for CB1 and 0.229 d for CB2, and their spectral type K suggests that these systems are near the shortest period limit. The absolute elements are estimated using GAIA parallaxes. CB2 is found to be at the beginning of its evolution, while CB1 will approach the final evolutionary stage. The sum of the component masses of CB1 is 0.813 M☉, below the mass limit of 1.0 − 1.2 M☉ assumed for the known contact binary stars.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46117694","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}
Pub Date : 2022-10-01DOI: 10.22201/ia.01851101p.2022.58.02.11
R. L. Branham, Jr.
Comet C/1830 F1 (Great March comet) is one of a large number of comets with parabolic orbits. Given that there are sufficient observations of the comet, (428 in right ascension and 424 in declination), it proves possible to calculate a better orbit. The calculations are based on a 12th order predictor-corrector method. The comet’s orbit is highly elliptical, e=0.99792 and, from calculated mean errors, statistically different from a parabola. The comet will not return for thousands of years and thus represents no immediate NEO threat.
C/1830 F1彗星(Great March Comet)是众多抛物线轨道彗星之一。考虑到对这颗彗星有足够的观测(赤经428次，赤纬424次)，计算出一个更好的轨道是可能的。计算基于12阶预测校正方法。这颗彗星的轨道是高度椭圆的，e=0.99792，从计算的平均误差来看，在统计上与抛物线不同。这颗彗星将在数千年内不会返回，因此不会对近地天体构成直接威胁。
{"title":"A NEW ORBIT FOR COMET C/1830 F1 (GREAT MARCH COMET)","authors":"R. L. Branham, Jr.","doi":"10.22201/ia.01851101p.2022.58.02.11","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.11","url":null,"abstract":"Comet C/1830 F1 (Great March comet) is one of a large number of comets with parabolic orbits. Given that there are sufficient observations of the comet, (428 in right ascension and 424 in declination), it proves possible to calculate a better orbit. The calculations are based on a 12th order predictor-corrector method. The comet’s orbit is highly elliptical, e=0.99792 and, from calculated mean errors, statistically different from a parabola. The comet will not return for thousands of years and thus represents no immediate NEO threat.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"48571722","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}
Pub Date : 2022-10-01DOI: 10.22201/ia.01851101p.2022.58.02.04
A. Raga, J. Cantó, A. Castellanos-Ramírez, A. Rodríguez-González, P. Rivera-Ortiz
We present a model for the “Bondi-Hoyle tail” left behind by the hypersonic passage of a compact, massive object through a dense, radiative environment. We derive simple equations for the flow velocity and the mass along the tail, and obtain numerical and approximate analytical solutions for the steady state problem. We then study a time-dependent problem in which the source first travels within a dense cloud, and then emerges into a low density environment. This flow results in the production of a trail of dense gas joining the source at the point in which it emerged from the dense cloud. This trail has a linear velocity vs. position profile.
{"title":"THE BONDI-HOYLE ACCRETION TAIL OF POINT SOURCES TRAVELLING HYPERSONICALLY THROUGH A DENSE ENVIRONMENT","authors":"A. Raga, J. Cantó, A. Castellanos-Ramírez, A. Rodríguez-González, P. Rivera-Ortiz","doi":"10.22201/ia.01851101p.2022.58.02.04","DOIUrl":"https://doi.org/10.22201/ia.01851101p.2022.58.02.04","url":null,"abstract":"We present a model for the “Bondi-Hoyle tail” left behind by the hypersonic passage of a compact, massive object through a dense, radiative environment. We derive simple equations for the flow velocity and the mass along the tail, and obtain numerical and approximate analytical solutions for the steady state problem. We then study a time-dependent problem in which the source first travels within a dense cloud, and then emerges into a low density environment. This flow results in the production of a trail of dense gas joining the source at the point in which it emerged from the dense cloud. This trail has a linear velocity vs. position profile.","PeriodicalId":49602,"journal":{"name":"Revista Mexicana de Astronomia y Astrofisica","volume":" ","pages":""},"PeriodicalIF":1.0,"publicationDate":"2022-10-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"46833922","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}
京公网安备 11010802042870号
京ICP备2023020795号-1
扫码关注我们
求助内容：
应助结果提醒方式：