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Interactions of multiple stressors on the Bombay-duck Harpadon nehereus population in a complex estuarine ecosystem 期刊论文  OAI收割
SCIENCE OF THE TOTAL ENVIRONMENT, 2024, 卷号: 953, 页码: 14
作者:  
Zhang, Zhaopeng;  Liang, Cui;  Zheng, Lei;  Cao, Wenzhuo;  Wang, Yuanchao
  |  收藏  |  浏览/下载:8/0  |  提交时间:2024/12/20
On Intelligent Mining With Parallel Intelligence 期刊论文  OAI收割
IEEE TRANSACTIONS ON INTELLIGENT VEHICLES, 2023, 卷号: 8, 期号: 10, 页码: 4296-4300
作者:  
Yang, Jianjian;  Huang, Qiankun;  Ge, Shirong;  Wang, Xiao;  Chen, Long
  |  收藏  |  浏览/下载:19/0  |  提交时间:2024/02/22
Urban land surface temperature prediction using parallel STL-Bi-LSTM neural network 期刊论文  OAI收割
JOURNAL OF APPLIED REMOTE SENSING, 2022, 卷号: 16, 期号: 3, 页码: 13
作者:  
Huo, Xing;  Cui, Guangpeng;  Ma, Lingling;  Tang, Bohui;  Tang, Ronglin
  |  收藏  |  浏览/下载:24/0  |  提交时间:2022/11/29
Periodicity Search on X-Ray Bursts of SGR J1935+2154 Using 8.5 yr of Fermi/GBM Data 期刊论文  OAI收割
The Astrophysical Journal, 2021, 卷号: 923, 页码: L30
作者:  
HXMT
  |  收藏  |  浏览/下载:22/0  |  提交时间:2022/02/08
Constraining the X-Ray-Infrared Spectral Index of Second-timescale Flares from SGR 1935+2154 with Palomar Gattini-IR 期刊论文  OAI收割
The Astrophysical Journal, 2020, 卷号: 901, 页码: L7
作者:  
HXMT
  |  收藏  |  浏览/下载:24/0  |  提交时间:2022/02/08
Radio transient sources  Magnetars  Soft gamma-ray repeaters  2008  992  1471  Astrophysics - High Energy Astrophysical Phenomena  Astrophysics - Instrumentation and Methods for Astrophysics  Abstract: The Galactic magnetar SGR 1935+2154 has been reported to produce the first example of a bright millisecond-duration radio burst (FRB 200428) similar to the cosmological population of fast radio bursts (FRBs). The detection of a coincident bright X-ray burst represents the first observed multiwavelength counterpart of an FRB. However, the search for similar emission at optical wavelengths has been hampered by the high inferred extinction on the line of sight. Here, we present results from the first search for second-timescale emission from the source at near-infrared (NIR) wavelengths using the Palomar Gattini-IR observing system in the J band, enabled by a novel detector readout mode that allows short exposure times of ?0.84 s with 99.9% observing efficiency. With a total observing time of ?12 hr (?47,728 images) during its 2020 outburst, we place median 3Ҡlimits on the second-timescale NIR fluence of ?18 Jy ms (13.1 AB mag). The corresponding extinction-corrected limit is ?125 Jy ms for an estimated extinction of AJ = 2.0 mag. Our observations were sensitive enough to easily detect an NIR counterpart of FRB 200428 if the NIR emission falls on the same power law as observed across its radio to X-ray spectrum. We report nondetection limits from epochs of four simultaneous X-ray bursts detected by the Insight-HXMT and NuSTAR telescopes during our observations. These limits provide the most stringent constraints to date on fluence of flares at 1014 Hz, and constrain the fluence ratio of the NIR emission to coincident X-ray bursts to RNIR ? 0.025 (fluence index ?0.35).  
In-orbit Demonstration of X-Ray Pulsar Navigation with the Insight-HXMT Satellite 期刊论文  OAI收割
The Astrophysical Journal Supplement Series, 2019, 卷号: 244, 页码: 1
作者:  
HXMT
  |  收藏  |  浏览/下载:15/0  |  提交时间:2022/02/08
pulsars: general  techniques: miscellaneous  Astrophysics -  Instrumentation and Methods for Astrophysics  Abstract: In this work, we report the in-orbit demonstration of X-ray pulsar navigation with Insight-Hard X-ray Modulation Telescope (Insight-HXMT) Satellite, which was launched on 2017 June 15. The new pulsar navigation method Significance Enhancement of Pulse-profile with Orbit-dynamics is adopted to determine the orbit with observations of only one pulsar. In this test, the Crab pulsar is chosen and observed by Insight-HXMT from 2017 August 31 to September 5. Using the five-day long observation data, the orbit of Insight-HXMT is determined successfully with the three telescopes onboard: High Energy X-ray Telescope, Medium Energy X-ray Telescope, and Low Energy X-ray Telescope, respectively. By combining all the data, the position and velocity of the Insight-HXMT are pinpointed to within 10 km (3ҩ and 10 m s-1 (3ҩ, respectively.  
Application of nanofilms for arsenic speciation using surface-enhanced Raman spectroscopy(SERS) 会议论文  OAI收割
2018-06-24
作者:  
V.Liamtsau;  Yong Cai
  |  收藏  |  浏览/下载:18/0  |  提交时间:2019/08/21
High-resolution topography measurement of PACMANUS and DESMOS hydrothermal fields using a ROV in Manus basin CNKI期刊论文  OAI收割
2016
作者:  
Xiaochuan Ma;  Jun Yan;  Zhendong Luan;  Xin Zhang;  Cui-E Zheng
  |  收藏  |  浏览/下载:1/0  |  提交时间:2024/12/18
城市污水处理与工业应用过程中有机磷酸酯阻燃剂的 迁移转化研究 学位论文  OAI收割
博士, 北京: 中国科学院研究生院, 2016
作者:  
梁钪
收藏  |  浏览/下载:230/0  |  提交时间:2017/07/12
Correlations between neutrons and protons near the Fermi surface and Q(alpha) of superheavy nuclei 期刊论文  OAI收割
PHYSICAL REVIEW C, 2016, 卷号: 93, 期号: 1, 页码: 14302
作者:  
Wang, N;  Liu, M;  Wu, XZ;  Meng, J;  Wang, N (reprint author), Guangxi Normal Univ, Dept Phys, Guilin 541004, Peoples R China.
  |  收藏  |  浏览/下载:42/0  |  提交时间:2017/10/13
The Shell Corrections And Shell Gaps In Nuclei Are Systematically Studied With The Latest Weizsacker-skyrme  (Ws4) Mass Model. We Find That Most Of Asymmetric Nuclei With (Sub) Shell Closures Locate Along The Shell Stability  Line (Ssl)  n=1.37z+13.5  Which Might Be Due To a Strong Correlation Between Neutrons And proTons Near  The Fermi Surface. The Double Magicity Of Nuclei Si-46 And Ni-78 Is Predicted According To The Corresponding  Shell Gaps  Shell Corrections  And Nuclear Deformations. The Unmeasured Superheavy Nuclei  (296)118 And (298)120  With Relatively Large Shell Gaps And Shell Corrections  Also Locate Along The Ssl  Whereas The Traditional Magic  Nucleus (298)F1 Evidently Deviates From The Line. The Alpha-decay Energies Of Superheavy Nuclei With Z=113-126  Are Simultaneously Investigated By Using The Ws4 Model togeTher With The Radial Basis Function Corrections. For  Superheavy Nuclei With Large Shell Corrections  The Smallest Alpha-decay Energy For Elements Z=116  117  And 118  In Their Isotope chaIns LocAtes At N=178 rAther Than 184.