Fast radio bursts(FRBs) are highly dispersed millisecond-duration radio bursts,[1,2]of which the physical origin is still not fully understood. FRB 20201124A is one of the most actively repeating FRBs. In this paper, ...Fast radio bursts(FRBs) are highly dispersed millisecond-duration radio bursts,[1,2]of which the physical origin is still not fully understood. FRB 20201124A is one of the most actively repeating FRBs. In this paper, we present the collection of 1863 burst dynamic spectra of FRB 20201124A measured with the Five-hundred-meter Aperture Spherical radio Telescope(FAST). The current collection, taken from the observation during the FRB active phase from April to June 2021, is the largest burst sample detected for any FRB so far. The standard PSRFITs format is adopted, including dynamic spectra of the burst, and the time information of the dynamic spectra, in addition, mask files help readers to identify the pulse positions are also provided. The dataset is available in Science Data Bank, with the link https://www.doi.org/10.57760/sciencedb.j00113.00076.展开更多
快速射电暴是近年来发展最快的天文学科之一。理论上,快速射电暴可能存在毫秒到小时时标的光学对应体.快速射电暴光学对应体有可能在中国未来大视场望远镜中探测到,例如:中国空间站工程巡天望远镜(China Space Station Telescope,CSST)...快速射电暴是近年来发展最快的天文学科之一。理论上,快速射电暴可能存在毫秒到小时时标的光学对应体.快速射电暴光学对应体有可能在中国未来大视场望远镜中探测到,例如:中国空间站工程巡天望远镜(China Space Station Telescope,CSST)、中国科学技术大学和紫金山天文台合作的2.5m大视场巡天望远镜(WideField Survey Telescope,WFST)和地球2.0(Earth 2.0,ET)等。快速射电暴光学对应体通常分为毫秒时标光学对应体、小时时标光学对应体和光学余辉。前两者可产生于快速射电暴的高能外延或是快速射电暴的射电辐射与高能电子的逆康普顿散射,探测率与光学-射电流量比η_(v)关系密切.对于毫秒时标光学对应体,最理想情况下WFST、CSST和ET的探测率可以达到每年上百个.当η_(v)~10^(-3)时,WFST、CSST的年探测率仅为1个的量级,ET的年探测率为19.5个.对于小时时标光学对应体,最理想情况下超新星遗迹的年龄为5年且η_(v)约为10^(-6)时,年探测率可到100以上.FRB200428的X射线对应体表明,快速射电暴可能产生相对论性外流并且与星际介质相互作用产生光学余辉.结合快速射电暴的能量、在宇宙中的分布以及标准余辉模型,可以对快速射电暴余辉的可探测性进行研究.当总能量-射电能量比与FRB200428类似(ζ=10^(5))时,CSST、WFST和ET的年探测率分别为1.3、1.0和67个。展开更多
Viscous scale effects on propeller TVC were investigated by testing a series of three geosim propeller models in the large cavitation Tunnel of CSSRC without and with two different turbulence stimulators. Tests includ...Viscous scale effects on propeller TVC were investigated by testing a series of three geosim propeller models in the large cavitation Tunnel of CSSRC without and with two different turbulence stimulators. Tests included flow visualization by oil film method and cavitation observation for five different stages of development of propeller TVC: desinent, unattached, attached, developed and fully developed TVC. The main findings are: 1)there existed a size effect of the boundary-layer transition on propeller models which could be analyzed by using the critical roughness Reynolds number and a newly defined quasi-critical Reynolds number, 2)the preliminary results of the blackboardpaint used as a tripping device was encouraging, 3)the Reynolds number exponent n of TVC scaling rules was found to be dependent upon the blade surface condition, the stage of development of TVC and the thrust loading of propeller models.展开更多
利用基于密度泛函理论(DFT)的Dmol^(3)程序广义梯度近似PBE泛函,研究了Co^(q)_(n)(n=1~5;q=0,+,-)团簇和原子氧吸附在团簇上的几何结构、稳定性、电子性质和吸附反应行为。结果表明:Co^(q)_(n)团簇的几何结构保持不变,阳离子型团簇(Co^(...利用基于密度泛函理论(DFT)的Dmol^(3)程序广义梯度近似PBE泛函,研究了Co^(q)_(n)(n=1~5;q=0,+,-)团簇和原子氧吸附在团簇上的几何结构、稳定性、电子性质和吸附反应行为。结果表明:Co^(q)_(n)团簇的几何结构保持不变,阳离子型团簇(Co^(+)_(n))的平均结合能远大于中性型(Co^(0)_(n))和阴离子型(Co^(-)_(n))团簇的平均结合能,这是因为团簇失去一个电子后可以显著增强该团簇的稳定性;原子氧在Co^(q)_(n)团簇顶位、桥位、空位的吸附稳定性、Co—O键长、原子氧的电荷转移都呈现出规律性变化,说明原子氧被活化;Co^(-)_(4) O B团簇的吸附能为-8.375 eV,轨道分析进一步表明其原子氧的2p轨道和钴的3d轨道杂化,相互作用为化学吸附。展开更多
基金supported by the National SKA Program of China (Grant Nos. 2020SKA0120100 and 2020SKA0120200)the National Natural Science Foundation of China (Grant Nos. 12041304, 11873067, 11988101, 12041303, 11725313, 11725314, 11833003, 12003028, 12041306, 12103089, U2031209, U2038105, and U1831207)+8 种基金the National Key Research and Development Program of China (Grant Nos. 2019YFA0405100, 2017YFA0402602, 2018YFA0404204, and 2016YFA0400801)Key Research Program of the Chinese Academy of Sciences (Grant No. QYZDJ-SSW-SLH021)Natural Science Foundation of Jiangsu Province (Grant No. BK20211000)Cultivation Project for FAST Scientific Payoff and Research Achievement of CAMS-CAS, the Strategic Priority Research Program on Space Science, the Western Light Youth Project of Chinese Academy of Sciences (Grant Nos. XDA15360000, XDA15052700, and XDB23040400)funding from the MaxPlanck Partner Group, the science research grants from the China Manned Space Project (Grant Nos. CMS-CSST2021-B11 and CMS-CSST-2021-A11)PKU development (Grant No. 7101502590)support from the XPLORER PRIZEsupported by Fundamental Research Funds for the Central Universities (Grant No. 14380046)the Program for Innovative Talents, Entrepreneur in Jiangsu。
文摘Fast radio bursts(FRBs) are highly dispersed millisecond-duration radio bursts,[1,2]of which the physical origin is still not fully understood. FRB 20201124A is one of the most actively repeating FRBs. In this paper, we present the collection of 1863 burst dynamic spectra of FRB 20201124A measured with the Five-hundred-meter Aperture Spherical radio Telescope(FAST). The current collection, taken from the observation during the FRB active phase from April to June 2021, is the largest burst sample detected for any FRB so far. The standard PSRFITs format is adopted, including dynamic spectra of the burst, and the time information of the dynamic spectra, in addition, mask files help readers to identify the pulse positions are also provided. The dataset is available in Science Data Bank, with the link https://www.doi.org/10.57760/sciencedb.j00113.00076.
文摘快速射电暴是近年来发展最快的天文学科之一。理论上,快速射电暴可能存在毫秒到小时时标的光学对应体.快速射电暴光学对应体有可能在中国未来大视场望远镜中探测到,例如:中国空间站工程巡天望远镜(China Space Station Telescope,CSST)、中国科学技术大学和紫金山天文台合作的2.5m大视场巡天望远镜(WideField Survey Telescope,WFST)和地球2.0(Earth 2.0,ET)等。快速射电暴光学对应体通常分为毫秒时标光学对应体、小时时标光学对应体和光学余辉。前两者可产生于快速射电暴的高能外延或是快速射电暴的射电辐射与高能电子的逆康普顿散射,探测率与光学-射电流量比η_(v)关系密切.对于毫秒时标光学对应体,最理想情况下WFST、CSST和ET的探测率可以达到每年上百个.当η_(v)~10^(-3)时,WFST、CSST的年探测率仅为1个的量级,ET的年探测率为19.5个.对于小时时标光学对应体,最理想情况下超新星遗迹的年龄为5年且η_(v)约为10^(-6)时,年探测率可到100以上.FRB200428的X射线对应体表明,快速射电暴可能产生相对论性外流并且与星际介质相互作用产生光学余辉.结合快速射电暴的能量、在宇宙中的分布以及标准余辉模型,可以对快速射电暴余辉的可探测性进行研究.当总能量-射电能量比与FRB200428类似(ζ=10^(5))时,CSST、WFST和ET的年探测率分别为1.3、1.0和67个。
文摘Viscous scale effects on propeller TVC were investigated by testing a series of three geosim propeller models in the large cavitation Tunnel of CSSRC without and with two different turbulence stimulators. Tests included flow visualization by oil film method and cavitation observation for five different stages of development of propeller TVC: desinent, unattached, attached, developed and fully developed TVC. The main findings are: 1)there existed a size effect of the boundary-layer transition on propeller models which could be analyzed by using the critical roughness Reynolds number and a newly defined quasi-critical Reynolds number, 2)the preliminary results of the blackboardpaint used as a tripping device was encouraging, 3)the Reynolds number exponent n of TVC scaling rules was found to be dependent upon the blade surface condition, the stage of development of TVC and the thrust loading of propeller models.
文摘利用基于密度泛函理论(DFT)的Dmol^(3)程序广义梯度近似PBE泛函,研究了Co^(q)_(n)(n=1~5;q=0,+,-)团簇和原子氧吸附在团簇上的几何结构、稳定性、电子性质和吸附反应行为。结果表明:Co^(q)_(n)团簇的几何结构保持不变,阳离子型团簇(Co^(+)_(n))的平均结合能远大于中性型(Co^(0)_(n))和阴离子型(Co^(-)_(n))团簇的平均结合能,这是因为团簇失去一个电子后可以显著增强该团簇的稳定性;原子氧在Co^(q)_(n)团簇顶位、桥位、空位的吸附稳定性、Co—O键长、原子氧的电荷转移都呈现出规律性变化,说明原子氧被活化;Co^(-)_(4) O B团簇的吸附能为-8.375 eV,轨道分析进一步表明其原子氧的2p轨道和钴的3d轨道杂化,相互作用为化学吸附。
