针对用于太阳磁场精确测量的中红外观测系统(Accurate Infrared Magnetic field Measurements of the Sun,AIMS)望远镜8~10μm真空制冷成像终端系统的高精度装调需求,提出了一种基于中红外可调谐激光光源的宽谱段干涉检测和装调方法。首...针对用于太阳磁场精确测量的中红外观测系统(Accurate Infrared Magnetic field Measurements of the Sun,AIMS)望远镜8~10μm真空制冷成像终端系统的高精度装调需求,提出了一种基于中红外可调谐激光光源的宽谱段干涉检测和装调方法。首先,采用泰曼-格林干涉仪,利用参考臂可调的优势,弥补光源相干性不足的缺陷,从而实现8~10μm宽谱段的干涉测量。其次,完成了干涉仪光学系统设计,可同时兼顾8~10μm和可见光双波段的波前质量,解决了肉眼不可见给干涉仪自身装调带来的困难。设计结果表明,利用可见光激光器进行干涉仪自身装调,可达到RMS 0.05λ@0.633μm的波前精度;在8~10μm检测波段,干涉仪波前均方根优于0.001λ,可满足待测系统的检测需求。最后,基于逆向优化法仿真了8~10μm光学系统的装调流程。展开更多
Hydroxysafflor yellow A(HSYA)extracted from the herb Cathartics tinctorius L.negatively regulates liver cancer growth.However,the exact mechanism of HSYA action in liver cancer remains largely unknown.In this study,HS...Hydroxysafflor yellow A(HSYA)extracted from the herb Cathartics tinctorius L.negatively regulates liver cancer growth.However,the exact mechanism of HSYA action in liver cancer remains largely unknown.In this study,HSY A inhibited liver cancer cell growth in vivo and in vitro,evidenced by cell proliferation inhibition detected by CCK8,numerous apoptotic cells shown by flow cytometry assay,and expression of apoptosis-related proteins determined by Western blot.展开更多
Kink oscillations,which are frequently observed in coronal loops and prominences,are often accompanied by extreme-ultraviolet(EUV)waves.However,much more needs to be explored regarding the causal relationships between...Kink oscillations,which are frequently observed in coronal loops and prominences,are often accompanied by extreme-ultraviolet(EUV)waves.However,much more needs to be explored regarding the causal relationships between kink oscillations and EUV waves.In this article,we report the simultaneous detection of kink oscillations and EUV waves that are both associated with an X2.1 flare on 2023 March 03(SOL2023-03-03T17:39).The kink oscillations,which are almost perpendicular to the axes of loop-like structures,are observed in three coronal loops and one prominence.One short loop shows in-phase oscillation within the same period of 5.2 min at three positions.This oscillation could be triggered by the pushing of an expanding loop and interpreted as the standing kink wave.Time lags are found between the kink oscillations of the short loop and two long loops,suggesting that the kink wave travels in different loops.The kink oscillations of one long loop and the prominence are possibly driven by the disturbance of the coronal mass ejection(CME),and that of another long loop might be attributed to the interaction of the EUV wave.The onset time of the kink oscillation of the short loop is nearly same as the beginning of an EUV wave.This fact demonstrates that they are almost simultaneous.The EUV wave is most likely excited by the expanding loop structure and shows two components.The leading component is a fast coronal wave,and the trailing one could be due to the stretching magnetic field lines.展开更多
The Space Advanced Technology demonstration satellite(SATech-01),a mission for low-cost space science and new technology experiments,organized by Chinese Academy of Sciences(CAS),was successfully launched into a Sun-s...The Space Advanced Technology demonstration satellite(SATech-01),a mission for low-cost space science and new technology experiments,organized by Chinese Academy of Sciences(CAS),was successfully launched into a Sun-synchronous orbit at an altitude of~500 km on July 27,2022,from the Jiuquan Satellite Launch Centre.Serving as an experimental platform for space science exploration and the demonstration of advanced common technologies in orbit,SATech-01 is equipped with 16 experimental payloads,including the solar upper transition region imager(SUTRI),the lobster eye imager for astronomy(LEIA),the high energy burst searcher(HEBS),and a High Precision Magnetic Field Measurement System based on a CPT Magnetometer(CPT).It also incorporates an imager with freeform optics,an integrated thermal imaging sensor,and a multi-functional integrated imager,etc.This paper provides an overview of SATech-01,including a technical description of the satellite and its scientific payloads,along with their on-orbit performance.展开更多
Magnetoseismology,a technique of magnetic field diagnostics based on observations of magnetohydrodynamic(MHD)waves,has been widely used to estimate the field strengths of oscillating structures in the solar corona.How...Magnetoseismology,a technique of magnetic field diagnostics based on observations of magnetohydrodynamic(MHD)waves,has been widely used to estimate the field strengths of oscillating structures in the solar corona.However,previously magnetoseismology was mostly applied to occasionally occurring oscillation events,providing an estimate of only the average field strength or one-dimensional distribution of field strength along an oscillating structure.This restriction could be eliminated if we apply magnetoseismology to the pervasive propagating transverse MHD waves discovered with the Coronal Multi-channel Polarimeter(CoMP).Using several CoMP observations of the Fe xiii 1074.7 nm and 1079.8 nm spectral lines,we obtained maps of the plasma density and wave phase speed in the corona,which allow us to map both the strength and direction of the coronal magnetic field in the plane of sky.We also examined distributions of the electron density and magnetic field strength,and compared their variations with height in the quiet Sun and active regions.Such measurements could provide critical information to advance our understanding of the Sun's magnetism and the magnetic coupling of the whole solar atmosphere.展开更多
文摘针对用于太阳磁场精确测量的中红外观测系统(Accurate Infrared Magnetic field Measurements of the Sun,AIMS)望远镜8~10μm真空制冷成像终端系统的高精度装调需求,提出了一种基于中红外可调谐激光光源的宽谱段干涉检测和装调方法。首先,采用泰曼-格林干涉仪,利用参考臂可调的优势,弥补光源相干性不足的缺陷,从而实现8~10μm宽谱段的干涉测量。其次,完成了干涉仪光学系统设计,可同时兼顾8~10μm和可见光双波段的波前质量,解决了肉眼不可见给干涉仪自身装调带来的困难。设计结果表明,利用可见光激光器进行干涉仪自身装调,可达到RMS 0.05λ@0.633μm的波前精度;在8~10μm检测波段,干涉仪波前均方根优于0.001λ,可满足待测系统的检测需求。最后,基于逆向优化法仿真了8~10μm光学系统的装调流程。
文摘Hydroxysafflor yellow A(HSYA)extracted from the herb Cathartics tinctorius L.negatively regulates liver cancer growth.However,the exact mechanism of HSYA action in liver cancer remains largely unknown.In this study,HSY A inhibited liver cancer cell growth in vivo and in vitro,evidenced by cell proliferation inhibition detected by CCK8,numerous apoptotic cells shown by flow cytometry assay,and expression of apoptosis-related proteins determined by Western blot.
基金supported by the National Key R&D Program of China 2021YFA1600502(Grant No.2021YFA1600500)the National Natural Science Foundation of China(Grant Nos.11973092,12073081,12003064+4 种基金12333009)supported by the Surface Project of Jiangsu Province(Grant No.BK20211402)Yunnan Key Laboratory of Solar Physics and Space Science(202205AG070009)(Grant No.YNSPCC202207)a collaborative project conducted by the National Astronomical Observatories of CAS,Peking University,Tongji University,Xi’an Institute of Optics and Precision Mechanics of CAS and the Innovation Academy for Microsatellites of CASsupported by the China National Space Administration(CNSA)。
文摘Kink oscillations,which are frequently observed in coronal loops and prominences,are often accompanied by extreme-ultraviolet(EUV)waves.However,much more needs to be explored regarding the causal relationships between kink oscillations and EUV waves.In this article,we report the simultaneous detection of kink oscillations and EUV waves that are both associated with an X2.1 flare on 2023 March 03(SOL2023-03-03T17:39).The kink oscillations,which are almost perpendicular to the axes of loop-like structures,are observed in three coronal loops and one prominence.One short loop shows in-phase oscillation within the same period of 5.2 min at three positions.This oscillation could be triggered by the pushing of an expanding loop and interpreted as the standing kink wave.Time lags are found between the kink oscillations of the short loop and two long loops,suggesting that the kink wave travels in different loops.The kink oscillations of one long loop and the prominence are possibly driven by the disturbance of the coronal mass ejection(CME),and that of another long loop might be attributed to the interaction of the EUV wave.The onset time of the kink oscillation of the short loop is nearly same as the beginning of an EUV wave.This fact demonstrates that they are almost simultaneous.The EUV wave is most likely excited by the expanding loop structure and shows two components.The leading component is a fast coronal wave,and the trailing one could be due to the stretching magnetic field lines.
基金supported by the Strategic Priority Program on Space Science,the Chinese Academy of Sciences。
文摘The Space Advanced Technology demonstration satellite(SATech-01),a mission for low-cost space science and new technology experiments,organized by Chinese Academy of Sciences(CAS),was successfully launched into a Sun-synchronous orbit at an altitude of~500 km on July 27,2022,from the Jiuquan Satellite Launch Centre.Serving as an experimental platform for space science exploration and the demonstration of advanced common technologies in orbit,SATech-01 is equipped with 16 experimental payloads,including the solar upper transition region imager(SUTRI),the lobster eye imager for astronomy(LEIA),the high energy burst searcher(HEBS),and a High Precision Magnetic Field Measurement System based on a CPT Magnetometer(CPT).It also incorporates an imager with freeform optics,an integrated thermal imaging sensor,and a multi-functional integrated imager,etc.This paper provides an overview of SATech-01,including a technical description of the satellite and its scientific payloads,along with their on-orbit performance.
基金This work was supported by the National Natural Science Foundation of China(Grant Nos.11825301,11790304(11790300))the Strategic Prior-ity Research Program of CAS(Grant No.XDA17040507)+1 种基金and Grant No.1916321TS00103201This material is based upon work supported by the National Center for Atmospheric Research,which is a major facility spon-sored by the National Science Foundation under Cooperative Agreement(Grant No.1852977)。
文摘Magnetoseismology,a technique of magnetic field diagnostics based on observations of magnetohydrodynamic(MHD)waves,has been widely used to estimate the field strengths of oscillating structures in the solar corona.However,previously magnetoseismology was mostly applied to occasionally occurring oscillation events,providing an estimate of only the average field strength or one-dimensional distribution of field strength along an oscillating structure.This restriction could be eliminated if we apply magnetoseismology to the pervasive propagating transverse MHD waves discovered with the Coronal Multi-channel Polarimeter(CoMP).Using several CoMP observations of the Fe xiii 1074.7 nm and 1079.8 nm spectral lines,we obtained maps of the plasma density and wave phase speed in the corona,which allow us to map both the strength and direction of the coronal magnetic field in the plane of sky.We also examined distributions of the electron density and magnetic field strength,and compared their variations with height in the quiet Sun and active regions.Such measurements could provide critical information to advance our understanding of the Sun's magnetism and the magnetic coupling of the whole solar atmosphere.
