“慧眼”硬X射线调制望远镜(简称慧眼卫星,英文名为Insight Hard X-ray Modulation Telescope,简称Insight-HXMT或HXMT),于2017年6月15日发射升空,标志着我国自主研发的首个天文台级X射线望远镜的诞生.慧眼卫星凭借其大面积、宽波段、...“慧眼”硬X射线调制望远镜(简称慧眼卫星,英文名为Insight Hard X-ray Modulation Telescope,简称Insight-HXMT或HXMT),于2017年6月15日发射升空,标志着我国自主研发的首个天文台级X射线望远镜的诞生.慧眼卫星凭借其大面积、宽波段、高时间分辨率和高能量分辨率的综合优势,为黑洞与中子星系统的硬X射线快速变化和宽波段能谱研究领域开辟了新的研究窗口.超出设计寿命的慧眼卫星已稳定运行超过8yr,目前状态良好,且有望进一步延长其在轨服务时间.截至2024年10月,慧眼卫星已7次向全球科学界公开征集观测提案,共收到334份有效的观测提案,并据此制定了2368个观测计划.此外,慧眼卫星已向公众发布数据13批次,累计数据量达到40 TB,数据公开比率高达94%.慧眼卫星还向用户提供了不同版本的数据分析软件和标定数据库,在轨标定精度在2%左右,满足科学分析的要求.来自全球17家及国内36家研究机构的学者使用慧眼数据开展了科学研究,发表了约300多篇高质量学术论文,累计引用次数约7300次.展开更多
The Hard X-ray Imager(HXI)payload,a component of China’s Advanced Space-based Solar Observatory satellite,is designed to observe solar X-ray emissions in the 30-200 keV range,with the aim of investigating nonthermal ...The Hard X-ray Imager(HXI)payload,a component of China’s Advanced Space-based Solar Observatory satellite,is designed to observe solar X-ray emissions in the 30-200 keV range,with the aim of investigating nonthermal physical processes during solar flares.Before launch,Geant4 simulations were employed to assess the onorbit background of the HXI instrument,evaluating its performance and potential to achieve its scientific objectives.This study addresses issues identified in previous simulations and conducts further analyses to examine the distribution of background counts across the 99 detectors.The results demonstrate alignment between simulations and observations at low and medium geomagnetic latitudes;however,challenges persist at high geomagnetic latitudes due to limitations in the current albedo photon model.This investigation provides insights into background sources from various particles,enhances understanding of space background characteristics,and offers guidance for background subtraction in imaging processes.展开更多
Early multiwavelength observations offer crucial insights into the nature of the relativistic jets responsible for gamma-ray bursts and their interaction with the surrounding medium.We present data of GRB 240825A from...Early multiwavelength observations offer crucial insights into the nature of the relativistic jets responsible for gamma-ray bursts and their interaction with the surrounding medium.We present data of GRB 240825A from 17 space-and ground-based telescopes/instruments,covering wavelengths from NIR/optical to X-ray and GeV,and spanning from the prompt emission to the afterglow phase triggered by Swift and Fermi.The early afterglow observations were carried out by SVOM/C-GFT,and spectroscopic observations of the afterglow by GTC,VLT,and TNG determined the redshift of the burst(z=0.659)later.A comprehensive analysis of the prompt emission spectrum observed by Swift-BAT and Fermi-GBM/LAT reveals a rare and significant high-energy cutoff at 76 MeV.Assuming this cutoff is due toγγabsorption allows us to place an upper limit on the initial Lorentz factor,Γ_(0)<245.The optical/NIR and GeV afterglow light curves can be described by the standard external shock model,with early-time emission dominated by a reverse shock(RS)and a subsequent transition to forward shock(FS)emission.Our afterglow modeling yields a consistent estimate of the initial Lorentz factor(Γ_(0)∼234).Furthermore,the RS-to-FS magnetic field ratio(R 302B)indicates that the RS region is significantly more magnetized than the FS region.An isotropic-equivalent kinetic energy of E_(k,iso)=5.25×10^(54) erg is derived,and the correspondingγ-ray radiation efficiency is estimated to beη_(γ)=3.1%.On the other hand,the standard afterglow model cannot reproduce the X-ray light curve of GRB 240825A,calling for improved models to characterize all multiwavelength data.展开更多
The main scientific payload of Macao Science Satellite-1B is a solar soft X-ray detection unit.To obtain an accurate solar X-ray spectrum,we have designed low-noise,high-throughput electronics.Solar radiation is detec...The main scientific payload of Macao Science Satellite-1B is a solar soft X-ray detection unit.To obtain an accurate solar X-ray spectrum,we have designed low-noise,high-throughput electronics.Solar radiation is detected using a low-leakage silicon drift detector(SDD),which is cooled to-30℃.The SDD output is processed using two parallel shaping amplifiers with peaking times of 315 ns and 65 ns.The amplifiers are designed using two-pole multiple-feedback active low-pass filters optimized to achieve a Bessel response.The differential output of the shaping amplifier generates a bipolar signal.The phase of the differential stage is tuned to ensure zero crossing corresponding to the peak of the shaping amplifier.A high-speed switch is inserted between the shaping amplifier and the peak-hold capacitor,and the peak value is maintained by turning off the switch.Fast and slow peak-hold circuits share a common ADC via time-division multiplexing.Both peak values are sampled for space-background rejection.Traditional pile-up detection methods cannot distinguish pulses that overlap in a fast channel.In this study,the differential of the“fast shaping”is selected,enabling the distinction of events separated by as little as 65ns,which is crucial for solar flare detection.The energy resolution is measured to be 138 eV at 5.90 keV.The centroid drift is less than 3.6 eV between-5℃ and 20℃.Compared with other solar X-ray instruments,this study demonstrates improved energy resolution with a lower peaking time,indicating a higher solar flare detection capability.展开更多
Supernova remnants(SNRs)interacting with molecular clouds(MCs)are recognized as the sources of γ-rays and cosmic rays in the Galaxy.Based on the SNR-MC system,this study establishes a particle cumulative diffusion mo...Supernova remnants(SNRs)interacting with molecular clouds(MCs)are recognized as the sources of γ-rays and cosmic rays in the Galaxy.Based on the SNR-MC system,this study establishes a particle cumulative diffusion model to investigate the mechanism by which high-energy protons escaping from SNRs interact with dense MCs through proton–proton interactions to produce high-energyγ-rays.Using the W51 complex,a typical star-forming region,as a research sample,we analyze the production and propagation characteristics of γ-rays.By employing the Exponential Cutoff Power-Law model and the Markov Chain Monte Carlo method,we fit theγ-ray observational data of W51C,successfully constraining the key physical parameters.Additionally,we systematically search for 1LHAASO sources spatially coincident with SNR-MC systems to explore the potential origins of ultra-high-energy(UHE) γ-ray sources.The results indicate that the radiation characteristics of the UHE γ-ray sources are highly consistent with the SNR-MC systems,further supporting their candidacy as PeVatrons in the Galaxy.展开更多
The study of high-energy gamma-ray emission from gamma-ray bursts(GRBs)involves complex synchrotron radiation and synchrotron self-Compton(SSC)scattering mechanisms with multiple parameters exhibiting a wide distribut...The study of high-energy gamma-ray emission from gamma-ray bursts(GRBs)involves complex synchrotron radiation and synchrotron self-Compton(SSC)scattering mechanisms with multiple parameters exhibiting a wide distribution.Recent advancements in GRB research,particularly the observation of very high energy(VHE,>100 Ge V)radiation,have ushered in a new era of multiwavelength exploration,offering fresh perspectives and limitations for understanding GRB radiation mechanisms.This study aimed to leverage VHE observations to refine constraints on synchrotron+SSC radiation from electrons accelerated by forward shocks.By analyzing two external environments—the uniform interstellar medium and stratified stellar wind medium,we conducted spectral and variability fitting for five specific bursts(GRB 180720B,GRB 190114C,GRB 190829A,GRB 201216C,and GRB 221009A)to identify the optimal parameters characterizing these events.A comparative analysis of model parameter distributions with and without VHE radiation observations reveals that the magnetic energy equipartition factorεBis more concentrated with VHE emissions.This suggests that VHE emissions may offer greater constraints on this microphysical parameter.Additionally,we found that the energy budget between VHE and ke V–Me Vγ-ray emissions under the SSC radiation exhibits an almost linear relationship,which may serve as a tool to differentiate radiation mechanisms.We anticipate future statistical analyses of additional VHE bursts to validate our findings.展开更多
We perform a time-resolved statistical study of GRB 221009A’s X-ray emission using Swift XRT Photon Counting and Windowed Timing data.After standard reduction(barycentric correction,pile-up,background subtraction via...We perform a time-resolved statistical study of GRB 221009A’s X-ray emission using Swift XRT Photon Counting and Windowed Timing data.After standard reduction(barycentric correction,pile-up,background subtraction via HEASOFT),we extracted light curves for each observational ID and for their aggregation.Countrate histograms were fitted using various statistical distributions;fit quality was assessed by chi-squared and the Bayesian Information Criterion.The first observational segment is best described by a Gaussian distribution(χ^(2)=68.4;BIC=7651.2),and the second by a Poisson distribution(χ^(2)=33.5;BIC=4413.3).When all segments are combined,the lognormal model provides the superior fit(χ^(2)=541.9;BIC=34365.5),indicating that the full data set’s count rates exhibit the skewness expected from a multiplicative process.These findings demonstrate that while individual time intervals conform to discrete or symmetric statistics,the collective emission profile across multiple observations is better captured by a lognormal distribution,consistent with complex,compounded variability in GRB afterglows.展开更多
近年来,随着宇宙线探测技术的不断提高,各空间探测实验对宇宙线粒子进行了高精度测量.其中,在宇宙线原初粒子和次级粒子能谱中,均发现在几百GV处存在能谱变硬特征.特别是,阿尔法磁谱仪2(Alpha Magnetic Spectrometer 2,AMS-2)实验发现...近年来,随着宇宙线探测技术的不断提高,各空间探测实验对宇宙线粒子进行了高精度测量.其中,在宇宙线原初粒子和次级粒子能谱中,均发现在几百GV处存在能谱变硬特征.特别是,阿尔法磁谱仪2(Alpha Magnetic Spectrometer 2,AMS-2)实验发现次级粒子相较原初粒子能谱变硬程度更为显著.目前,导致这一现象的原因还尚未有定论.论文利用AMS-2、反物质探测和轻核天体物理载荷(Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics,PAMELA)、先进成分探测器(Advanced Composition Explorer,ACE)中的宇宙线同位素光谱仪(Cosmic Ray Isotope Spectrometer,CRIS)(ACE-CRIS)以及旅行者1号(Voyager-1)探测器的最新实验数据对这一问题进行了研究.数据包括质子(p)和碳核(C)两种类型的原初粒子能谱以及锂碳比(Li/C)、铍碳比(Be/C)和硼碳比(B/C)3种类型的次级粒子原初粒子能谱比.论文分别假定高能区变硬现象是由发射谱拐折或是扩散拐折两种不同因素所导致,在此基础上对扩散-重加速(diffusionreacceleration,DR)以及扩散-对流(diffusion-convection,DC)两种不同的模型框架进行分析.在各模型框架下,计算结果显示:在低-中能区,各模型扩散指数δ_(L)的最佳估算值在0.41-0.48之间.其中,DR模型所需的δ_(L)值要比DC模型低0.06左右,这说明相较于对流,重加速机制会导致(Li,Be,B)/C在1至几百GeV/n之间的形状变陡.因此,拟合同样的(Li,Be,B)/C数据,DR模型所需的扩散指数更小.在高能区,结合暗物质探测卫星实验(the Dark Matter Particle Explorer,DAMPE)测量的B/C数据,我们发现相较于注入谱的高能拐折效应,DAMPE观测到的B/C高能区硬化现象更倾向于用扩散指数的变化来解释.不管是DR还是DC模型,得到的扩散指数拐折参数△δ都约为-0.19.展开更多
自触发射电阵列的设计是宇宙线大气簇射的射电探测所面临的机遇和难题之一,例如由背景源产生高振幅的瞬时噪声会导致射电阵列的误触发,而阵列设计需要避免由噪声导致的误触发.大气簇射射电信号独有的偏振特征为解决阵列的误触发问题提...自触发射电阵列的设计是宇宙线大气簇射的射电探测所面临的机遇和难题之一,例如由背景源产生高振幅的瞬时噪声会导致射电阵列的误触发,而阵列设计需要避免由噪声导致的误触发.大气簇射射电信号独有的偏振特征为解决阵列的误触发问题提供了解决方案,而利用信号偏振特征解决阵列误触发的方法的前提是射电信号的电场重建.由于背景噪声也会通过天线响应耦合到最终的观测数据中,这对正确重建射电信号的电场构成不可忽视的挑战.基于GRAND(Giant Radio Array for Neutrino Detection)验证阵列GP300(GRAND-Proto 300)的样机,结合模拟软件ZHAireS(ZHS AIR-shower Extended Simulations)模拟大气簇射产生的射电信号,耦合三极化天线的真实响应并使用最小二乘法重建电场,研究了射电信号的偏振特性,最终统计了以偏振为基础的天线的触发效率.展开更多
基金supported by the National Natural Science Foundation of China(NSFC,grant Nos.12173100,11973097 and 12022302)the Youth Innovation Promotion Association CAS(Nos.2021317 and Y2021087)+1 种基金the Scientific Instrument Developing Project of the CAS(No.20200077)the Strategic Priority Research Program on Space Science,Chinese Academy of Sciences(No.XDA 15320104).
文摘The Hard X-ray Imager(HXI)payload,a component of China’s Advanced Space-based Solar Observatory satellite,is designed to observe solar X-ray emissions in the 30-200 keV range,with the aim of investigating nonthermal physical processes during solar flares.Before launch,Geant4 simulations were employed to assess the onorbit background of the HXI instrument,evaluating its performance and potential to achieve its scientific objectives.This study addresses issues identified in previous simulations and conducts further analyses to examine the distribution of background counts across the 99 detectors.The results demonstrate alignment between simulations and observations at low and medium geomagnetic latitudes;however,challenges persist at high geomagnetic latitudes due to limitations in the current albedo photon model.This investigation provides insights into background sources from various particles,enhances understanding of space background characteristics,and offers guidance for background subtraction in imaging processes.
基金supported by the National Key R&D Program of China(grant No.2024YFA1611600)the SVOM project(a mission under the Strategic Priority Program on Space Science of the Chinese Academy of Sciences)+23 种基金the Strategic Priority Research Program of the Chinese Academy of Sciences(grant No.XDB0550401)the National Natural Science Foundation of China(NSFC,grant No.12494573)partly supported by Natural Science Foundation of Xinjiang Uygur Autonomous Region(grant No.2024D01D32)Tianshan Talent Training Program(grant No.2023TSYCLJ0053)Tianshan Innovation Team Program(grant No.2024D14015)supported by the Jiangsu Funding Program for Excellent Postdoctoral Talent(grant No.2024ZB110)the Postdoctoral Fellowship Program(grant No.GZC20241916)the General Fund(grant No.2024M763531)of the China Postdoctoral Science Foundationsupported by a Royal Society Dorothy Hodgkin Fellowship(grant Nos.DHF-R1-221175 and DHF-ERE-221005)support by a postdoctoral fellowship from the CNESsupported by the National Key R&D Program of China(grant No.2024YFA1611702)the Strategic Priority Research Program of the Chinese Academy of Sciences(grant No.XDB0550101)the support of the French Agence Nationale de la Recherche(ANR),under grant ANR-23-CE31-0011(project PEGaSUS)financial support from the GRAWITA Large Program Grant(PI P.D’Avanzo)financial support from the Italian Space Agency,contract ASI/INAF No.I/004/11/6support from the INAF project Premiale Supporto Arizona&Italiasupported by the National Natural Science Foundation of China(NSFC,grant No.12133003)supported by the National Natural Science Foundation of China(NSFC,grant No.12373042)the Bagui Scholars Program(No.GXR-6BG2424001)funded by the European Union(ERC,HEAVYMETAL,101071865,Views and opinions expressed are,however,those of the authors only and do not necessarily reflect those of the European Union or the European Research Council Neither the European Union nor the granting authority can be held responsible for them)the Cosmic Dawn Center(DAWN)is funded by the Danish National Research Foundation under grant No.DNRF140supported by the National Natural Science Foundation of China(NSFC,grant Nos.12225305 and 12321003)supported by the National Natural Science Foundation of China(NSFC,grant No.12473049)supported by the General Fund(grant No.2024M763530)of the China Postdoctoral Science Foundation。
文摘Early multiwavelength observations offer crucial insights into the nature of the relativistic jets responsible for gamma-ray bursts and their interaction with the surrounding medium.We present data of GRB 240825A from 17 space-and ground-based telescopes/instruments,covering wavelengths from NIR/optical to X-ray and GeV,and spanning from the prompt emission to the afterglow phase triggered by Swift and Fermi.The early afterglow observations were carried out by SVOM/C-GFT,and spectroscopic observations of the afterglow by GTC,VLT,and TNG determined the redshift of the burst(z=0.659)later.A comprehensive analysis of the prompt emission spectrum observed by Swift-BAT and Fermi-GBM/LAT reveals a rare and significant high-energy cutoff at 76 MeV.Assuming this cutoff is due toγγabsorption allows us to place an upper limit on the initial Lorentz factor,Γ_(0)<245.The optical/NIR and GeV afterglow light curves can be described by the standard external shock model,with early-time emission dominated by a reverse shock(RS)and a subsequent transition to forward shock(FS)emission.Our afterglow modeling yields a consistent estimate of the initial Lorentz factor(Γ_(0)∼234).Furthermore,the RS-to-FS magnetic field ratio(R 302B)indicates that the RS region is significantly more magnetized than the FS region.An isotropic-equivalent kinetic energy of E_(k,iso)=5.25×10^(54) erg is derived,and the correspondingγ-ray radiation efficiency is estimated to beη_(γ)=3.1%.On the other hand,the standard afterglow model cannot reproduce the X-ray light curve of GRB 240825A,calling for improved models to characterize all multiwavelength data.
基金supported by the National Natural Science Foundation of China(No.12035020)National Key Scientific Instrument and Equipment Development Projects of China(No.42327802).
文摘The main scientific payload of Macao Science Satellite-1B is a solar soft X-ray detection unit.To obtain an accurate solar X-ray spectrum,we have designed low-noise,high-throughput electronics.Solar radiation is detected using a low-leakage silicon drift detector(SDD),which is cooled to-30℃.The SDD output is processed using two parallel shaping amplifiers with peaking times of 315 ns and 65 ns.The amplifiers are designed using two-pole multiple-feedback active low-pass filters optimized to achieve a Bessel response.The differential output of the shaping amplifier generates a bipolar signal.The phase of the differential stage is tuned to ensure zero crossing corresponding to the peak of the shaping amplifier.A high-speed switch is inserted between the shaping amplifier and the peak-hold capacitor,and the peak value is maintained by turning off the switch.Fast and slow peak-hold circuits share a common ADC via time-division multiplexing.Both peak values are sampled for space-background rejection.Traditional pile-up detection methods cannot distinguish pulses that overlap in a fast channel.In this study,the differential of the“fast shaping”is selected,enabling the distinction of events separated by as little as 65ns,which is crucial for solar flare detection.The energy resolution is measured to be 138 eV at 5.90 keV.The centroid drift is less than 3.6 eV between-5℃ and 20℃.Compared with other solar X-ray instruments,this study demonstrates improved energy resolution with a lower peaking time,indicating a higher solar flare detection capability.
基金supported by NSFC grant No.12393852the Yunnan Fundamental Research Project(grant No.202501AS070068).
文摘Supernova remnants(SNRs)interacting with molecular clouds(MCs)are recognized as the sources of γ-rays and cosmic rays in the Galaxy.Based on the SNR-MC system,this study establishes a particle cumulative diffusion model to investigate the mechanism by which high-energy protons escaping from SNRs interact with dense MCs through proton–proton interactions to produce high-energyγ-rays.Using the W51 complex,a typical star-forming region,as a research sample,we analyze the production and propagation characteristics of γ-rays.By employing the Exponential Cutoff Power-Law model and the Markov Chain Monte Carlo method,we fit theγ-ray observational data of W51C,successfully constraining the key physical parameters.Additionally,we systematically search for 1LHAASO sources spatially coincident with SNR-MC systems to explore the potential origins of ultra-high-energy(UHE) γ-ray sources.The results indicate that the radiation characteristics of the UHE γ-ray sources are highly consistent with the SNR-MC systems,further supporting their candidacy as PeVatrons in the Galaxy.
基金supported by the National Natural Science Foundation of China(NSFC,grant Nos.12275279 and 12405124)the China Postdoctoral Science Foundation(No.2023M730423)Horizontal research project in natural sciences(No.H20230120)。
文摘The study of high-energy gamma-ray emission from gamma-ray bursts(GRBs)involves complex synchrotron radiation and synchrotron self-Compton(SSC)scattering mechanisms with multiple parameters exhibiting a wide distribution.Recent advancements in GRB research,particularly the observation of very high energy(VHE,>100 Ge V)radiation,have ushered in a new era of multiwavelength exploration,offering fresh perspectives and limitations for understanding GRB radiation mechanisms.This study aimed to leverage VHE observations to refine constraints on synchrotron+SSC radiation from electrons accelerated by forward shocks.By analyzing two external environments—the uniform interstellar medium and stratified stellar wind medium,we conducted spectral and variability fitting for five specific bursts(GRB 180720B,GRB 190114C,GRB 190829A,GRB 201216C,and GRB 221009A)to identify the optimal parameters characterizing these events.A comparative analysis of model parameter distributions with and without VHE radiation observations reveals that the magnetic energy equipartition factorεBis more concentrated with VHE emissions.This suggests that VHE emissions may offer greater constraints on this microphysical parameter.Additionally,we found that the energy budget between VHE and ke V–Me Vγ-ray emissions under the SSC radiation exhibits an almost linear relationship,which may serve as a tool to differentiate radiation mechanisms.We anticipate future statistical analyses of additional VHE bursts to validate our findings.
文摘We perform a time-resolved statistical study of GRB 221009A’s X-ray emission using Swift XRT Photon Counting and Windowed Timing data.After standard reduction(barycentric correction,pile-up,background subtraction via HEASOFT),we extracted light curves for each observational ID and for their aggregation.Countrate histograms were fitted using various statistical distributions;fit quality was assessed by chi-squared and the Bayesian Information Criterion.The first observational segment is best described by a Gaussian distribution(χ^(2)=68.4;BIC=7651.2),and the second by a Poisson distribution(χ^(2)=33.5;BIC=4413.3).When all segments are combined,the lognormal model provides the superior fit(χ^(2)=541.9;BIC=34365.5),indicating that the full data set’s count rates exhibit the skewness expected from a multiplicative process.These findings demonstrate that while individual time intervals conform to discrete or symmetric statistics,the collective emission profile across multiple observations is better captured by a lognormal distribution,consistent with complex,compounded variability in GRB afterglows.
文摘近年来,随着宇宙线探测技术的不断提高,各空间探测实验对宇宙线粒子进行了高精度测量.其中,在宇宙线原初粒子和次级粒子能谱中,均发现在几百GV处存在能谱变硬特征.特别是,阿尔法磁谱仪2(Alpha Magnetic Spectrometer 2,AMS-2)实验发现次级粒子相较原初粒子能谱变硬程度更为显著.目前,导致这一现象的原因还尚未有定论.论文利用AMS-2、反物质探测和轻核天体物理载荷(Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics,PAMELA)、先进成分探测器(Advanced Composition Explorer,ACE)中的宇宙线同位素光谱仪(Cosmic Ray Isotope Spectrometer,CRIS)(ACE-CRIS)以及旅行者1号(Voyager-1)探测器的最新实验数据对这一问题进行了研究.数据包括质子(p)和碳核(C)两种类型的原初粒子能谱以及锂碳比(Li/C)、铍碳比(Be/C)和硼碳比(B/C)3种类型的次级粒子原初粒子能谱比.论文分别假定高能区变硬现象是由发射谱拐折或是扩散拐折两种不同因素所导致,在此基础上对扩散-重加速(diffusionreacceleration,DR)以及扩散-对流(diffusion-convection,DC)两种不同的模型框架进行分析.在各模型框架下,计算结果显示:在低-中能区,各模型扩散指数δ_(L)的最佳估算值在0.41-0.48之间.其中,DR模型所需的δ_(L)值要比DC模型低0.06左右,这说明相较于对流,重加速机制会导致(Li,Be,B)/C在1至几百GeV/n之间的形状变陡.因此,拟合同样的(Li,Be,B)/C数据,DR模型所需的扩散指数更小.在高能区,结合暗物质探测卫星实验(the Dark Matter Particle Explorer,DAMPE)测量的B/C数据,我们发现相较于注入谱的高能拐折效应,DAMPE观测到的B/C高能区硬化现象更倾向于用扩散指数的变化来解释.不管是DR还是DC模型,得到的扩散指数拐折参数△δ都约为-0.19.
文摘自触发射电阵列的设计是宇宙线大气簇射的射电探测所面临的机遇和难题之一,例如由背景源产生高振幅的瞬时噪声会导致射电阵列的误触发,而阵列设计需要避免由噪声导致的误触发.大气簇射射电信号独有的偏振特征为解决阵列的误触发问题提供了解决方案,而利用信号偏振特征解决阵列误触发的方法的前提是射电信号的电场重建.由于背景噪声也会通过天线响应耦合到最终的观测数据中,这对正确重建射电信号的电场构成不可忽视的挑战.基于GRAND(Giant Radio Array for Neutrino Detection)验证阵列GP300(GRAND-Proto 300)的样机,结合模拟软件ZHAireS(ZHS AIR-shower Extended Simulations)模拟大气簇射产生的射电信号,耦合三极化天线的真实响应并使用最小二乘法重建电场,研究了射电信号的偏振特性,最终统计了以偏振为基础的天线的触发效率.
