WANG JiaLu, ZHANG LiCheng, SHEN ZhiHong, LI CongQiao, ZHANG ShuNan, LI ZhiYuan, HU WenHua, GENG XinYue, TONG XingYu, DAI XinChen, GAO YuanNing, MAO YaJun, BAN Yong, YANG ZhenWei, LI Qiang, WANG DaYong, ZHANG YanXi, SUN XiaoHu, ZHOU Chen
{"title":"Experimental progress of Higgs and flavor physics at the LHC","authors":"WANG JiaLu, ZHANG LiCheng, SHEN ZhiHong, LI CongQiao, ZHANG ShuNan, LI ZhiYuan, HU WenHua, GENG XinYue, TONG XingYu, DAI XinChen, GAO YuanNing, MAO YaJun, BAN Yong, YANG ZhenWei, LI Qiang, WANG DaYong, ZHANG YanXi, SUN XiaoHu, ZHOU Chen","doi":"10.1360/sspma-2022-0444","DOIUrl":"https://doi.org/10.1360/sspma-2022-0444","url":null,"abstract":"","PeriodicalId":44892,"journal":{"name":"Scientia Sinica-Physica Mechanica & Astronomica","volume":"21 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136235185","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}
As the only binary neutron star (BNS) merger detected thus far via both gravitational waves (GWs) and definitive electromagnetic (EM) counterparts, GW170817 not only provided crucial information for many astrophysical processes but also opened an exciting era of multi-messenger astronomy. However, due to the high operating frequency, ground-based GW detectors cannot provide alerts with a sufficient early-warning time, making it difficult for EM facilities to capture the early evolution of detectable BNS mergers. In view of this, we assess the detections and early-warning abilities of space-borne decihertz GW detectors for BNS mergers because they can provide alerts much earlier. We discuss the precision in localization and timing for two proposed decihertz GW observatories, B-DECIGO and DO-Conservative, as an extension of recent work. During an assumed 4-year mission time, sources that merge in 1–4 years will yield the most precise angular resolution with ΔΩ~10 –2 deg 2 and time-of-merger accuracy with Δ t c ~0.2 s. After BNS mergers, we examine the possibility of multi-messenger early-warning detections with space-borne decihertz GW detectors for different types of EM transients, covering γ-ray/X-ray to radio bands. Based on our analyses, we propose that a “wait-for” detection scheme could open up new opportunities for future multi-messenger astronomy.
{"title":"Multi-messenger detections of binary neutron star mergers powered by decihertz gravitational-wave observations","authors":"YaCheng KANG, Chang LIU, JinPing ZHU, LiJing SHAO","doi":"10.1360/sspma-2022-0428","DOIUrl":"https://doi.org/10.1360/sspma-2022-0428","url":null,"abstract":"As the only binary neutron star (BNS) merger detected thus far via both gravitational waves (GWs) and definitive electromagnetic (EM) counterparts, GW170817 not only provided crucial information for many astrophysical processes but also opened an exciting era of multi-messenger astronomy. However, due to the high operating frequency, ground-based GW detectors cannot provide alerts with a sufficient early-warning time, making it difficult for EM facilities to capture the early evolution of detectable BNS mergers. In view of this, we assess the detections and early-warning abilities of space-borne decihertz GW detectors for BNS mergers because they can provide alerts much earlier. We discuss the precision in localization and timing for two proposed decihertz GW observatories, B-DECIGO and DO-Conservative, as an extension of recent work. During an assumed 4-year mission time, sources that merge in 1–4 years will yield the most precise angular resolution with ΔΩ~10 –2 deg 2 and time-of-merger accuracy with Δ t c ~0.2 s. After BNS mergers, we examine the possibility of multi-messenger early-warning detections with space-borne decihertz GW detectors for different types of EM transients, covering γ-ray/X-ray to radio bands. Based on our analyses, we propose that a “wait-for” detection scheme could open up new opportunities for future multi-messenger astronomy.","PeriodicalId":44892,"journal":{"name":"Scientia Sinica-Physica Mechanica & Astronomica","volume":"36 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136309089","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}
The foundation of the development of flexible semiconductor and micro-nano ultrafast response devices in the post-Moore era is to measure and manipulate ultrafast optical physical processes in new materials and devices with extreme spatiotemporal small-scale. The spatiotemporal-and energy-resolved photoemission electron microscopy (PEEM) combines the pump-probe optical scheme with the electron microscopic imaging technology and possesses femtosecond-nanometer time-space resolution. It has evolved into an excellent ultrafast microscopy technique for investigating nanophotonics and low-dimensional device physics, leading to the revolutionary development of plasmonics, semiconductor science and related cross-disciplinary studies. In this review, we have summarized the application of PEEM in micro-nano plasmonic function devices, high-order plasmonic vortex fields, plasmonic skyrmion, and low-dimensional semiconductors. Finally, we discussed the future opportunities of PEEM. the spatiotemporal and energy-resolved photoemission electron microscope, plasmonic function devices, high-order plasmonic vortices, plasmonic skyrmion, low dimensional semiconductor materials PACS
{"title":"Ultrafast photoelectron imaging with high spatiotemporal and energy resolution","authors":"YuLu QIN, Rui WANG, YunQuan LIU","doi":"10.1360/sspma-2022-0442","DOIUrl":"https://doi.org/10.1360/sspma-2022-0442","url":null,"abstract":"The foundation of the development of flexible semiconductor and micro-nano ultrafast response devices in the post-Moore era is to measure and manipulate ultrafast optical physical processes in new materials and devices with extreme spatiotemporal small-scale. The spatiotemporal-and energy-resolved photoemission electron microscopy (PEEM) combines the pump-probe optical scheme with the electron microscopic imaging technology and possesses femtosecond-nanometer time-space resolution. It has evolved into an excellent ultrafast microscopy technique for investigating nanophotonics and low-dimensional device physics, leading to the revolutionary development of plasmonics, semiconductor science and related cross-disciplinary studies. In this review, we have summarized the application of PEEM in micro-nano plasmonic function devices, high-order plasmonic vortex fields, plasmonic skyrmion, and low-dimensional semiconductors. Finally, we discussed the future opportunities of PEEM. the spatiotemporal and energy-resolved photoemission electron microscope, plasmonic function devices, high-order plasmonic vortices, plasmonic skyrmion, low dimensional semiconductor materials PACS","PeriodicalId":44892,"journal":{"name":"Scientia Sinica-Physica Mechanica & Astronomica","volume":"13 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135436740","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}
Nuclear first-principles (or called ab initio ) studies are the frontier of theoretical nuclear physics research for their reliable predictions and the ability to guide experiments. It bridges low-energy nuclear physics and the fundamental theory (quantum chromodynamics QCD) through the Chiral effective field theory. In past decades, ab initio methods have gained great success, benefiting from developments of quantum many-body methods and computer hardware. Using the innovative quantum many-body methods and the chiral potential that is fitted to low-energy nucleon-nucleon scattering data, ab initio calculations have been pushed from the light mass nuclei to heavy mass nuclei, from well-bound stable nuclei to weakly bound or unbound nuclei. During pasting years, we have been concentrating on exploring two aspects in ab initio calculations: chiral three-body forces and continuum effects. Chiral three-body forces have been shown to have broad influences on both the properties of finite nuclei and nuclear matter. Continuum effects are the key ingredient in the calculations of weakly bound or unbound nuclei. This paper reviews the series of achievements that we gained in the development of chiral three-body forces and ab initio Gamow shell model which takes the continuum coupling into account.
{"title":"Chiral three-body forces and nuclear first-principles studies","authors":"YuanZhuo MA, JianGuo LI, ZhongHao SUN, BaiShan HU, Shuang ZHANG, FuRong XU","doi":"10.1360/sspma-2022-0432","DOIUrl":"https://doi.org/10.1360/sspma-2022-0432","url":null,"abstract":"Nuclear first-principles (or called ab initio ) studies are the frontier of theoretical nuclear physics research for their reliable predictions and the ability to guide experiments. It bridges low-energy nuclear physics and the fundamental theory (quantum chromodynamics QCD) through the Chiral effective field theory. In past decades, ab initio methods have gained great success, benefiting from developments of quantum many-body methods and computer hardware. Using the innovative quantum many-body methods and the chiral potential that is fitted to low-energy nucleon-nucleon scattering data, ab initio calculations have been pushed from the light mass nuclei to heavy mass nuclei, from well-bound stable nuclei to weakly bound or unbound nuclei. During pasting years, we have been concentrating on exploring two aspects in ab initio calculations: chiral three-body forces and continuum effects. Chiral three-body forces have been shown to have broad influences on both the properties of finite nuclei and nuclear matter. Continuum effects are the key ingredient in the calculations of weakly bound or unbound nuclei. This paper reviews the series of achievements that we gained in the development of chiral three-body forces and ab initio Gamow shell model which takes the continuum coupling into account.","PeriodicalId":44892,"journal":{"name":"Scientia Sinica-Physica Mechanica & Astronomica","volume":"19 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134912259","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}
The broad emission line region size of active galactic nuclei (AGN) is an important parameter for calculating the mass of the central black hole. Usually, the size is measured by spectral reverberation mapping to obtain the time lag between the broad emission line and continuum radiations, but measurement using intermediate or large optical telescopes is time-consuming. Here, we adopt another method to perform photometric reverberation mapping. We used a 60-cm telescope at the Xinglong station of the National Astronomical Observatories of China (NAOC) to observe six AGNs at redshift z ≃ 0 . 3. We used the V broad band to trace the continuum and the narrow OIII band to trace the redshifted H β emission line. To eliminate the influence of the continuum in the OIII band, we assumed that the continuum flux in the narrow band is equal to a fixed fraction α of the flux in the continuum band for each AGN. Under this assumption, we subtracted the continuum band flux with the ratio α from the narrow-band flux and obtained the light curve of the H β line via the improved interpolated cross-correlation function (ICCF) method (ICCF-Cut). The extracted H β light curves were compared with the lagged continuum band light curves. We also used another method JAVELIN to calculate the H β time lags. The H β time lags obtained from the ICCF-Cut and JAVELIN were consistent with the results of spectroscopic reverberation mapping for two AGNs (Mrk 335 and 3C 120). The H β time lags obtained from ICCF-Cut were 7 . 8 + 8 . 0 − 11 . 4 and 13 . 5 + 13 . 0 − 8 . 8 d. To explain why only two of the six AGNs had good results, we used the damped random walk (DRW) model to simulate the light curves of AGNs and found that the photometric reverberation mapping required su ffi cient observations with high cadence. The observation and simulation results revealed that combining the ICCF-Cut and JAVELIN results may enable us to obtain reliable emission line lags for AGNs with large variability and high cadence, although the errors of lags are large.
{"title":"Photometric reverberation mapping of several active galactic nuclei","authors":"MA Qinchun, WU Xue-Bing","doi":"10.1360/sspma-2022-0451","DOIUrl":"https://doi.org/10.1360/sspma-2022-0451","url":null,"abstract":"The broad emission line region size of active galactic nuclei (AGN) is an important parameter for calculating the mass of the central black hole. Usually, the size is measured by spectral reverberation mapping to obtain the time lag between the broad emission line and continuum radiations, but measurement using intermediate or large optical telescopes is time-consuming. Here, we adopt another method to perform photometric reverberation mapping. We used a 60-cm telescope at the Xinglong station of the National Astronomical Observatories of China (NAOC) to observe six AGNs at redshift z ≃ 0 . 3. We used the V broad band to trace the continuum and the narrow OIII band to trace the redshifted H β emission line. To eliminate the influence of the continuum in the OIII band, we assumed that the continuum flux in the narrow band is equal to a fixed fraction α of the flux in the continuum band for each AGN. Under this assumption, we subtracted the continuum band flux with the ratio α from the narrow-band flux and obtained the light curve of the H β line via the improved interpolated cross-correlation function (ICCF) method (ICCF-Cut). The extracted H β light curves were compared with the lagged continuum band light curves. We also used another method JAVELIN to calculate the H β time lags. The H β time lags obtained from the ICCF-Cut and JAVELIN were consistent with the results of spectroscopic reverberation mapping for two AGNs (Mrk 335 and 3C 120). The H β time lags obtained from ICCF-Cut were 7 . 8 + 8 . 0 − 11 . 4 and 13 . 5 + 13 . 0 − 8 . 8 d. To explain why only two of the six AGNs had good results, we used the damped random walk (DRW) model to simulate the light curves of AGNs and found that the photometric reverberation mapping required su ffi cient observations with high cadence. The observation and simulation results revealed that combining the ICCF-Cut and JAVELIN results may enable us to obtain reliable emission line lags for AGNs with large variability and high cadence, although the errors of lags are large.","PeriodicalId":44892,"journal":{"name":"Scientia Sinica-Physica Mechanica & Astronomica","volume":"22 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134913136","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}
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