GUO Sai-shan was born on October 24, 1938, in Putian Fujian Province, 1960 graduated in Shanghai First Medical College （now Shanghai Medical University）. At present, she is the Professor of Peking Union Medical Coll...GUO Sai-shan was born on October 24, 1938, in Putian Fujian Province, 1960 graduated in Shanghai First Medical College （now Shanghai Medical University）. At present, she is the Professor of Peking Union Medical College. Chief Doctor,Post-doctorate Tutor, in 1991 to 2002 she was appointed as Director of Department of Traditional Chinese Medicine （TOM）;展开更多
Magnetic reconnection driving a two-sided-loop jet is typically associated with interactions between an emerging bipole and the overlying horizontal magnetic field,or between filaments from separate magnetic systems.L...Magnetic reconnection driving a two-sided-loop jet is typically associated with interactions between an emerging bipole and the overlying horizontal magnetic field,or between filaments from separate magnetic systems.Leveraging high temporal and spatial resolution observations from ground-based and space-borne instruments,we have identified a two-sided-loop jet originating from magnetic reconnection between threads within a single filament.Our observations show that as two initially crossing filamentary threads within the filament converge,reconnection takes place at their intersection.In the Doppler images,distinct redshift and blueshift signals are observed at the locations where the filament threads intersected.This process generates a two-sided-loop jet with outflow speeds of 22.2 and 62.5 km s^(-1).Following reconnection,the original crossing threads transform into two parallel threads that subsequently separate at speeds of 2.8 and 8.3kms^(-1).This observation offers a new perspective on the mechanisms responsible for jet formation.展开更多
A 50 mm balloon-borne white-light coronagraph(BBWLC)to observe white-light solar corona over the altitude range from 1.08 R_(⊙)to 1.50 R_(⊙)has recently been indigenously developed by Yunnan Observatories in collabo...A 50 mm balloon-borne white-light coronagraph(BBWLC)to observe white-light solar corona over the altitude range from 1.08 R_(⊙)to 1.50 R_(⊙)has recently been indigenously developed by Yunnan Observatories in collaboration with Shandong University(in Weihai)and Changchun Institute of Optics,Fine Mechanics and Physics,which will significantly improve the ability of China to detect and measure the inner corona.On 2022 October 4,its first scientific flight took place at the Dachaidan area in Qinghai province of China.We briefly describe the BBWLC mission including its optical design,mechanical structure,pointing system,the first flight and results associated with the data processing approach.Preliminary analysis of the data shows that BBWLC imaged the K-corona with three streamer structures on the west limb of the Sun.To further confirm the coronal signals obtained by BBWLC,comparisons were made with observations of the K-coronagraph of the High Altitude Observatory and the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory.We conclude that BBWLC eventually observed the white-light corona in its first scientific flight.展开更多
The assortedness of Chinese food,together with the complexity of their naming elements,has ignited numerous scholars' interests in this field and prompted them to make abundant analyses of Chinese dish names.Most ...The assortedness of Chinese food,together with the complexity of their naming elements,has ignited numerous scholars' interests in this field and prompted them to make abundant analyses of Chinese dish names.Most of them,however,were done in studies of traditional linguistics,rhetoric,translatology and cross-cultural communication.And studies,based on corpus,on the naming elements of Chinese dishes under cognitive linguistic theories almost remain a blank.This paper aims to conduct a quantitative analysis of 4,000 Chinese dish names(500 ones selected freely from each of the eight cuisines),based on the Prominence Principle,in order to identify the specific naming elements of Chinese dishes and forward related statistics and ratios.展开更多
Magnetic flux ropes are characterized by coherently twisted magnetic field lines,which are ubiquitous in magnetized plasmas.As the core structure of various eruptive phenomena in the solar atmosphere,flux ropes hold t...Magnetic flux ropes are characterized by coherently twisted magnetic field lines,which are ubiquitous in magnetized plasmas.As the core structure of various eruptive phenomena in the solar atmosphere,flux ropes hold the key to understanding the physical mechanisms of solar eruptions,which impact the heliosphere and planetary atmospheres.The strongest disturbances in the Earth’s space environments are often associated with large-scale flux ropes from the Sun colliding with the Earth’s magnetosphere,leading to adverse,sometimes catastrophic,space-weather effects.However,it remains elusive as to how a flux rope forms and evolves toward eruption,and how it is structured and embedded in the ambient field.The present paper addresses these important questions by reviewing current understandings of coronal flux ropes from an observer’s perspective,with an emphasis on their structures and nascent evolution toward solar eruptions,as achieved by combining observations of both remote sensing and in-situ detection with modeling and simulation.This paper highlights an initiation mechanism for coronal mass ejections(CMEs)in which plasmoids in current sheets coalesce into a’seed’flux rope whose subsequent evolution into a CME is consistent with the standard model,thereby bridging the gap between microscale and macroscale dynamics.展开更多
During vertebrate embryonic development,neural crest-derived ectomesenchyme within the maxillary prominences undergoes precisely coordinated proliferation and differentiation to give rise to diverse craniofacial struc...During vertebrate embryonic development,neural crest-derived ectomesenchyme within the maxillary prominences undergoes precisely coordinated proliferation and differentiation to give rise to diverse craniofacial structures,such as tooth and palate.However,the transcriptional regulatory networks underpinning such an intricate process have not been fully elucidated.Here,we perform single-cell RNA-Seq to comprehensively characterize the transcriptional dynamics during mouse maxillary development from embryonic day(E)10.5eE14.5.Our single-cell transcriptome atlas of~28,000 cells uncovers mesenchymal cell populations representing distinct differentiating states and reveals their developmental trajectory,suggesting that the segregation of dental from the palatal mesenchyme occurs at E11.5.Moreover,we identify a series of key transcription factors(TFs)associated with mesenchymal fate transitions and deduce the gene regulatory networks directed by these TFs.Collectively,our study provides important resources and insights for achieving a systems-level understanding of craniofacial morphogenesis and abnormality.展开更多
Study of the small-scale structures and material flows associated with solar quiescent filaments is very important for understanding the formation and equilibrium of solar filaments. Using high resolution Ha data obse...Study of the small-scale structures and material flows associated with solar quiescent filaments is very important for understanding the formation and equilibrium of solar filaments. Using high resolution Ha data observed by the New Vacuum Solar Telescope, we present the structures of barbs and material flows along the threads across the spine in two quiescent filaments on 2013 September 29 and on 2012 November 2, respectively. During the evolution of the filament barb, several paral- lel tube-shaped structures formed and the width of the structures ranged from about 2.3 Mm to 3.3 Mm. The parallel tube-shaped structures merged together accompanied by material flows from the spine to the barb. Moreover, the boundary between the barb and surrounding atmosphere was very neat. The counter-streaming flows were not found to appear alternately in the adjacent threads of the filament. However, the large-scale patchy counter-streaming flows were detected in the filament. The flows in one patch of the filament have the same direction but flows in the adjacent patch have opposite direction. The patches of two opposite flows with a size of about 10＂ were alternately exhibited along the spine of the filament. The velocity of these material flows ranged from 5.6 km s^-1 to 15.0 km s^-1. The material flows along the threads of the filament did not change their direction for about two hours and fourteen minutes during the evolution of the filament. Our results confirm that the large-scale counter- streaming flows with a certain width along the threads of solar filaments exist and are coaligned well with the threads.展开更多
High-resolution Ha observations indicate that filaments consist of an as- sembly of thin threads. In quiescent filaments, the threads are generally short, whereas in active region filaments, the threads are generally ...High-resolution Ha observations indicate that filaments consist of an as- sembly of thin threads. In quiescent filaments, the threads are generally short, whereas in active region filaments, the threads are generally long. In order to explain these observational features, we performed one-dimensional radiative hydrodynamic sim- ulations of filament formation along a dipped magnetic flux tube in the framework of the chromospheric evaporation-coronal condensation model. The geometry of a dipped magnetic flux tube is characterized by three parameters, i.e., the depth （D）, the half-width （w） and the altitude （h） of the magnetic dip. A survey of the parame- ters in numerical simulations shows that when allowing the filament thread to grow in 5 days, the maximum length （Lth） of the filament thread increases linearly with w, and decreases linearly with D and h. The dependence is fitted into a linear function Lth = 0.84w --0.88D - 2.78h ＋ 17.31 （Mm）. Such a relation can qualitatively explain why quiescent filaments have shorter threads and active region filaments have longer threads.展开更多
We observed an Hα surge that occurred in NOAA Active Region 12401 on 2015 August 17, and we discuss its trigger mechanism, and kinematic and thermal properties. It is suggested that this surge was caused by a chromos...We observed an Hα surge that occurred in NOAA Active Region 12401 on 2015 August 17, and we discuss its trigger mechanism, and kinematic and thermal properties. It is suggested that this surge was caused by a chromospheric reconnection which ejected cool and dense material with transverse velocity of about 21–28 km s-1 and initial Doppler velocity of 12 km s^-1. This surge is similar to the injection of newly formed filament materials from their footpoints, except that the surge here occurred in a relatively weak magnetic environment of 100 G. Thus, we discuss the possibility of filament material replenishment via the erupting mass in such a weak magnetic field, which is often associated with quiescent filaments. It is found that the local plasma can be heated up to about 1.3 times the original temperature, which results in an acceleration of about –0.017 km s^-2. It can lift the dense material up to 10 Mm and higher with an inclination angle smaller than 50°, namely the typical height of active region filaments, but it can hardly inject the material up to those filaments higher than 25 Mm, like some quiescent filaments. Thus, we think that the injection model does not work well in describing the formation of quiescent filaments.展开更多
Mg-Gd-Y-Zr alloy,as a typical magnesium rare-earth(Mg-RE)alloy,is gaining popularity in the advanced equipment manufacturing fields owing to its noticeable age-hardening properties and high specific strength.However,i...Mg-Gd-Y-Zr alloy,as a typical magnesium rare-earth(Mg-RE)alloy,is gaining popularity in the advanced equipment manufacturing fields owing to its noticeable age-hardening properties and high specific strength.However,it is extremely challenging to prepare wrought components with large dimensions and complex shapes because of the poor room-temperature processability of Mg-Gd-Y-Zr alloy.Herein,we report a wire-arc directed energy deposited(DED)Mg-10.45Gd-2.27Y-0.52Zr(wt.%,GW102K)alloy with high RE content presenting a prominent combination of strength and ductility,realized by tailored nanoprecipitates through an optimized heat treatment procedure.Specifically,the solution-treated sample exhibits excellent ductility with an elongation(EL)of(14.6±0.1)%,while the aging-treated sample at 200°C for 58 h achieves an ultra-high ultimate tensile strength(UTS)of(371±1.5)MPa.Besides,the aging-treated sample at 250°C for 16 h attains a good strength-ductility synergy with a UTS of(316±2.1)MPa and a EL of(8.5±0.1)%.Particularly,the evolution mechanisms of precipitation response induced by various aging parameters and deformation behavior caused by nanoprecipitates type were also systematically revealed.The excellent ductility resulted from coordinating localized strains facilitated by active slip activity.And the ultra-high strength should be ascribed to the dense nano-β'hampering dislocation motion.Additionally,the shearable nano-β1 contributed to the good strength-ductility synergy.This work thus offers insightful understanding into the nanoprecipitates manipulation and performance tailoring for the wire-arc DED preparation of large-sized Mg-Gd-Y-Zr components with complex geometries.展开更多
Solar filaments are an intriguing phenomenon,like cool clouds suspended in the hot corona.Similar structures exist in the intergalactic medium as well.Despite being a long-studied topic,solar filaments have continuall...Solar filaments are an intriguing phenomenon,like cool clouds suspended in the hot corona.Similar structures exist in the intergalactic medium as well.Despite being a long-studied topic,solar filaments have continually attracted intensive attention because of their link to coronal heating,coronal seismology,solar flares and coronal mass ejections(CMEs).In this review paper,by combing through the solar filament-related work done in the past decade,we discuss several controversial topics,such as the fine structures,dynamics,magnetic configurations and helicity of filaments.With high-resolution and highsensitivity observations,combined with numerical simulations,it is expected that resolving these disputes will definitely lead to a huge leap in understanding the physics related to solar filaments,and even shed light on galactic filaments.展开更多
After surveying the spectra of 39 prominences observed by the Multi-channel Infrared Solar Spectrograph at Purple Mountain Observatory and the 25 cm coronagraph at the Norikura Solar Observatory, we found that about 2...After surveying the spectra of 39 prominences observed by the Multi-channel Infrared Solar Spectrograph at Purple Mountain Observatory and the 25 cm coronagraph at the Norikura Solar Observatory, we found that about 28% of them show small spatial scale (6''–8'') and short time scale (tens of seconds to a few minutes), unusual large broadening and large shift velocities in spectral lines including Hα, Hβ, H, Ca II H, Ca II K, Ca II 8542?, He I D3 and He I 10830?. We present in detail two typical events observed respectively on 2002 May 27 and 1981 August 2. The full-width at half maximum of the widest profile of the 2001 prominence is 1.8? for Hα and 2.9 ? for He I 10830?, while that of the 1981 prominence is 5.3 ? for Hβ, 3.6 ? for Ca II K, 4.0 ? for Ca II H and 2.8 ? for He I D3. Such broadenings generally occur at a level of several-thousand kilometres above the chromosphere. Further, most of these prominences manifest a rotation of (0.4–1.35)×10<SUP>-2</SUP> rads s<SUP>?1</SUP> pointing to the Sun and large line-of-sight velocities of 20–200 km s<SUP>?1</SUP>. Some of these events correspond in time to an enhancement or a small peak in the GOES X-ray flux, indicating the existence of high energy process at work. These prominences generally display discernible changes in the Hα morphology around the time of large broadening, but do not show Hα brightening or overall eruption except for a few small surge-like events, hence, they are hardly observed in daily Hα patrols. According to the characteristics of their Hα structures and spectral properties, we infer these events are small-scale eruptions similar to nano-flares, which may contribute to the mass and energy transported into the corona. Large turbulent velocities of 25–120 km s<SUP>?1</SUP> are responsible for the observed broadenings.展开更多
Prominence plumes are evacuated upflows that emerge from bubbles below prominences,whose formation mechanism is still unclear.Here we present a detailed study of plumes in a quiescent prominence using the high-resolut...Prominence plumes are evacuated upflows that emerge from bubbles below prominences,whose formation mechanism is still unclear.Here we present a detailed study of plumes in a quiescent prominence using the high-resolution Hαfiltergrams at the line center as well as line wing at±0.4 A from the New Vacuum Solar Telescope.Enhancements of brightening,blue shifts,and turbulence at the fronts of plumes are found during their formation.Some large plumes split at their heads and finger-shaped structures are formed between them.Blue-shifted flows along the bubble-prominence interface are found before and during the plume formation.Our observations are consistent with the hypothesis that prominence plumes are related to coupled Kelvin-Helmholtz and Rayleigh-Taylor(KH/RT)instabilities.Plume splittings and fingers are evidence of RT instability,and the flows may increase the growth rate of KH/RT instabilities.However,the significant turbulence at plume fronts may suggest that the RT instability is triggered by the plumes penetrating into the prominence.In this scenario,extra mechanisms are necessary to drive the plumes.展开更多
Pancreatic carcinoma occasionally associated with prominent mucin production and this type of tumor designated as PCM (pancreatic carcinoma with prominent mucin production) was diagnosed depends on subjective estimati...Pancreatic carcinoma occasionally associated with prominent mucin production and this type of tumor designated as PCM (pancreatic carcinoma with prominent mucin production) was diagnosed depends on subjective estimation of the amount of mucous area, and there has been no report on a quantitative evaluation of the amount of mucinous area in the tumor. To examine the feature of PCM, we analyzed 9 cases of PCM among 243 cases of pancreas carcinoma and evaluated the amount of mucin by imaging analysis. Morphologically, 5 cases were classified as intradactal papillary mucinous neoplasms (IPMN)-derived PCM and 4 cases were as ductal adenocarcinoma (DA)-derived PCM. Mucous composition was found to be more than 50% in all IPMN-derived PCM cases, and that was 40% - 50% in DA-derived PCM cases with one exception. IPMN-derived PCM cases showed expansive growth with pancreatic duct dilatation filled with mucin, while DA-derived PCM cases possessed mucin infiltration into interstitial tissue. Immunohisto-chemically, three of 4 DA-derived PCM cases were MUC1(–)/MUC2(+), and the results of expressions for p16 and Dpc4 suggesting that DA-derived PCM was similar to IPMN-derived PCM rather than ordinary DA. Survival rate of DA-derived PCM cases was lower than that of IPMN-derived PCM cases. We advocate that DA-derived PCM may constitute a borderline group between IPMN and ordinary DA.展开更多
We present the results of a study on the north-south asymmetry of solar filaments at low（〈50°） and high（〉60°） latitudes using daily filament numbers from January 1998 to November 2008（solar cycle 23）...We present the results of a study on the north-south asymmetry of solar filaments at low（〈50°） and high（〉60°） latitudes using daily filament numbers from January 1998 to November 2008（solar cycle 23）. It is found that the northern hemisphere is dominant at low latitudes for cycle 23. However, a similar asymmetry does not occur for solar filaments at high latitudes. The present study indicates that the hemispheric asymmetry of solar filaments at high latitudes in a cycle appears to have little connection with that at low latitudes. Our results support that the observed magnetic fields at high latitudes include two components： one comes from the emergence of the magnetic fields from the solar interior and the other comes from the drift of the magnetic activity at low latitudes.展开更多
Prof. WANG Cheng-bai, male, was born in Hunan Province, October 1926. He started working as a physician in 1947, and was assigned to Dalian Medical College for further
We attempt to propose a method for automatically detecting the solar filament chirality and barb beating. We first introduce the concept of an unweighted undirected graph and adopt the Dijkstra shortest path algorithm...We attempt to propose a method for automatically detecting the solar filament chirality and barb beating. We first introduce the concept of an unweighted undirected graph and adopt the Dijkstra shortest path algorithm to recognize the filament spine. Then, we use the polarity inversion line （PIL） shift method for measuring the polarities on both sides of the filament, and employ the connected components labeling method to identify the barbs and calculate the angle between each barb and the spine to determine the bearing of the barbs, i.e., left or right. We test the automatic detection method with Ha filtergrams from the Big Bear Solar Observatory （BBSO） Ha archive and magnetograms observed with the Helioseismic and Magnetic Imager （HMI） on board the Solar Dynamics Observatory （SDO）. Four filaments are automatically detected and illustrated to show the results. The barbs in different parts of a filament may have opposite bearings. The filaments in the southern hemisphere （northern hemisphere） mainly have left-bearing （fight- bearing） barbs and positive （negative） magnetic helicity, respectively. The tested results demonstrate that our method is efficient and effective in detecting the bearing of filament barbs. It is demonstrated that the conventionally believed one-to-one correspondence between filament chirality and barb bearing is not valid. The correct detection of the filament axis chirality should be done by combining both imaging morphology and magnetic field observations.展开更多
Pun,as a figure of speech applied in advertisements,can make the advertisements more vivid and indelible by adding attraction and humor,stimulating consumers' purchasing desire.Based on the elaboration of puns in ...Pun,as a figure of speech applied in advertisements,can make the advertisements more vivid and indelible by adding attraction and humor,stimulating consumers' purchasing desire.Based on the elaboration of puns in English advertisements from the cognitive perspective,this paper attempts to analyze those puns under the guidance of relevant cognitive theoretical framework such as figure/ground theory,prominence view and conceptual blending theory.It also aims to explore the human cognitive activities involved in creation and understanding of advertising language.展开更多
The mean length of the stria vascularis (SV) and the basilar membrane of four normalguinea pigs measured by means of surface preparation was 21.11 mm and 19. 90 mm respectively,and the mean width of their apical turns...The mean length of the stria vascularis (SV) and the basilar membrane of four normalguinea pigs measured by means of surface preparation was 21.11 mm and 19. 90 mm respectively,and the mean width of their apical turns of SV and the turns of the cochlear basis was 0. 44 mmand 0. 86 mm respectively. The ultrastructure of SV, spiral ligament (SL) and spiral prominence(SP) of both ears of eight guinea pigs were observed by scanning electron microscopy(SEM) andtransmission electron microsoopy(TEM). There were a large number of coated vesicles in thesupranuclear region of SV, some opened to the endolymph. A great number of folding cytoplasmicprojections were filled with small vesicles The capillary network was extremely rich indicating thatthe endolymph could be secreted and absorbed by SV. The cellular conjunction in the SV. SL andSP formed an effective barrier. It has not been proved in this study that the melanin offers resistanceto acoustic stimulation.展开更多
文摘GUO Sai-shan was born on October 24, 1938, in Putian Fujian Province, 1960 graduated in Shanghai First Medical College （now Shanghai Medical University）. At present, she is the Professor of Peking Union Medical College. Chief Doctor,Post-doctorate Tutor, in 1991 to 2002 she was appointed as Director of Department of Traditional Chinese Medicine （TOM）;
基金supported by the National Natural Science Foundation of China(NSFC,grant Nos.12303062 and 12203043)the Sichuan Science and Technology Program(2023NSFSC1351,2025ZNSFSC0315)+1 种基金Key Laboratory of Detection and Application of Space Effect in Southwest Sichuan at Leshan Normal University,Education Department of Sichuan Province(No.ZDXM20241002)Project Supported by the Specialized Research Fund for State Key Laboratory of Solar Activity and Space Weather。
文摘Magnetic reconnection driving a two-sided-loop jet is typically associated with interactions between an emerging bipole and the overlying horizontal magnetic field,or between filaments from separate magnetic systems.Leveraging high temporal and spatial resolution observations from ground-based and space-borne instruments,we have identified a two-sided-loop jet originating from magnetic reconnection between threads within a single filament.Our observations show that as two initially crossing filamentary threads within the filament converge,reconnection takes place at their intersection.In the Doppler images,distinct redshift and blueshift signals are observed at the locations where the filament threads intersected.This process generates a two-sided-loop jet with outflow speeds of 22.2 and 62.5 km s^(-1).Following reconnection,the original crossing threads transform into two parallel threads that subsequently separate at speeds of 2.8 and 8.3kms^(-1).This observation offers a new perspective on the mechanisms responsible for jet formation.
基金supported by the National Key R&D Program of China No.2022YFF0503800the Strategic Priority Research Program of the Chinese Academy of Sciences(grant Nos.XDA17040507 and XDB0560000)+1 种基金NSFC grant 11933009the Yunnan Province Scientist Workshop of Solar Physics,the Yunnan Key Laboratory of Solar Physics and Space Science(202205AG070009)。
文摘A 50 mm balloon-borne white-light coronagraph(BBWLC)to observe white-light solar corona over the altitude range from 1.08 R_(⊙)to 1.50 R_(⊙)has recently been indigenously developed by Yunnan Observatories in collaboration with Shandong University(in Weihai)and Changchun Institute of Optics,Fine Mechanics and Physics,which will significantly improve the ability of China to detect and measure the inner corona.On 2022 October 4,its first scientific flight took place at the Dachaidan area in Qinghai province of China.We briefly describe the BBWLC mission including its optical design,mechanical structure,pointing system,the first flight and results associated with the data processing approach.Preliminary analysis of the data shows that BBWLC imaged the K-corona with three streamer structures on the west limb of the Sun.To further confirm the coronal signals obtained by BBWLC,comparisons were made with observations of the K-coronagraph of the High Altitude Observatory and the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory.We conclude that BBWLC eventually observed the white-light corona in its first scientific flight.
文摘The assortedness of Chinese food,together with the complexity of their naming elements,has ignited numerous scholars' interests in this field and prompted them to make abundant analyses of Chinese dish names.Most of them,however,were done in studies of traditional linguistics,rhetoric,translatology and cross-cultural communication.And studies,based on corpus,on the naming elements of Chinese dishes under cognitive linguistic theories almost remain a blank.This paper aims to conduct a quantitative analysis of 4,000 Chinese dish names(500 ones selected freely from each of the eight cuisines),based on the Prominence Principle,in order to identify the specific naming elements of Chinese dishes and forward related statistics and ratios.
基金supported by the National Natural Science Foundation of China(Grant Nos.41761134088,41774150,and 11925302)CAS Key Research Program(Grant No.KZZD-EW-01-4)the fundamental research funds for the central universities,and the Strategic Priority Program of the Chinese Academy of Sciences(Grant No.XDB41000000)。
文摘Magnetic flux ropes are characterized by coherently twisted magnetic field lines,which are ubiquitous in magnetized plasmas.As the core structure of various eruptive phenomena in the solar atmosphere,flux ropes hold the key to understanding the physical mechanisms of solar eruptions,which impact the heliosphere and planetary atmospheres.The strongest disturbances in the Earth’s space environments are often associated with large-scale flux ropes from the Sun colliding with the Earth’s magnetosphere,leading to adverse,sometimes catastrophic,space-weather effects.However,it remains elusive as to how a flux rope forms and evolves toward eruption,and how it is structured and embedded in the ambient field.The present paper addresses these important questions by reviewing current understandings of coronal flux ropes from an observer’s perspective,with an emphasis on their structures and nascent evolution toward solar eruptions,as achieved by combining observations of both remote sensing and in-situ detection with modeling and simulation.This paper highlights an initiation mechanism for coronal mass ejections(CMEs)in which plasmoids in current sheets coalesce into a’seed’flux rope whose subsequent evolution into a CME is consistent with the standard model,thereby bridging the gap between microscale and macroscale dynamics.
基金supported by the National Natural Science Foundation of China(82071096 to X.W,31970585,32170544,and 31801056 to Q.B.)the National Key Research and Development Program of China(2017YFC1001800 to X.W.,2018YFC1004703 to Q.B),the Fundamental research program funding of Ninth People’s Hospital affiliated to Shanghai Jiao Tong University School of Medicine(JYZZ179 to J.S.)+1 种基金the Innovative research team of high-level local universities in Shanghai(SHSMU-ZLCX20211700)the SHIPM-pi fund No.JY201803 from Shanghai Institute of Precision Medicine,Ninth People’s Hospital,Shanghai Jiao Tong University School of Medicine.
文摘During vertebrate embryonic development,neural crest-derived ectomesenchyme within the maxillary prominences undergoes precisely coordinated proliferation and differentiation to give rise to diverse craniofacial structures,such as tooth and palate.However,the transcriptional regulatory networks underpinning such an intricate process have not been fully elucidated.Here,we perform single-cell RNA-Seq to comprehensively characterize the transcriptional dynamics during mouse maxillary development from embryonic day(E)10.5eE14.5.Our single-cell transcriptome atlas of~28,000 cells uncovers mesenchymal cell populations representing distinct differentiating states and reveals their developmental trajectory,suggesting that the segregation of dental from the palatal mesenchyme occurs at E11.5.Moreover,we identify a series of key transcription factors(TFs)associated with mesenchymal fate transitions and deduce the gene regulatory networks directed by these TFs.Collectively,our study provides important resources and insights for achieving a systems-level understanding of craniofacial morphogenesis and abnormality.
基金supported by the National Natural Science Foundation of China(NSFC)under grant numbers 11373066,11373065 and 11203077the Yunnan Science Foundation of China under number 2013FB086+3 种基金the Talent Project of Western Light of Chinese Academy of Sciencesthe National Basic Research Program of China(973 program)under grant number G2011CB811400the Key Laboratory of Solar Activity of CAS under number KLSA 201303,KLSA 201412 and KLSA201407Youth Innovation Promotion Association of CAS(No.2011056)
文摘Study of the small-scale structures and material flows associated with solar quiescent filaments is very important for understanding the formation and equilibrium of solar filaments. Using high resolution Ha data observed by the New Vacuum Solar Telescope, we present the structures of barbs and material flows along the threads across the spine in two quiescent filaments on 2013 September 29 and on 2012 November 2, respectively. During the evolution of the filament barb, several paral- lel tube-shaped structures formed and the width of the structures ranged from about 2.3 Mm to 3.3 Mm. The parallel tube-shaped structures merged together accompanied by material flows from the spine to the barb. Moreover, the boundary between the barb and surrounding atmosphere was very neat. The counter-streaming flows were not found to appear alternately in the adjacent threads of the filament. However, the large-scale patchy counter-streaming flows were detected in the filament. The flows in one patch of the filament have the same direction but flows in the adjacent patch have opposite direction. The patches of two opposite flows with a size of about 10＂ were alternately exhibited along the spine of the filament. The velocity of these material flows ranged from 5.6 km s^-1 to 15.0 km s^-1. The material flows along the threads of the filament did not change their direction for about two hours and fourteen minutes during the evolution of the filament. Our results confirm that the large-scale counter- streaming flows with a certain width along the threads of solar filaments exist and are coaligned well with the threads.
基金Supported by the National Natural Science Foundation of China
文摘High-resolution Ha observations indicate that filaments consist of an as- sembly of thin threads. In quiescent filaments, the threads are generally short, whereas in active region filaments, the threads are generally long. In order to explain these observational features, we performed one-dimensional radiative hydrodynamic sim- ulations of filament formation along a dipped magnetic flux tube in the framework of the chromospheric evaporation-coronal condensation model. The geometry of a dipped magnetic flux tube is characterized by three parameters, i.e., the depth （D）, the half-width （w） and the altitude （h） of the magnetic dip. A survey of the parame- ters in numerical simulations shows that when allowing the filament thread to grow in 5 days, the maximum length （Lth） of the filament thread increases linearly with w, and decreases linearly with D and h. The dependence is fitted into a linear function Lth = 0.84w --0.88D - 2.78h ＋ 17.31 （Mm）. Such a relation can qualitatively explain why quiescent filaments have shorter threads and active region filaments have longer threads.
基金supported by the National Natural Science Foundation of China (41731067 and 41822404)Shenzhen Technology Project (JCYJ20170307150645407)+6 种基金the Fundamental Research Funds for the Central Universities (Grant No. HIT.BRETV.201901)the support by China Postdoctoral Science Foundation (2018M641812)support of the US NSF (AGS-1821294)the National Natural Science Foundation of China (11729301)supported by NJIT and US NSF AGS 1821294 grantpartly supported by the Korea Astronomy and Space Science Institute and Seoul National Universitythe strategic priority research program of Chinese Academy of Science (CAS) (Grant No. XDB09000000)
文摘We observed an Hα surge that occurred in NOAA Active Region 12401 on 2015 August 17, and we discuss its trigger mechanism, and kinematic and thermal properties. It is suggested that this surge was caused by a chromospheric reconnection which ejected cool and dense material with transverse velocity of about 21–28 km s-1 and initial Doppler velocity of 12 km s^-1. This surge is similar to the injection of newly formed filament materials from their footpoints, except that the surge here occurred in a relatively weak magnetic environment of 100 G. Thus, we discuss the possibility of filament material replenishment via the erupting mass in such a weak magnetic field, which is often associated with quiescent filaments. It is found that the local plasma can be heated up to about 1.3 times the original temperature, which results in an acceleration of about –0.017 km s^-2. It can lift the dense material up to 10 Mm and higher with an inclination angle smaller than 50°, namely the typical height of active region filaments, but it can hardly inject the material up to those filaments higher than 25 Mm, like some quiescent filaments. Thus, we think that the injection model does not work well in describing the formation of quiescent filaments.
基金National Natural Science Foundation of China (52275374, 52205414)Xi’an Jiaotong University Basic Research Funds for Freedom of Exploration and Innovation-Student Programs (xzy022023066)+3 种基金Key Research and Development Projects of Shaanxi Province (2023-YBGY-361)Young Elite Scientists Sponsorship Program by CAST (2021QNRC001)State Key Laboratory for Mechanical Behavior of Materials (20212311)Xiaomi Foundation through Xiaomi Young Scholar Program
文摘Mg-Gd-Y-Zr alloy,as a typical magnesium rare-earth(Mg-RE)alloy,is gaining popularity in the advanced equipment manufacturing fields owing to its noticeable age-hardening properties and high specific strength.However,it is extremely challenging to prepare wrought components with large dimensions and complex shapes because of the poor room-temperature processability of Mg-Gd-Y-Zr alloy.Herein,we report a wire-arc directed energy deposited(DED)Mg-10.45Gd-2.27Y-0.52Zr(wt.%,GW102K)alloy with high RE content presenting a prominent combination of strength and ductility,realized by tailored nanoprecipitates through an optimized heat treatment procedure.Specifically,the solution-treated sample exhibits excellent ductility with an elongation(EL)of(14.6±0.1)%,while the aging-treated sample at 200°C for 58 h achieves an ultra-high ultimate tensile strength(UTS)of(371±1.5)MPa.Besides,the aging-treated sample at 250°C for 16 h attains a good strength-ductility synergy with a UTS of(316±2.1)MPa and a EL of(8.5±0.1)%.Particularly,the evolution mechanisms of precipitation response induced by various aging parameters and deformation behavior caused by nanoprecipitates type were also systematically revealed.The excellent ductility resulted from coordinating localized strains facilitated by active slip activity.And the ultra-high strength should be ascribed to the dense nano-β'hampering dislocation motion.Additionally,the shearable nano-β1 contributed to the good strength-ductility synergy.This work thus offers insightful understanding into the nanoprecipitates manipulation and performance tailoring for the wire-arc DED preparation of large-sized Mg-Gd-Y-Zr components with complex geometries.
基金supported by the National Natural Science Foundation of China(NSFC 11533005,11961131002,11733003 and U1731241)supported by the Science and Technology Development Fund of Macao(275/2017/A)。
文摘Solar filaments are an intriguing phenomenon,like cool clouds suspended in the hot corona.Similar structures exist in the intergalactic medium as well.Despite being a long-studied topic,solar filaments have continually attracted intensive attention because of their link to coronal heating,coronal seismology,solar flares and coronal mass ejections(CMEs).In this review paper,by combing through the solar filament-related work done in the past decade,we discuss several controversial topics,such as the fine structures,dynamics,magnetic configurations and helicity of filaments.With high-resolution and highsensitivity observations,combined with numerical simulations,it is expected that resolving these disputes will definitely lead to a huge leap in understanding the physics related to solar filaments,and even shed light on galactic filaments.
基金Support by the National Natural Science Foundation of China.
文摘After surveying the spectra of 39 prominences observed by the Multi-channel Infrared Solar Spectrograph at Purple Mountain Observatory and the 25 cm coronagraph at the Norikura Solar Observatory, we found that about 28% of them show small spatial scale (6''–8'') and short time scale (tens of seconds to a few minutes), unusual large broadening and large shift velocities in spectral lines including Hα, Hβ, H, Ca II H, Ca II K, Ca II 8542?, He I D3 and He I 10830?. We present in detail two typical events observed respectively on 2002 May 27 and 1981 August 2. The full-width at half maximum of the widest profile of the 2001 prominence is 1.8? for Hα and 2.9 ? for He I 10830?, while that of the 1981 prominence is 5.3 ? for Hβ, 3.6 ? for Ca II K, 4.0 ? for Ca II H and 2.8 ? for He I D3. Such broadenings generally occur at a level of several-thousand kilometres above the chromosphere. Further, most of these prominences manifest a rotation of (0.4–1.35)×10<SUP>-2</SUP> rads s<SUP>?1</SUP> pointing to the Sun and large line-of-sight velocities of 20–200 km s<SUP>?1</SUP>. Some of these events correspond in time to an enhancement or a small peak in the GOES X-ray flux, indicating the existence of high energy process at work. These prominences generally display discernible changes in the Hα morphology around the time of large broadening, but do not show Hα brightening or overall eruption except for a few small surge-like events, hence, they are hardly observed in daily Hα patrols. According to the characteristics of their Hα structures and spectral properties, we infer these events are small-scale eruptions similar to nano-flares, which may contribute to the mass and energy transported into the corona. Large turbulent velocities of 25–120 km s<SUP>?1</SUP> are responsible for the observed broadenings.
基金supported by the National Natural Science Foundation of China(NSFC,Grant Nos.11427803,U1731241,U1631242 and 11820101002)by CAS Strategic Pioneer Program on Space Science(Grant Nos.XDA15052200,XDA15320103,XDA15320300 and XDA15320301)+2 种基金the Jiangsu Double Innovation PlanNSFC(Grant No.11873091)Yunnan Province Basic Research Plan(No.2019FA001)。
文摘Prominence plumes are evacuated upflows that emerge from bubbles below prominences,whose formation mechanism is still unclear.Here we present a detailed study of plumes in a quiescent prominence using the high-resolution Hαfiltergrams at the line center as well as line wing at±0.4 A from the New Vacuum Solar Telescope.Enhancements of brightening,blue shifts,and turbulence at the fronts of plumes are found during their formation.Some large plumes split at their heads and finger-shaped structures are formed between them.Blue-shifted flows along the bubble-prominence interface are found before and during the plume formation.Our observations are consistent with the hypothesis that prominence plumes are related to coupled Kelvin-Helmholtz and Rayleigh-Taylor(KH/RT)instabilities.Plume splittings and fingers are evidence of RT instability,and the flows may increase the growth rate of KH/RT instabilities.However,the significant turbulence at plume fronts may suggest that the RT instability is triggered by the plumes penetrating into the prominence.In this scenario,extra mechanisms are necessary to drive the plumes.
文摘Pancreatic carcinoma occasionally associated with prominent mucin production and this type of tumor designated as PCM (pancreatic carcinoma with prominent mucin production) was diagnosed depends on subjective estimation of the amount of mucous area, and there has been no report on a quantitative evaluation of the amount of mucinous area in the tumor. To examine the feature of PCM, we analyzed 9 cases of PCM among 243 cases of pancreas carcinoma and evaluated the amount of mucin by imaging analysis. Morphologically, 5 cases were classified as intradactal papillary mucinous neoplasms (IPMN)-derived PCM and 4 cases were as ductal adenocarcinoma (DA)-derived PCM. Mucous composition was found to be more than 50% in all IPMN-derived PCM cases, and that was 40% - 50% in DA-derived PCM cases with one exception. IPMN-derived PCM cases showed expansive growth with pancreatic duct dilatation filled with mucin, while DA-derived PCM cases possessed mucin infiltration into interstitial tissue. Immunohisto-chemically, three of 4 DA-derived PCM cases were MUC1(–)/MUC2(+), and the results of expressions for p16 and Dpc4 suggesting that DA-derived PCM was similar to IPMN-derived PCM rather than ordinary DA. Survival rate of DA-derived PCM cases was lower than that of IPMN-derived PCM cases. We advocate that DA-derived PCM may constitute a borderline group between IPMN and ordinary DA.
基金Supported by the National Natural Science Foundation of China
文摘We present the results of a study on the north-south asymmetry of solar filaments at low（〈50°） and high（〉60°） latitudes using daily filament numbers from January 1998 to November 2008（solar cycle 23）. It is found that the northern hemisphere is dominant at low latitudes for cycle 23. However, a similar asymmetry does not occur for solar filaments at high latitudes. The present study indicates that the hemispheric asymmetry of solar filaments at high latitudes in a cycle appears to have little connection with that at low latitudes. Our results support that the observed magnetic fields at high latitudes include two components： one comes from the emergence of the magnetic fields from the solar interior and the other comes from the drift of the magnetic activity at low latitudes.
文摘Prof. WANG Cheng-bai, male, was born in Hunan Province, October 1926. He started working as a physician in 1947, and was assigned to Dalian Medical College for further
基金supported by NKBRSF (Grant Nos.2011CB811402 and 2014CB744203)the National Natural Science Foundation of China (Grant Nos.11203014,11533005 and 11025314)the grants from CSC201306190046 and CXZZ130041
文摘We attempt to propose a method for automatically detecting the solar filament chirality and barb beating. We first introduce the concept of an unweighted undirected graph and adopt the Dijkstra shortest path algorithm to recognize the filament spine. Then, we use the polarity inversion line （PIL） shift method for measuring the polarities on both sides of the filament, and employ the connected components labeling method to identify the barbs and calculate the angle between each barb and the spine to determine the bearing of the barbs, i.e., left or right. We test the automatic detection method with Ha filtergrams from the Big Bear Solar Observatory （BBSO） Ha archive and magnetograms observed with the Helioseismic and Magnetic Imager （HMI） on board the Solar Dynamics Observatory （SDO）. Four filaments are automatically detected and illustrated to show the results. The barbs in different parts of a filament may have opposite bearings. The filaments in the southern hemisphere （northern hemisphere） mainly have left-bearing （fight- bearing） barbs and positive （negative） magnetic helicity, respectively. The tested results demonstrate that our method is efficient and effective in detecting the bearing of filament barbs. It is demonstrated that the conventionally believed one-to-one correspondence between filament chirality and barb bearing is not valid. The correct detection of the filament axis chirality should be done by combining both imaging morphology and magnetic field observations.
文摘Pun,as a figure of speech applied in advertisements,can make the advertisements more vivid and indelible by adding attraction and humor,stimulating consumers' purchasing desire.Based on the elaboration of puns in English advertisements from the cognitive perspective,this paper attempts to analyze those puns under the guidance of relevant cognitive theoretical framework such as figure/ground theory,prominence view and conceptual blending theory.It also aims to explore the human cognitive activities involved in creation and understanding of advertising language.
文摘The mean length of the stria vascularis (SV) and the basilar membrane of four normalguinea pigs measured by means of surface preparation was 21.11 mm and 19. 90 mm respectively,and the mean width of their apical turns of SV and the turns of the cochlear basis was 0. 44 mmand 0. 86 mm respectively. The ultrastructure of SV, spiral ligament (SL) and spiral prominence(SP) of both ears of eight guinea pigs were observed by scanning electron microscopy(SEM) andtransmission electron microsoopy(TEM). There were a large number of coated vesicles in thesupranuclear region of SV, some opened to the endolymph. A great number of folding cytoplasmicprojections were filled with small vesicles The capillary network was extremely rich indicating thatthe endolymph could be secreted and absorbed by SV. The cellular conjunction in the SV. SL andSP formed an effective barrier. It has not been proved in this study that the melanin offers resistanceto acoustic stimulation.
