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An intense solar energetic particle (SEP) event was observed on 2021 October 9 by multiple spacecraft distributed near the ecliptic plane at heliocentric radial distances R ≲ 1 au and within a narrow range of heliolongitudes. A stream interaction region (SIR), sequentially observed by Parker Solar Probe (PSP) at R = 0.76 au and 48° east from Earth (ϕ = E48°), STEREO-A (at R = 0.96 au, ϕ = E39°), Solar Orbiter (SolO; at R = 0.68 au, ϕ = E15°), BepiColombo (at R = 0.33 au, ϕ = W02°), and near-Earth spacecraft, regulated the observed intensity-time profiles and the anisotropic character of the SEP event. PSP, STEREO-A, and SolO detected strong anisotropies at the onset of the SEP event, which resulted from the fact that PSP and STEREO-A were in the declining-speed region of the solar wind stream responsible for the SIR and from the passage of a steady magnetic field structure by SolO during the onset of the event. By contrast, the intensity-time profiles observed near Earth displayed a delayed onset at proton energies ≳13 MeV and an accumulation of ≲5 MeV protons between the SIR and the shock driven by the parent coronal mass ejection (CME). Even though BepiColombo, STEREO-A, and SolO were nominally connected to the same region of the Sun, the intensity-time profiles at BepiColombo resemble those observed near Earth, with the bulk of low-energy ions also confined between the SIR and the CME-driven shock. This event exemplifies the impact that intervening large-scale interplanetary structures, such as corotating SIRs, have in shaping the properties of SEP events., Solar Orbiter is a space mission of international collaboration between ESA and NASA, operated by ESA. The STEREO SECCHI data are produced by a consortium of RAL (UK), NRL (USA), LMSAL (USA), GSFC (USA), MPS (Germany), CSL (Belgium), IOTA (France), and IAS (France). SOHO is a mission of international cooperation between ESA and NASA. The SDO/AIA data are provided by the Joint Science Operations Center (JSOC) Science Data Processing (SDP). Parker Solar Probe was designed, built, and is now operated by the Johns Hopkins University Applied Physics Laboratory as part of NASA's LWS program (contract NNN06AA01C). We thank the German Federal Ministry for Economic Affairs and Energy and the German Space Agency (Deutsches Zentrum für Luft- und Raumfahrt, e.V., (DLR)) for their unwavering support of STEP, EPT, and HET under grants Nos. 50OT0901, 50OT1202, 50OT1702, and 50OT2002. N.W. acknowledges funding from the Research Foundation—Flanders (FWO–Vlaanderen, fellowship No. 1184319N). This project has received funding from the European Union's Horizon 2020 research and innovation programs under grant agreement No. 870405 (EUHFORIA 2.0). These results were also obtained in the framework of the ESA project "Heliospheric modeling techniques" (contract No. 4000133080/20/NL/CRS) and the projects C14/19/089 (C1 project Internal Funds KU Leuven), G.0D07.19N (FWO–Vlaanderen), SIDC Data Exploitation (ESA Prodex-12), and Belspo project B2/191/P1/SWiM. E.P. acknowledges support from NASA's PSP-GI (grant No. 80NSSC22K0349) and O2R (grant No. 80NSSC20K0285) programs. B.S.-C. acknowledges support through UK-STFC Ernest Rutherford Fellowship ST/V004115/1 and STFC grants ST/W00089X/1 and ST/V000209/1. R.G.H. acknowledges the financial support by the Spanish MICIU (project PID2019-104863RB-I00/AEI/10.13039/501100011033). R.V. and N.D. acknowledge funding from the European Union's Horizon 2020 research and innovation program under grant agreement No. 101004159 (SERPENTINE). N.D. also acknowledges support from the Turku Collegium for Science, Medicine and Technology of the University of Turku, Finland. A.A. acknowledges the support by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019-105510GB-C31 and through the "Centre of Excellence María de Maeztu 2020-2023" award to the ICCUB (CEX2019-000918-M). D.L. and I.G.R. acknowledge support from NASA Living With a Star (LWS) programs NNH17ZDA001N-LWS and NNH19ZDA001N-LWS, the Goddard Space Flight Center Internal Scientist Funding Model (competitive work package) program, and the Heliophysics Innovation Fund (HIF) program. I.G.R. also acknowledges support from the ACE mission. The data used in this paper can be downloaded from spdf.gsfc.nasa.gov, www.srl.caltech.edu/ACE/ASC/, soar.esac.esa.int/soar/, stereo.gsfc.nasa.gov, gong.nso.edu/data/magmap/, sdo.gsfc.nasa.gov/data/aiahmi/. See also 10.48322/7gr7-1791, 10.48322/97te-0132, 10.48322/wpk2-yq48, and 10.48322/c0zj-xf76. BepiColombo data used in Figures 11 and 12 can be downloaded from 10.25392/leicester.data.19447259.v1.

To summarize the clinical experience of sandwich-shaped resection and cheiloplasty in the treatment of macrocheilia secondary to arteriovenous malformation, and to observe its clinical efficacy and complications. The clinical data of 27 patients with macrocheilia secondary to arteriovenous malformation who received surgical treatment from January 2018 to October 2020 in Linyi Cancer Hospital were retrospectively analyzed. There were 14 males and 13 females. The median age was 4.5 years (ranged from 2 to 57 years). There were 18 cases of upper lip and 9 cases of lower lip. All patients had received interventional embolization sclerotherapy for 5 to 10 times before surgery with unsatisfied effect. There was no obvious improvement in the appearance,whereas 3 cases progressed presenting as abnormal enlargement. Sandwich-shaped resection and cheiloplasty was performed in all the patients. Histopathological examinations confirmed arteriovenous malformations in all 27 cases. Twenty-six patients received one course of operation and one received two courses. Partial mucosal necrosis occurred in 1 case and healed after dressing change, while the rest healed by first intention. Local recurrence occurred in 2 cases within 6 months after operation. A four-level standard was used for long-term evaluation, and 24 cases got grade Ⅲ (good), three cases got grade Ⅱ (moderate) after 1 to 3 years of follow-up. Sandwich-shaped resection and cheiloplasty can achieve good long-term efficacy with excellent appearance and function. Due to its advantages of hidden incision and three-dimensional resection and reservation, it is worthy of further clinical promotion.总结“三明治”式唇病变切除成形术治疗动静脉畸形巨唇症的临床经验，观察其临床疗效和并发症。回顾性分析2018年1月至2020年10月在临沂市肿瘤医院接受手术治疗的27例动静脉畸形巨唇症患者的临床资料，其中男14例，女13例；中位年龄4.5岁（2~57岁）；上唇18例，下唇9例。所有患者在手术前均接受过（外院或本院）5~10次的介入栓塞硬化治疗，巨唇外形改善均不明显，3例病变进展增大。本组病例均采用“三明治”式唇病变切除成形术治疗。共行“三明治”式唇病变切除成形术28例次（1例2次手术）。27例次患者一期切口愈合，1例部分黏膜坏死，后经换药后愈合。有2例分别于术后半年内局部复发。随访1~3年，远期疗效评价Ⅲ级（好）24例，Ⅱ级（中）3例，Ⅰ级（差）0例。“三明治”式唇病变切除成形术切口隐蔽，立体式切除病变彻底，能最大限度保留三维结构，术后外形和功能良好，远期疗效好，建议临床推广该手术方式。.

We investigate the waiting time statistics of solar flares both in a flare-productive active region (AR 12673) of the solar cycle 24 and in a three-dimensional magnetohydrodynamic (MHD) simulated AR. The statistical models of a discrete random process and a continuous memory-dependent process are applied to interpret the waiting time distributions (WTDs) of solar flares. Our results indicate that the occurrence of a solar flare in an individual AR maintains a certain amount of memory, and probably arises from MHD turbulence rather than from intermittent avalanches in a self-organized criticality system. It differs from the occurrence of ‘super flares’ when treating the star/Sun as a single non-linear system.

The origin of 3He abundance enhancements in coronal mass ejection (CME)-driven shock gradual solar energetic particle (SEP) events remains largely unexplained. Two mechanisms have been suggested - the re-acceleration of remnant flare material in interplanetary space and concomitant activity in the corona. We explore the first gradual SEP event with enhanced 3He abundance observed by Solar Orbiter. The event started on 2020 November 24 and was associated with a relatively fast halo CME. During the event, the spacecraft was at 0.9 au from the Sun. The event averaged 3He/4He abundance ratio is 24 times higher than the coronal or solar wind value, and the 3He intensity had timing similar to other species. We inspected available imaging, radio observations, and spacecraft magnetic connection to the CME source. It appears the most probable cause of the enhanced 3He abundance are residual 3He ions remaining from a preceding long period of 3He-rich SEPs on 2020 November 17-23., Comment: 9 pages, 9 figures, accepted for publication in A&A

Kollhoff, A., et al., Context. On 2020 November 29, the first widespread solar energetic particle (SEP) event of solar cycle 25 was observed at four widely separated locations in the inner (≲ 1 AU) heliosphere. Relativistic electrons as well as protons with energies > 50 MeV were observed by Solar Orbiter (SolO), Parker Solar Probe, the Solar Terrestrial Relations Observatory (STEREO)-A and multiple near-Earth spacecraft. The SEP event was associated with an M4.4 class X-ray flare and accompanied by a coronal mass ejection and an extreme ultraviolet (EUV) wave as well as a type II radio burst and multiple type III radio bursts. Aims. We present multi-spacecraft particle observations and place them in context with source observations from remote sensing instruments and discuss how such observations may further our understanding of particle acceleration and transport in this widespread event. Methods. Velocity dispersion analysis (VDA) and time shift analysis (TSA) were used to infer the particle release times at the Sun. Solar wind plasma and magnetic field measurements were examined to identify structures that influence the properties of the energetic particles such as their intensity. Pitch angle distributions and first-order anisotropies were analyzed in order to characterize the particle propagation in the interplanetary medium. Results. We find that during the 2020 November 29 SEP event, particles spread over more than 230° in longitude close to 1 AU. The particle onset delays observed at the different spacecraft are larger as the flare-footpoint angle increases and are consistent with those from previous STEREO observations. Comparing the timing when the EUV wave intersects the estimated magnetic footpoints of each spacecraft with particle release times from TSA and VDA, we conclude that a simple scenario where the particle release is only determined by the EUV wave propagation is unlikely for this event. Observations of anisotropic particle distributions at SolO, Wind, and STEREO-A do not rule out that particles are injected over a wide longitudinal range close to the Sun. However, the low values of the first-order anisotropy observed by near-Earth spacecraft suggest that diffusive propagation processes are likely involved., The CAU Kiel team acknowledges support from the German Federal Ministry for Economic Affairs and Energy, the German Space Agency (Deutsches Zentrum für Luft- und Raumfahrt e.V., DLR) under grants 50OT0901, 50OT1202, 50OT1702, and 50OT2002. A.K. acknowledges financial support from the ANR COROSHOCK project (ANR-17-CE31-0006-01). D.L. acknowledges support from NASA-HGI grant NNX16AF73G and the NASA Program NNH17ZDA001N-LWS. This study has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 101004159 (SERPENTINE). The U. Turku team acknowledges funding by the Academy of Finland (Grant No. 336809). The UAH team acknowledges financial support by the Spanish Ministerio de Ciencia, Innovación y Universidades FEDER/MCIU/AEI Projects ESP2017-88436-R and PID2019-104863RB-I00/AEI/10.13039/501100011033. [...] The Swedish National Space Agency, ESA-PRODEX and all the participating institutes. I.G.R. acknowledges support from NASA programs NNH19ZDA001N-HSR and NNH19ZDA001N-LWS, and the STEREO mission. IRFU team acknowledges support from the Swedish National Space Agency grant 20/136. A.A. acknowledges the support of the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019- 105510GB-C31 and through the ‘Center of Excellence María de Maeztu 2020-2023’ award to the ICCUB (CEX2019-000918- M). F.C. acknowledges the financial support by the Spanish MINECO-FPI-2016 predoctoral grant with FSE. E.A. would like to acknowledge the financial support by the Academy of Finland (Postdoctoral Grant No 322455). V.K. acknowledges the support by NASA under grants 18-2HSWO218_2-0010 and 19-HSR-19_2-0143. Solar Orbiter magnetometer operations are funded by the UK Space Agency (grant ST/T001062/1). T.S.H. is supported by STFC grant ST/S000364/1. T.L. and S.D. acknowledge support from the UK Science and Technology Facilities Council (STFC; grant ST/R000425/1).

Wimmer-Schweingruber, R. F., et al., [Context] Solar Orbiter strives to unveil how the Sun controls and shapes the heliosphere and fills it with energetic particle radiation. To this end, its Energetic Particle Detector (EPD) has now been in operation, providing excellent data, for just over a year. [Aims] EPD measures suprathermal and energetic particles in the energy range from a few keV up to (near-) relativistic energies (few MeV for electrons and about 500 MeV nuc-1 for ions). We present an overview of the initial results from the first year of operations and we provide a first assessment of issues and limitations. In addition, we present areas where EPD excels and provides opportunities for significant scientific progress in understanding how our Sun shapes the heliosphere. [Methods] We used the solar particle events observed by Solar Orbiter on 21 July and between 10 and 11 December 2020 to discuss the capabilities, along with updates and open issues related to EPD on Solar Orbiter. We also give some words of caution and caveats related to the use of EPD-derived data. [Results] During this first year of operations of the Solar Orbiter mission, EPD has recorded several particle events at distances between 0.5 and 1 au from the Sun. We present dynamic and time-averaged energy spectra for ions that were measured with a combination of all four EPD sensors, namely: the SupraThermal Electron and Proton sensor (STEP), the Electron Proton Telescope (EPT), the Suprathermal Ion Spectrograph (SIS), and the High-Energy Telescope (HET) as well as the associated energy spectra for electrons measured with STEP and EPT. We illustrate the capabilities of the EPD suite using the 10 and 11 December 2020 solar particle event. This event showed an enrichment of heavy ions as well as 3He, for which we also present dynamic spectra measured with SIS. The high anisotropy of electrons at the onset of the event and its temporal evolution is also shown using data from these sensors. We discuss the ongoing in-flight calibration and a few open instrumental issues using data from the 21 July and the 10 and 11 December 2020 events and give guidelines and examples for the usage of the EPD data. We explain how spacecraft operations may affect EPD data and we present a list of such time periods in the appendix. A list of the most significant particle enhancements as observed by EPT during this first year is also provided., We acknowledge the Spanish Ministerio de Ciencia, Innovación y Universidades for their invaluable support on the development of the EPD suite and the ICU under grants FEDER/MCIU – Agencia Estatal de Investigación/Projects ESP2015-68266-R, ESP2017-88436-R and PID2019-104863RB-I00/AEI/10.13039/501100011033. We also thank acknowledge the financial support by the Spanish MINECO-FPI-2016 predoctoral grant with FSE. We thank the German Federal Ministry for Economic Affairs and Energy and the German Space Agency (Deutsches Zentrum für Luft- und Raumfahrt, e.V., (DLR)) for their unwavering support of STEP, EPT, and HET under grants numbers 50OT0901, 50OT1202, 50OT1702, and 50OT2002; and ESA for supporting the build of SIS under contract number SOL.ASTR.CON.00004, as well as the University of Kiel and the Land Schleswig-Holstein for their support of SIS. We thank NASA headquarters and the GSFC Solar Orbiter project office for support of SIS at APL under contract NNN06AA01C. A.A. acknowledges the support by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019- 105510GB-C31 and through the ‘Center of Excellence María de Maeztu 2020-2023’ award to the ICCUB (CEX2019-000918- M). Solar Orbiter magnetometer operations are funded by the UK Space Agency (grant ST/T001062/1). Tim Horbury is supported by STFC grant ST/S000364/1. We acknowledge funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No. 101004159 (SERPENTINE).

Aran, A., et al., [Context] In mid-June 2020, the Solar Orbiter (SolO) mission reached its first perihelion at 0.51 au and started its cruise phase, with most of the in situ instruments operating continuously. [Aims] We present the in situ particle measurements of the first proton event observed after the first perihelion obtained by the Energetic Particle Detector (EPD) suite on board SolO. The potential solar and interplanetary (IP) sources of these particles are investigated. Methods. Ion observations from ∼20 keV to ∼1 MeV are combined with available solar wind data from the Radio and Plasma Waves (RPW) instrument and magnetic field data from the magnetometer on board SolO to evaluate the energetic particle transport conditions and infer the possible acceleration mechanisms through which particles gain energy. We compare > 17-20 MeV ion count rate measurements for two solar rotations, along with the solar wind plasma data available from the Solar Wind Analyser (SWA) and RPW instruments, in order to infer the origin of the observed galactic cosmic ray (GCR) depressions. [Results] The lack of an observed electron event and of velocity dispersion at various low-energy ion channels and the observed IP structure indicate a local IP source for the low-energy particles. From the analysis of the anisotropy of particle intensities, we conclude that the low-energy ions were most likely accelerated via a local second-order Fermi process. The observed GCR decrease on 19 June, together with the 51.8-1034.0 keV nuc-1 ion enhancement, was due to a solar wind stream interaction region (SIR). The observation of a similar GCR decrease in the next solar rotation favours this interpretation and constitutes the first observation of a recurrent GCR decrease by SolO. The analysis of the recurrence times of this SIR suggests that it is the same SIR responsible for the He events previously measured in April and May. Finally, we point out that an IP structure more complex than a common SIR cannot be discarded, mainly due to the lack of solar wind temperature measurements and the lack of a higher cadence of solar wind velocity observations., EPD was built with funding from Ministerio de Ciencia e Innovación (Spain), Deutsches Zentrum für Luft- und Raumfahrt (Germany), and the European Space Agency (ESA); operations are funded by FEDER/MCI/AEI Projects ESP2017-88436-R and PID2019-104863RBI00/AEI/10.13039/501100011033 (Spain), 50OT 2002 (DLR, Germany), and NASA contract 80MSFC19F0002. The UB team acknowledges the support by the Spanish Ministerio de Ciencia e Innovación (MICINN) under grant PID2019-105510GB-C31 and through the “Center of Excellence María de Maeztu 2020-2023” award to the ICCUB (CEX2019-000918-M). The CAU Kiel team acknowledges support by the German Federal Ministry for Economic Affairs and Energy, the German Space Agency (Deutsches Zentrum für Luft- und Raumfahrt e.V., DLR) under grants 50OT0901, 50OT1202, 50OT1702, 50OT2002, and 50OC1702. The Solar Orbiter magnetometer was funded by the UK Space Agency (grant ST/T001062/1). M.L. and S.B. acknowledge financial support by the Italian MIUR-PRIN grant 2017APKP7T on Circumterrestrial Environment: Impact of Sun-Earth Interaction. N.W. acknowledges funding from the Research Foundation – Flanders (FWO – Vlaanderen, fellowship no. 1184319N). D.L. acknowledges the support from the NASA-HGI grant NNX16AF73G and the NASA Programs NNH17ZDA001N-LWS. I.G.R. and D.L. acknowledge support from NASA program NNH19ZDA001N-LWS. E.S. was supported by a PhD grant awarded by the Royal Observatory of Belgium. V.K. acknowledges the support by NASA under grants 18-2HSWO218_2-0010 and 19-HSR-19_2-0143. S.P. is supported by the projects C14/19/089 (C1 project Internal Funds KU Leuven), G.0D07.19N (FWO-Vlaanderen), SIDEX (ESA Prodex-12), and EUHFORIA 2.0 (funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 870405). IRFU team acknowledges support from the Swedish National Space Agency grant 20/136. F.C. acknowledges the financial support by the Spanish MINECO-FPI-2016 predoctoral grant with FSE. The JHU/APL team is supported under NASA contract NNN06AA01C and thanks NASA headquarters and the NASA/GSFC Solar Orbiter project office for their continuing support. Solar Orbiter Solar Wind Analyser (SWA) data are derived from scientific sensors which have been designed and created, and are operated under funding provided in numerous contracts from the UK Space Agency (UKSA, most recently grant ST/T001356/1), the UK Science and Technology Facilities Council (STFC), the Agenzia Spaziale Italiana (ASI), the Centre National d’Etudes Spatiales (CNES, France), the Centre National de la Recherche Scientifique (CNRS, France), the Czech contribution to the ESA PRODEX programme and NASA.

The liquid metal cooling (LMC) process has attracted increasing attention in the investment casting industry in recent years. Liquid Sn is generally used as the cooling medium in state-of-the-art LMC processes even though Sn is known to be a detrimental element in Ni-based superalloys. Therefore, Sn contamination in superalloys has become one of the top concerns for the LMC process. In this work, the reaction between liquid Sn and a Ni-based superalloy was investigated. The detectable reaction between superalloy and liquid Sn began at approximately 500 °C, and the reaction products became complex with increasing temperature. At high temperatures beyond 750 °C, a very short contact period of less than 1 minute led to a severe surface reaction. The results were compared to the surface reaction zone of the large blade. The critical time when the superalloy casting contacted liquid Sn is obtained based on experimental observations and numerical simulations. The surface reaction will occur if the ceramic mold cracked at this point or previously. The surface contamination during LMC solidification is associated with the volume of the casting. The present results indicate that surface reaction would be avoided if the volume of the large blade is reduced to ~ 30 pct of the original size.

Context.Following a multi-year minimum of solar activity, a solar energetic particle event on 2020 Nov. 29 was observed by multiple spacecraft covering a wide range of solar longitudes including ACE, the Solar Terrestrial Relations Observatory-A, and the recently launched Parker Solar Probe and Solar Orbiter.Aims.Multi-point observations of a solar particle event, combined with remote-sensing imaging of flaring, shocks, and coronal mass ejections allows for a global picture of the event to be synthesized, and made available to the modeling community to test, constrain, and refine models of particle acceleration and transport according to such parameters as shock geometries and particle mass-to-charge ratios.Methods.Detailed measurements of heavy ion intensities, time dependence, fluences, and spectral slopes provided the required test data for this study.Results.The heavy ion abundances, timing, and spectral forms for this event fall well within the range found in prior surveys at 1 au. The spectra were well fitted by broken power law shapes; the Fe/O ratio was somewhat lower than the average of other events. In addition,3He/4He was very low, with only the upper limits established here.

The Solar Orbiter flyby of Venus on 27 December 2020 allowed for an opportunity to measure the suprathermal to energetic ions in the Venusian system over a large range of radial distances to better understand the acceleration processes within the system and provide a characterization of galactic cosmic rays near the planet. Bursty suprathermal ion enhancements (up to ∼10 keV) were observed as far as ∼50RVdowntail. These enhancements are likely related to a combination of acceleration mechanisms in regions of strong turbulence, current sheet crossings, and boundary layer crossings, with a possible instance of ion heating due to ion cyclotron waves within the Venusian tail. Upstream of the planet, suprathermal ions are observed that might be related to pick-up acceleration of photoionized exospheric populations as far as 5RVupstream in the solar wind as has been observed before by missions such as Pioneer Venus Orbiter and Venus Express. Near the closest approach of Solar Orbiter, the Galactic cosmic ray (GCR) count rate was observed to decrease by approximately 5 percent, which is consistent with the amount of sky obscured by the planet, suggesting a negligible abundance of GCR albedo particles at over 2RV. Along with modulation of the GCR population very close to Venus, the Solar Orbiter observations show that the Venusian system, even far from the planet, can be an effective accelerator of ions up to ∼30 keV. This paper is part of a series of the first papers from the Solar Orbiter Venus flyby.

Context. The Solar Orbiter spacecraft cruised in the inner heliosphere during Feb. 2020 – Jan. 2021, moving between ∼0.5–1.0 au radial distance. The Energetic Particle Detector suite operated continuously during this period. Aims. The Suprathermal Ion Spectrograph and High Energy Telescope observations made during intervals in between transient intensity increases were used to determine the low energy ion spectra and composition during quiet times. Methods. Energetic particle spectra and major ion components, including 3He, were measured over the range ∼0.1–100 MeV nucleon−1. The radial dependence of 4.4 MeV nucleon−1 4He and O was measured. A short interval of extremely low intensities (“super-quiet”) was also studied. Results. Spectra measured during the quiet period showed transitions, including galactic cosmic rays (> 50 MeV nucleon−1), anomalous cosmic rays (a few to ∼50 MeV nucleon−1), and a steeply rising “turn-up” spectrum below a few MeV nucleon−1 whose composition resembled impulsive, 3He-rich solar energetic particle events. The radial dependence had large uncertainties but was consistent with a small gradient. During the super-quiet interval, the higher energy components remained similar to the quiet period, while the approximately flat low energy 4He spectrum extended downward, reaching ∼300 keV nucleon−1 before transitioning to a steeply rising spectrum.

Background and Aims In southern China, where the solar radiation is insufficient for optimised grapevine growth, supplemental light sources are being used. The aim of the present study was to assess the practicability of light-emitting diode (LED) light as a supplemental light source to improve grape photosynthesis and berry composition. Methods and Results The leaf abaxial surface (Ab) of cv. Summer Black grapevines was illuminated by red, blue and compound LED light strips. In most cases, the net photosynthetic rate (Pn) of the light-treated plants was typically higher than that of the untreated Control (CK) on sunny and rainy days in all stages. Blue light promoted the Pn of the leaf adaxial surface (Ad), whereas red light promoted the Pn of Ab, and the effect of compound light was moderate. The light response curve on the Ad showed that blue and compound light can facilitate the use of high light by the grape leaf. The CO2 response curve indicated that leaves supplemented with blue light have a significantly advantageous CO2 assimilation. Grapes supplemented with compound and red light had a berry mass higher than that of the Control, whereas grapes supplemented with blue and compound light had improved berry composition. Conclusions Blue and compound LED irradiation increased leaf photosynthetic capacity and improved fruit composition, whereas red and compound LED irradiation increased berry mass. Significance of the Study The supplemental LED lights significantly optimised the light environment and improved photosynthesis and the composition of grape in southern China.

The aim of this study was to explore a panel of useful markers in differential diagnosis of primary endocervical adenocarcinoma (ECA) and endometrial adenocarcinoma (EMA). Materials anid Methods: Thirty-three ECAs and 31 EMAs were collected and examined for high-risk human papillomavirus (hr-HPV) (16/18) DNA using in situ hybridization, and for p16, vimentin, ER, PR expression using immunohistochemistry (IHC).Detection rate of hr-HPV (16/18) DNA in ECA (72.7%, 24/33) was significantly higher than that in EMA (12.9%, 4/31) (p0.01). Twenty-four of 33 (72.7%) cases of ECA, but only five of 31 (16.1%) cases of EMA showed high expression of pl6. Twenty-three of 24 (95.8%) hr-HPV DNA-positive ECA and all four (100.0%) hr-HPV DNA-positive EMA showed high levels of pl6 expression. High expression rates of vimentin (90.3%, 28/31), ER (58.1%, 18/31), and PR (71.0%, 22/31) in EMA were significantly higher than those in ECA, respectively (p0.01).Detection of hr-HPV DNA combined with immunohistochemical expressions of pl6, vimentin, ER, and PR have important value in differential diagnosis between ECA and EMA.

Stainless steel fiber felts are important porous stainless steel products for a variety of industry applications. A systematic study of the sintering of 28-µm stainless steel fibers has been conducted for the first time, assisted with synchrotron radiation experiments to understand the evolution of the sintered joints. The critical sintering conditions for the formation of bamboo-like grain structures in the fiber ligaments were identified. The evolution of the number density of the sintered joints and the average sintered neck radius during sintering was assessed based on synchrotron radiation experiments. The optimum sintering condition for the fabrication of high strength and ductile 28-µm-diameter stainless steel fiber felts was determined to be sintering at 1000°C for 900 s. Sintering under this optimum condition increased the tensile strength of the as-sintered stainless steel fiber felts by 50% compared to conventional sintering (1200°C for 7200 s), in addition to much reduced sintering cycle and energy consumption.

B4Cp/2024Al composite with volume fraction of 45% was designed and fabricated by pressure infiltration technology. Microstructure and friction and wear properties of B4Cp/2024Al composites were studied. The results show that reinforcement particles are uniformly distributed and a qualified relative density of the composite has been achieved. A high density of dislocations was observed to be in the peripheral area of the reinforcement particles, and a large number of fine acicular precipitates were found. Coefficient of friction of B4Cp/2024Al composites decreased slightly with increasing load and sliding speed, meanwhile, the wear rate increased with increasing load and sliding speed. Main forms of wear in B4Cp/2024Al composites were abrasive wear, adhesive wear and oxidation wear.

To evaluate the relationship between different RET mutations and the aggressiveness of hereditary medullary thyroid cancer (HMTC) or the presentation of other endocrine disorders in patients with multiple endocrine neoplasia type 2 (MEN2).A total of 73 thyroid medullary carcinoma patients from 22 Chinese kindreds who were treated in our center from 2010 to 2015 were enrolled. RET genes in the patients and their relatives were screened.According to the clinical data and 2015 American Thyroid Association (ATA) guidelines, patients were classified into 3 RET mutation risk groups: Modest, 24 cases; High, 48 cases; and Highest, 1 case. Multivariate analysis showed an increased likelihood of MTC stage III or IV at diagnosis with increasing of age and risk. The likelihood increased 11.6% per year of age at surgery (95% confidence interval, 1.040-1.198; P=0.002). The likelihood in patients with high risk was 7.9 times higher than patients with modest risk (95% confidence interval, 1.607-38.717; P=0.003). Aside from one patient with MEN2B, other 72 patients were MEN2A, of them, 28 cases from 7 kindreds with classical MEN2A (codon 634618), 14 cases from 3 kindreds with cutaneous lichen amyloidosis (codon 634), 4 cases from 1 kindred with Hirschsprung's disease (codon 620), and 26 cases from 10 kindreds with familial MTC.The aggressiveness of HMTC and the presentation of other endocrine diseases are related to specific RET mutations. For RET mutation carriers, MTC and other endocrine diseases should be diagnosed and treated early based on the RET genotypes.

Fragment yields of projectile fragmentation reactions using primary beams of 36,40Ar at 50 MeV/nucleon on 64 Ni target have been measured. Fragment yields of different isotopes were obtained for Z ≥ 5 in RIBLL fragment seperator. We compare the extracted yields to the predictions of the empirical parametrization of fragmentation cross-sections(EPAX) and Statistical Abration-Ablation model(SAA) considering the RIBLL separator transmission rate. Isotope yield ratios between these 2 reactions were calculated, isoscaling parameters α and β, their dependence on fragment atomic number Z and neutron number N were calculated.

To systematically evaluate the security of hormone replacement therapy (HRT) among postoperative patients with endometrial carcinoma (EC).A systematic review and Meta-analysis of studies on security of HRT among EC patients after operation was done by Revman 5.2 software. Studies were mainly searched from the CENTRAL, Medline, Embase, Ovid, Wanfang, CNKI databases.A total of 7 studies with 2 038 stageⅠand stageⅡ endometrial carcinoma patients were included. The quality of 6 studies included were medium, and 1 study was high. The endometrial carcinoma patients on HRT did not have a statistically increased incidence in the EC recurrence (RR=0.69, 95%CI (0.42-1.15), P=0.16) and cancer-induced death (RR=0.55, 95%CI (0.25-1.21), P=0.14). Subgroup analysis for the start of HRT within 6 months from time of surgery group and only estrogen replacement therapy group found no statistical different in the risk of the EC recurrence and cancer-induced death, compared with control group. No statistically increased risk of the EC recurrence was observed for estrogen plus progestin replacement therapy group.There is no statistical difference in the recurrence rate and cancer-induced death rate of EC whether the early stage postoperative patients used HRT or not.

High speed countercurrent chromatography was used for enantioseparation of chlorpheniramine. The separation was performed with a two‐phase system composed of ethyl acetate∶methanol∶water (10∶1∶9) within 2 hours in a tail‐to‐head elution mode. The lower phase contained 20 mmol/L of carboxymethly‐β‐cyclodextrin as a chiral selector. The enantiomers separated were identified by chiral HPLC, which confirmed that this method was very useful for the chiral preparative separation.

The Substance-field analysis is put forward. The functional analysis method is studied to find out the problem, and an improved algorithm is put forward. The internal combustion engine is taken as an example, the harmful function is recognized, and is improved, i.e, high pressure gas is introduced to remove polluted air. The working principle of pneumatic engine is described, the thermodynamic engineering is analyzed, the energy release amounts are analyzed in the isothermal, polymorphism and adiabatic processes. It is concluded that, the isothermal process releases the most energy than the others. The expansion process of the pneumatic engine should be as close as possible to the isothermal process.

In engineering practice, engineer needs to carry out complicated calculation when the loads on the beam are complex. The processes of analysis and calculation take a lot of time and the results are unreliable. So VS2005 and ADK are used to develop a software for beams design based on the 3D CAD software SINOVATION with C ++ programming language. The software can realize the mechanical analysis and parameterized design of various types of beams and output the report of design in HTML format. Efficiency and reliability of design of beams are improved.