1,929 research outputs found
Periacma ziyangensis Wang & Zheng 1995
No full textPeriacma ziyangensis Wang & Zheng, 1995 (Figure 9) Periacma ziyangensis Wang & Zheng, 1995: 7. Wing expanse: 15.0–17.0 mm. Material examined: Holotype: „, Ziyang (32 ° 33 9 N, 108 ° 32 9 E), Shaanxi Province, 350 m, 21 May 1994, coll. Jin Zhou. Allotype: ♀, 22 May 1994, same location data as holotype. Additional material: 1 „, 3 ♀♀, Ziyang, Shaanxi Province, 7 June 1973, coll. Feng Yuan and Chou Tian; 1 „, Ankang (32 ° 41 9 N, 109 ° 01 9 E), Shaanxi Province, 800 m, 5 July 2003, coll. Haili Yu; 10 „„, 11 ♀♀, Mt. Emei (29 ° 32 9 N, 103 ° 19 9 E), Sichuan Province, 24 May– 12 June 1979; 46 „„, 18 ♀♀, Chishui (28 ° 34 9 N, 105 ° 42 9 E), Guizhou Province, 390–500 m, 27–31 May 2000, coll. Yanli Du. Distribution: China (Beijing, Heilongjiang, Guizhou, Shaanxi, Sichuan) Remarks: This species is characterized by the gnathos with the ventral plate somewhat axe-like, the sacculus roundly projected near distal end, and the aedeagus with a narrow band at middle in the male genitalia; and the corpus bursae without signum but with two slightly sclerotized areas in the female genitalia.Published as part of Wang, S. X. & Li, H. H., 2006, Review of the genus Periacma Meyrick (Lepidoptera, Oecophoridae) from China, with descriptions of four new species, pp. 2371-2393 in Journal of Natural History 40 (41 - 43) on page 2379, DOI: 10.1080/00222930601088123, http://zenodo.org/record/523174
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No full textData from Weixing Liu, Lin Jiang,
Sen Yang, Zhou Wang, Rui Tian,
Ziyang Peng, Yongliang
Chen, Xingxu Zhang, Jialiang Kuang, Ning
Ling, Shaopeng Wang; Lingli Liu. Critical transition of soil bacterial diversity and
composition triggered by nitrogen enrichment</b
Influence of liquid CO2 phase transition blasting on hydraulic fracturing in combined fracturing conditions
Get PDFAcoustic emission noise reduction: A case of a uniaxial compression test of gypsum-like rock
No full textIn acoustic emission tests, the effective signal generated by crack initiation and propagation inside a sample is easily affected by the testing machine, earth vibration and other external noise, which increases the difficulty of data processing and analysis. To solve this problem, a gypsum sample under uniaxial compression is taken as an example to analyze and process the acoustic emission signal during the experiment. The test results show that these noises generally have the characteristics of acoustic sources far from the probe and signal types different from the effective signal. Therefore, a series of methods concerning the noise reduction of acoustic emission signals, including acoustic emission signal preprocessing, acoustic source distance denoising, and acoustic source type denoising, is proposed. Through three analyses and treatments of acoustic emission parameters, noise reduction was achieved with good results. According to the principles of these methods, some suggestions have been put forward for the position of probes in acoustic emission tests; that is, the connection of two probes should not be perpendicular to a weak plane (bedding, joints, etc.). These results could provide a theoretical reference for the postprocessing of acoustic emission signals in mechanical tests
Greenhouse gas emissions and nitrogen removal from wastewater - constructed wetland solutions
No full textSince the Paris Agreement in 2015, total carbon emissions have been controlled. However, greenhouse gas emissions from the wastewater treatment industry have increased almost every year since 2009. Although constructed wetlands have been proposed as a green water treatment technology to address climate challenges, our understanding of their role is still limited. Therefore, we review the research status of greenhouse gases in constructed wetlands and synthesize the current best estimates of their impact on the global greenhouse gas cycle from five perspectives, particularly in the field of wastewater nitrogen cycle. These perspectives include energy self-sufficiency and complete neutralization, their role as a complete ecosystem, the unique advantages compared to other treatment methods, countermeasures in special environments, and future development strategies. We believe that new insights and innovations will promote the practical application of constructed wetlands and potentially achieve complete greenhouse gas neutralization in the wastewater treatment industry
Massive stars exploding in a He-rich circumstellar medium: X. Flash spectral features in the Type Ibn SN 2019cj and observations of SN 2018jmt
No full textZ.-Y. Wang et al. -- Optical and NIR photometric measurements of SN 2018jmt and SN 2019cj are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/691/A156. Our observations are available via the Weizmann Interactive Supernova Data Repository (WISeREP; Yaron & Gal-Yam 2012).We present optical and near-infrared observations of two Type Ibn supernovae (SNe), SN 2018jmt and SN 2019cj. Their light curves have rise times of about ten days, reaching an absolute peak magnitude of Mg(SN 2018jmt) = −19.07 ± 0.37 and MV(SN 2019cj) = −18.94 ± 0.19 mag, respectively. The early-time spectra of SN 2018jmt are dominated by a blue continuum, accompanied by narrow (600−1000 km s−1) He I lines with the P-Cygni profile. At later epochs, the spectra become more similar to those of the prototypical SN Ibn 2006jc. At early phases, the spectra of SN 2019cj show flash ionisation emission lines of C III, N III, and He II superposed on a blue continuum. These features disappear after a few days, and then the spectra of SN 2019cj evolve similarly to those of SN 2018jmt. The spectra indicate that the two SNe exploded within a He-rich circumstellar medium (CSM) lost by the progenitors a short time before the explosion. We modelled the light curves of the two SNe Ibn to constrain the progenitor and the explosion parameters. The ejecta masses are consistent with either what is expected for a canonical SN Ib (∼2 M⊙) or for a massive Wolf Rayet star (> ∼4 M⊙), with the kinetic energy on the order of 1051 erg. The lower limit on the ejecta mass (> ∼2 M⊙) argues against a scenario involving a relatively low-mass progenitor (e.g. MZAMS ∼ 10 M⊙). We set a conservative upper limit of ∼0.1 M⊙ for the 56Ni masses in both SNe. From the light curve modelling, we determined a two-zone CSM distribution, with an inner, flat CSM component and an outer CSM with a steeper density profile. The physical properties of SN 2018jmt and SN 2019cj are consistent with those expected from the core collapse of relatively massive envelope-stripped stars.We gratefully thank the anonymous referee for his/her insight ful comments and suggestions that improved the paper. We thank J. Burke, C. Pellegrino for their LCO data, thank S. J. Smartt for his ePESSTO support, and thank K. Maguire, V. Brinnel, C. Barbarino, A. Razza for conducting part of the ePESSTO observations. Y.-Z. Cai thanks for the help ful discussion with Zhengwei Liu. Y.-Z. Cai is supported by the National Natural Science Foundation of China (NSFC, Grant No. 12303054) and the Yunnan Fundamental Research Projects (Grant No. 202401AU070063). BW, JJZ and YZC are supported by the International Centre of Supernovae, Yun nan Key Laboratory (No. 202302AN360001). AP, AR, EC, NER, SB, and GV acknowledge support from the PRIN-INAF 2022 project “Shedding light on the nature of gap transients: from the observations to the model”. AR also acknowledges financial support from the GRAWITA Large Program Grant (PI P. D’Avanzo). KM acknowledges support from the JSPS KAKENHI grant JP20H00174 and JP24H01810. RC acknowl edges support from Gemini ANID ASTRO21-0036. T.-W.C., AA acknowledge the Yushan Fellow Program by the Min istry of Education, Taiwan for the financial support (MOE 111-YSFMS-0008-001-P1). AGY’s research is supported by the EU via ERC grant No. 725161, the ISF GW excellence cen ter, an IMOS space infrastructure grant and a GIF grant, as well as the André Deloro Institute for Advanced Research in Space and Optics, The Helen Kimmel Center for Planetary Science, the Schwartz/Reisman Collaborative Science Program and the Norman E Alexander Family M Foundation ULTRA SAT Data Center Fund, Minerva and Yeda-Sela; AGY is the incumbent of the The Arlyn Imberman Professorial Chair. MN is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 948381) and by UK Space Agency Grant No. ST/Y000692/1. F.O.E. acknowledges sup port from the FONDECYT grant nr. 1201223. M.P. acknowl edges support from a UK Research and Innovation Fellow ship (MR/T020784/1). Maokai Hu is Supported by the Post doctoral Fellowship Program of CPSF under Grant Number GZB20240376 and the Shuimu Tsinghua Scholar Program. Q.W. is supported in part by NASA grants 80NSSC22K0494, 80NSSC21K0242 and 80NSSC19K0112. Q.W. is also par tially supported by STScI DDRF fund. L.G. acknowledges financial support from AGAUR, CSIC, MCIN and AEI 10.13039/501100011033 under projects PID2020-115253GA I00, PIE 20215AT016, CEX2020-001058-M, and 2021-SGR 01270. H.Lin is supported by the National Natural Science Foun dation of China (NSFC, Grant No. 12403061) and the innovative project of “Caiyun Post-doctoral Project” of Yunnan Province. MR acknowledges support from National Agency for Research and Development (ANID) grants ANID-PFCHA/Doctorado Nacional/2020-21202606. D.-D.Shi acknowledges the support from the National Science Foundation of China (12303015) and the National Science Foundation of Jiangsu Province (BK20231106). B. Warwick acknowledges the support from UKRI’s STFC studentship grant funding, project reference ST/X508871/1. J.Z. is supported by the National Key R&D Program of China with No. 2021YFA1600404, the National Natural Science Foundation of China (12173082), the science research grants from the China Manned Space Project with No. CMS-CSST-2021-A12, the Yunnan Province Foundation (202201AT070069), the Top-notch Young Talents Program of Yunnan Province, the Light of West China Program provided by the Chinese Academy of Sciences, the International Centre of Supernovae, Yunnan Key Laboratory (No. 202302AN360001). B. Wang is supported by the National Natural Science Founda tion of China (No 12225304) and the Western Light Project of CAS (No. XBZG-ZDSYS-202117). XFW is supported by the National Natural Science Foundation of China (NSFC grants 12288102, 12033003, 11633002, and 12303047) and the Ten cent Xplorer Prize. XJZ is supported by the National Natu ral Science Foundation of China (Grant No. 12203004) and by the Fundamental Research Funds for the Central Universi ties. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA’s Sci ence Mission Directorate. Some of the observations reported in this paper were obtained with the Southern African Large Tele scope (SALT). The Inter-University Centre for Astronomy and Astrophysics (IUCAA), India is an official partner of SALT col laboration. RR acknowledges IUCAA SALT collaboration for providing the observing time at SALT under SALT large sci ence proposal “Observing the Transient Universe” with David Buckley as the Principal Investigator. Polish participation in SALT is funded by grant No. MEiN nr 2021/WK/01. Based on observations collected at the European Southern Observatory under ESO programmes 199.D-0143, 0102.A-9099(A) and data obtained from the ESO Science Archive Facility with DOI(s) under https://doi.org/10.18727/archive/86. Part of the funding for GROND (both hardware as well as personnel) was gener ously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). This work makes use of data from the Las Cumbres Observatory Network and the Global Supernova Project. The LCO team is supported by U.S. NSF grants AST 1911225 and AST-1911151, and NASA. We thank Las Cum bres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grants GBMF5490 and GBMF10501 to the Ohio State University, and also funded in part by the Alfred P. Sloan Foundation grant G-2021-14192. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmol ogy and AstroParticle Physics at the Ohio State University, the Chinese Academy of Sciences South America Center for Astron omy (CAS-SACA), and the Villum Foundation. SDSS is man aged by the Astrophysical Research Consortium for the Par ticipating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Sci ence, Carnegie Mellon University, Center for Astrophysics | Har vard & Smithsonian (CfA), the Chilean Participation Group, the French Participation Group, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU) / University of Tokyo, the Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max Planck-Institut für Astrophysik (MPA Garching), Max-Planck Institut für Extraterrestrische Physik (MPE), National Astro nomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatório Nacional / MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United King dom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boul der, University of Oxford, University of Portsmouth, Univer sity of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale Uni versity. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the National Science Foundation. This work has made use of data from the Asteroid Terrestrial-impact Last Alert System (ATLAS) project. The Asteroid Terrestrial-impact Last Alert System (ATLAS) project is primarily funded to search for near earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; byproducts of the NEO search include images and catalogues from the sur vey area. This work was partially funded by Kepler/K2 grant J1944/80NSSC19K0112 and HST GO-15889, and STFC grants ST/T000198/1 and ST/S006109/1. The ATLAS science prod ucts have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen’s Uni versity Belfast, the Space Telescope Science Institute, the South African Astronomical Observatory, and The Millennium Insti tute of Astrophysics (MAS), Chile. This research is based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia, e Inovação (MCTI) da República Federa tiva do Brasil, the U.S. National Optical Astronomy Observa tory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, Califor nia Institute of Technology, under contract with the National Aeronautics and Space Administration. iraf was distributed by the National Optical Astronomy Observatory, which was man aged by the Association of Universities for Research in Astron omy (AURA), Inc., under a cooperative agreement with the U.S. NSF.With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (CEX2020-001058-M)Peer reviewe
Environmental performance of urban integration regions of Chengdu, Deyang, Meishan and Ziyang, based on DPSIR model
Get PDFThe paper focuses on the quantitative assessment of the environmental performance of the Urban Integration region of Chengdu, Deyang, Meishan, and Ziyang (Chengdemeizi Urban Integration) in 2015-2019, including the overall level, changing trends of the environmental performance, and the key factors that influence the environmental performance. The theme framework and driver-force-pressure-state-impact-response (DPSIR) model is used to build the evaluation indicator system, the target approximation method and the combination weighting method are adopted to calculate the environmental performance index (EPI). In addition, the Pearson correlation analysis with GDP is performed to analyze the relationship between environmental performance and the economic development level of the Urban Integration region. The results indicated that regional average scores of comprehensive environmental performances show an obvious improvement trend and had significantly positive correlation with economic level from 2015 to 2019. For the EPIs of 2nd indicators, environmental quality is the main restrictive indicator. For the EPIs of 3rd indicators, air quality, noise, and environmental management are the main restrictive indicators. Each city has different performance, and the order of EPI scores of the four cities from largest to smallest is Chengdu > Deyang > Ziyang > Meishan. Therefore, the four cities need to continuously improve their respective shortcoming environmental performance indicators and promote the balanced improvement of indicators at all levels.The paper focuses on the quantitative assessment of the environmental performance of the Urban Integration region of Chengdu, Deyang, Meishan, and Ziyang (Chengdemeizi Urban Integration) in 2015-2019, including the overall level, changing trends of the environmental performance, and the key factors that influence the environmental performance. The theme framework and driver-force-pressure-state-impact-response (DPSIR) model is used to build the evaluation indicator system, the target approximation method and the combination weighting method are adopted to calculate the environmental performance index (EPI). In addition, the Pearson correlation analysis with GDP is performed to analyze the relationship between environmental performance and the economic development level of the Urban Integration region. The results indicated that regional average scores of comprehensive environmental performances show an obvious improvement trend and had significantly positive correlation with economic level from 2015 to 2019. For the EPIs of 2nd indicators, environmental quality is the main restrictive indicator. For the EPIs of 3rd indicators, air quality, noise, and environmental management are the main restrictive indicators. Each city has different performance, and the order of EPI scores of the four cities from largest to smallest is Chengdu > Deyang > Ziyang > Meishan. Therefore, the four cities need to continuously improve their respective shortcoming environmental performance indicators and promote the balanced improvement of indicators at all levels
The impact of temperature and pressures on the efficiency of CH4 replacement in CO2-injected coal
No full texthis study examines the effects of temperature (T), CO2 injection pressure (P0), and initial CH4 adsorption equilibrium pressure
(P1) on the CH4 replacement rate (η) following CO2 injection into anthracite coal. Using experimental data on the CH4 replacement rate under
varying conditions, a response surface methodology (RSM) was applied to evaluate the individual and interactive influences of these param-
eters on the CH4 replacement process. The results demonstrate that the CH4 replacement rate increases with both temperature and CO2
injection pressure but decreases with higher initial CH4 adsorption equilibrium pressure. Furthermore, the sensitivity of the CH4 replacement
rate to the individual factors is ordered as P1 > P0 > T. The interaction effects between two factors are ranked as follows: fP1 and P0g >
fP1 and Tg > fP0 and Tg. These findings provide valuable insights for optimizing CO2-ECBM technology and refining operational
parameters
DS_TECH834057 – Supplemental material for A Mass-Ratiometry-Based CD45 Barcoding Method for Mass Cytometry Detection
No full textSupplemental material, DS_TECH834057 for A Mass-Ratiometry-Based CD45 Barcoding Method for Mass Cytometry Detection by Hongu Meng, Antony Warden, Lulu Zhang, Ting Zhang, Yiyang Li, Ziyang Tan, Boqian Wang, Hongxia Li, Hui Jiang, Guangxia Shen, Yifan Hong and Xianting Ding in SLAS Technology</p
Supplemental Material - A diffuse reflectance portable near infrared spectroscopy system for the determination of biuret content in urea fertilizer
No full textSupplemental Material for A diffuse reflectance portable near infrared spectroscopy system for the determination of biuret content in urea fertilizer by Jing Liu, Shaohui Yu, Shupeng Hu, Ziyang Ling, Jiguang Gao, Binmei Liu, Lixiang Yu, Yang Yang, Ye Yang, Qi Wang, Xiaoyu Ni, Liping Zhao and Yuejin Wu in Journal of Near Infrared Spectroscopy</p
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