Predicting impacts of climate change on the biogeographic patterns of representative species richness in Prydz Bay-Amery Ice Shelf

The research on the biological ecology of the Prydz Bay-Amery Ice Shelf in East Antarctica is inadequate under the increasing threat from climate change, especially for Antarctic fish and krill. The Dynamic Bioclimatic Envelope Model(DBEM) has been widely used in predicting the variation of species distribution and abundance in ocean and land under climate change; it can quantify the spatiotemporal changes of multi population under different climate emission scenarios by identifying the environm...     

地下水气体组分的潮汐变化

我们观察了日本中部Omaezaki地区地下水气体组分时间序列数据的周期性变化,Omaezaki是日本地震预报目录中即将到来的Tokai地震前兆信号观察的重要地区.我们已经开始在一口100 m深的井中对地下水中气体组分进行持续监测.     

不同种植方式高油酸花生小气候特征研究

为研究不同种植方式下高油酸花生小气候特征,于2020年在商丘国家基准气候站内开展花生分期播种试验,试验设计5月6日、5月26日和6月15日3个播期,按垄作和平作两种方式种植。在5月6日播种的垄上、垄下和平作的花生田内安装温湿度自动记录仪,对比分析不同种植方式对农田气温、相对湿度及产量的影响,研究农田温湿度与基准站气象要素的定量关系。结果表明,种植方式不同,花生农田小气候特征存在差异。不同发育期,垄上和垄下气温均高于平作的,且二者之间的差异白天的大于夜间的。下针-饱果期和饱果-成熟期垄上平均气温分别比平作的高0.5℃和0.9℃,日较差分别比平作的高1.1℃和2.1℃;田间相对湿度平作的高于垄上和垄下的,下针-饱果期和饱果-成熟期垄上相对湿度日较差分别比平作的高11.2%和15.3%。典型晴天和多云天,基准站夜间气温高于垄上、垄下和平作的,白天的气温低于垄上、垄下和平作的;阴雨天垄上气温高于垄下、平作和基准站的。3种天气条件下,平作相对湿度高于垄上、垄下和基准站的。高油酸花生小气候与基准站温湿度之间存在显著的一元线性相关关系。3个播期的垄作花生单株荚果数、单株果重和产量均高于平作的,且呈极...     

Application of soft computing techniques for shallow foundation reliability in geotechnical engineering

This research focuses on the application of three soft computing techniques including Minimax Probability Machine Regression(MPMR),Particle Swarm Optimization based Artificial Neural Network(ANN-PSO)and Particle Swarm Optimization based Adaptive Network Fuzzy Inference System(ANFIS-PSO)to study the shallow foundation reliability based on settlement criteria.Soil is a heterogeneous medium and the involvement of its attributes for geotechnical behaviour in soil-foundation system makes the prediction of settlement of shallow a complex engineering problem.This study explores the feasibility of soft computing techniques against the deterministic approach.The settlement of shallow foundation depends on the parametersγ(unit weight),e0(void ratio)and CC(compression index).These soil parameters are taken as input variables while the settlement of shallow foundation as output.To assess the performance of models,different performance indices i.e.RMSE,VAF,R^2,Bias Factor,MAPE,LMI,U(95),RSR,NS,RPD,etc.were used.From the analysis of results,it was found that MPMR model outperformed PSO-ANFIS and PSO-ANN.Therefore,MPMR can be used as a reliable soft computing technique for non-linear problems for settlement of shallow foundations on soils.     

A New Emission Mode of PSR B1859+07

Previous studies have identified two emission modes in PSR B1859+07: a normal mode that has three prominent components in the average profile, with the trailing one being the brightest, and an anomalous mode(i.e., the A mode) where emissions seem to be shifted to an earlier phase. Within the normal mode, further analysis has revealed the presence of two submodes, i.e., the cW mode and c B mode, where the central component can appear either weak or bright. As for the anomalous mode, a new bright ...     

Challenges in the Detection and Attribution of Northern Hemisphere Surface Temperature Trends Since 1850

Since 2007, the Intergovernmental Panel on Climate Change(IPCC) has heavily relied on the comparison between global climate model hindcasts and global surface temperature(ST) estimates for concluding that post-1950s global warming is mostly human-caused. In Connolly et al., we cautioned that this approach to the detection and attribution of climate change was highly dependent on the choice of Total Solar Irradiance(TSI) and ST data sets.We compiled 16 TSI and five ST data sets and found by alter...     

New Cases of Superflares on Slowly Rotating Solar-type Stars and Large Amplitude Superflares in G-and M-type Main Sequence Stars

In our previous work, we searched for superflares on different types of stars while focusing on G-type dwarfs using entire Kepler data to study statistical properties of the occurrence rate of superflares. Using these new data, as a byproduct, we found 14 cases of superflare detection on 13 slowly rotating Sun-like stars with rotation periods of24.5–44 days. This result supports the earlier conclusion by others that the Sun may possibly undergo a surprise superflare. Moreover, we found 12 and se...     

Effect of Matching Algorithm and Profile Shape on Pulsar Pulse Time of Arrival Uncertainties

For high-precision pulsar timing analysis and low-frequency gravitational wave detection, it is essential to accurately determine pulsar pulse times of arrival(ToAs) and associated uncertainties. To measure the ToAs and their uncertainties, various cross-correlation-based techniques can be employed. We develop methodologies to investigate the impact of the template-matching method, profile shape, signal-to-noise ratio of both template and observation on ToA uncertainties. These methodologies are...     

The Variability and Radial Velocity of Planetary Nebula Central Stars

The extremely accurate estimates of stellar variability and radial velocity in the Gaia Data Release 3(Gaia DR3)have enabled us to examine the close binarity and radial velocity(RV) of central stars(CSs) of planetary nebulae(PNe). This study is twofold:(1) searching for new close binary CS candidates to better understand how binarity affects the formation and evolution of PNe; and(2) extending the sample size of known RVs of PNe in order to understand their kinematics and the dynamics of the Mil...     

Validation of Foreground Emission Model using GALEX Medium Observations

The study of diffuse ultraviolet(UV) background radiation is vital in the investigation of stellar and galactic evolution. Space-based UV observations are comprised of both foreground and background radiations. The foreground emission in an observation is a result of solar contamination in the direction of observation. In our previous work, we modeled airglow(one of the major constituents of the foreground emission) as a function of10.7 cm Solar Flux and Sun Angle with great accuracy using GALEX...