Prompt optical emission and synchrotron self-absorption constraints on emission site of GRBs

We constrain the distance of the gamma-ray burst (GRB) prompt emission site from the explosion centre R , by determining the location of the electron's self-absorption frequency in the GRB prompt optical-to-X/γ-ray spectral energy distribution, assuming that the optical and the γ-ray emissions are among the same synchrotron radiation continuum of a group of hot electrons. All possible spectral regimes are considered in our analysis. The method has only two assumed parameters, namely the bulk Lorentz factor of the emitting source Γ and the magnetic field strength B in the emission region (with a weak dependence). We identify a small sample of four bursts that satisfy the following three criteria: (1) they all have simultaneous optical and γ-ray detections in multiple observational time intervals, (2) they all show temporal correlations between the optical and γ-ray light curves and (3) the optical emission is consistent with belonging to the same spectral component as the γ-ray emission. For all the time intervals of these four bursts, it is inferred that   R ≥ 10¹⁴  (Γ/300)^3/4 ( B /10⁵ G)^1/4  cm. For a small fraction of the sample, the constraint can be pinned down to   R ≈ 10¹⁴–10¹⁵ cm  for  Γ∼ 300  . For a second sample of bursts with prompt optical non-detections, only upper limits on R can be obtained. We find no inconsistency between the R -constraints for this non-detection sample and those for the detection sample.     

Variability of Extended Bipolar Regions

Using NSO/Kitt Peak synoptic charts from 1975 to 2003, we group the main solar magnetic fields into two categories: one for active regions (ARs) and the other for extended bipolar regions (EBRs). Comparing them, we find that there exist three typical characteristics in the variability of EBRs: First, there exists a correlation between ARs and EBRs. The phase of EBR flux has a delay nearly two CRs. Second, we find that the EBR flux has two prominent periods at 1.79 years and 3.21 years. The 1.79-year period seems to only belong to large-scale magnetic features. Lastly, the North – South asymmetry of EBR flux is not very significant on a time scale of one solar cycle. However, during solar maxima, its dominance is found to shift from one hemisphere to the other.     

青藏高原河流网络高分CubeSat遥感监测

河流网络是地表水循环的重要组成部分,如何实现河流网络动态监测已成为河流遥感研究的热点。近年来,以PlanetScope为代表的CubeSat小卫星已具备了米级空间分辨率、1 d重访周期的优势,这为河流网络高时空分辨率动态监测提供了可能。本文以青藏高原长江源区的通天河流域（227 km²）为研究区,选取2017-05—2017-10 5期3 m空间分辨率CubeSat遥感影像,增强河流横纵剖面特征自动化提取了河流网络,研究了通天河流域河流网络动态变化,对比分析了3 m CubeSat与30 m Landsat 8、10 m Sentinel-2所提取的河流网络,以及5种现有水体数据集（GRWL,GSW,FROM-GLC 2017,OpenStreetMap,HydroSHEDS）。研究结果表明：（1）研究区内河流网络5月水系密度较低（0.38 km^-1）,7—8月河流网络进入丰水期,水系密度显著增加至0.61 km^-1,9月河流网络进入平水期,水系密度趋于平稳（0.53 km^-1）,随后迅速退化并于10月开始冻结,水系密度迅速降低至0.37 km^-1;（2）采用高空间分辨率CubeSat所提取的河流网络能够识别更多细小河流（河宽3—30 m）,CubeSat所提取的河流总长分别为Landsat 8、Sentinel-2所提取河流总长的1.6倍和1.3倍;（3）CubeSat所提取的河流网络水系密度高于现有水体数据集（2.9—12.4倍）,弥补了现有水体数据集无法反映细小河流的不足。     

Using a New Sky Brightness Monitor to Observe the Annular Solar Eclipse on 15 January 2010

For the future development of Chinese Giant Solar Telescope (CGST) in Western China, a new sky brightness monitor (SBM) has been produced for the site survey for CGST. To critically examine the performance and sensitivity of SBM, we used it in the observation of the annular solar eclipse in Dali City, Yunnan, on 15 January 2010. The observation met good weather conditions with an almost clear sky during the eclipse. The SBM measurement translates into the solar illuminance changes at a level of 2.4×10^?4 I?s^?1 during the eclipse. The time of the minimal sky brightness in the field of view (FOV) is found consistent with the time of maximum eclipse. Two local sky regions in the FOV are chosen to make a time series of the calibrated skylight profiles. The evolution of the sky brightness thus calibrated also shows good consistency with the eclipse, particularly between the second and the third contacts. The minimal sky brightness in each local sky region took place within half a minute from the corresponding predicted contact time. Such small time delays were mainly caused by occasional cirri. The minimal sky brightness measured during the eclipse is a few millionths of I _?? with standard deviation of 0.11 millionths of I _??. The observation supports that the single-scattering process (optically thin conditions) is the main contributor to the atmospheric scattering. We have demonstrated that many important aerosol optical parameters can be deduced from our data. We conclude that the new SBM is a sensitive sky photometer that can be used for our CGST and coronagraph site surveys.     

基于CLG光学流和波场分解的逆时偏移角度道集提取方法研究

角度域共成像点道集是衔接叠前地震数据与储层特征的重要桥梁,对地震偏移成像与储层描述具有重要意义.与克希霍夫偏移和单向波动方程偏移相比,逆时偏移是复杂地区最精确的成像方法.高效稳健地生成逆时偏移角度道集目前仍然是一个挑战.本文主要讨论如何采用光学流方法高效、高质量地提取角度道集.在逆时偏移波场外推过程中,光学流方法可以估计波场传播方向.其中Lucas-Kanade(LK)和Horn-Schunck(HS)方法是光学流方法中两种典型的方法.LK光学流方法是一种局部方法,该方法依赖于局部点的梯度值,但是容易出现奇异现象,HS光学流方法属于全局方法,波场方向估计依赖于整个波场,易受噪声影响,对异常值比较敏感,导致整体波场方向计算精度不高.本文提出采用局部和整体结合(Combining Local and Global,CLG)的光学流方法估计波场传播方向.该方法可以有效地提高波场方向的精度,并且简单高效,便于并行处理.对比HS光学流方法,CLG光学流方法几乎不增加额外的计算量.另外,为了弱化光学流方法无法处理波前重叠问题,本文利用解析波场和方向滤波对波场进行方向分解,仅需波场的空间傅里叶变换即可实现任意波场方向分解,将分解后的波场分别估计波场反向,提取成像结果.进一步地,在估计反射张角和方位角时,本文提出有效的归一化方法和改进的最小二乘除法,提高角度估计的精度和稳定性.最后,理论和实际资料例证了本文提出方法的有效性.     

岷县-漳县MS6.6地震前后甘肃前兆异常及响应特征

分析总结了2013年7月22日甘肃岷县—漳县MS6.6地震前后甘肃前兆台网观测资料变化情况,发现该地震前有7个台站、4种观测手段、14个测项出现了明显的异常,既有长期、中长期异常,也有短期和短临异常,说明对资料的分析既要看短期变化,还要看中期和长期变化。出现异常测点的震中距多数在200 km范围之内。另外部分水位、流量和水温测点的资料记录到不同程度的同震效应;形变观测多数测点记录到比较明显的同震响应,记录同震响应的测点与震中位置、方向、距离无明显关系。     

青海玛多7.4级地震极震区震灾调查及分析

2021年5月22日2时4分,青海省玛多县发生7.4级地震,距震中26 km的野马滩大桥及周边区域为此次地震极震区（地震烈度Ⅹ度,面积约69 km2）,受损尤为严重。桥梁表现为落梁式破坏,房屋不同程度受损。对极震区内野马滩大桥及周边房屋进行实地调查与震灾分析,并提出灾后重建及震灾防御相关建议,包括组织专业人员进行灾区房屋安全鉴定,建议牧民居住建筑采用轻钢式结构,建议原地重建野马滩大桥并增加限位装置及连梁装置。