TEROS:雷暴高能辐射观测系统的设计与实现

为获取雷暴高能辐射的强度、能量及时间等信息,本文设计了一套基于双通道闪烁体探测器的分布式雷暴高能辐射观测系统.该系统由远程终端单元和高能辐射探测单元组成,基于本底放射性统计涨落实现了短爆发事件的在线识别,并可通过累积能谱数据离线检索γ射线辉光事件,具有测量能量范围宽、抗干扰能力强、易组网等特点.利用碘化钠闪烁体探测器建立的国内首个分布式雷暴高能辐射观测系统在人工引雷试验中得到应用验证,在全部5次人工触发闪电的22次先导/回击过程中,捕获到17次高能辐射事件.试验结果表明该系统具备复杂电磁环境下的雷暴高能辐射在线监测与数据采集能力,将为本领域研究持续提供观测资料,推动国内高能大气物理研究的发展.

     

滇黔桂“金三角”地区晚三叠世地层碎屑物源示踪

三叠系是滇黔桂分布最广泛的岩系,赋存卡林型金矿等各种低温矿产。在前人研究基础上,运用LA-ICP-MS分析技术,对滇黔桂"金三角"地区的碎屑锆石进行了U-Pb测年。结果显示,大部分锆石具岩浆环带,Th/U值大于0.4,锆石U-Pb年龄集中在308~396 Ma、440~680 Ma、727~930 Ma、1004~1266 Ma、1400~1880 Ma、2360~2724 Ma六个区段。通过对比研究区及周围地块的碎屑锆石年龄分布特征,结合研究区岩相古地理、古海流及古流向,综合分析认为,研究区物源以越北古陆为主,同时湘粤桂构造山系和云开地区也可能提供了部分物源。该物源印证了古特提斯洋在印支期逐渐闭合,华南陆块与印支地块沿松马缝合带发生碰撞。     

英国约克郡地区的喀斯特景观、土地利用与科研专用区

英国约克郡地区的冰川喀斯特以台地－谷地两大单元、地表─地下两大结构为特征。景观价值的多样性和地产权的多属性决定了土地的多功能、开发的多目的和利用的多层次。现代各种自然保护用地、养羊养牛业为主的畜牧用地和开采石灰石为主的采矿用地等在约克郡国家公园内虽有机地融为一体,但对喀斯特科研专用区（ＫＳＳＳＩ）构成威胁。最大的潜在威胁是采矿,其次是农业和各种教育、探险和旅游活动。因此,在确定喀斯特科研保护价值的基础上,应根据国家公园管理政策的特殊性,通过土地购买、设施配置、区界调整、接近控制和管理分区等措施对ＫＳＳＳＩ进行有效的保护与管理。     

四川彭州葛仙山巨型冰川漂砾的发现及意义

四川彭州市葛仙山巨型冰川漂砾距四川盆地边缘地带约３～４ｋｍ,规模巨大（约６ｋｍ×２５ｋｍ×０３ｋｍ）,是目前世界上发现的罕见巨型冰川漂砾。现有资料研究结果表明,葛仙山巨型漂砾是早更新世青藏大冰盖冰流的搬运作用所形成的。是青藏大冰盖存在的有力证据之一,也是全球泛大冰盖形成的重要历史见证。同时对众多相关边缘学科的重大基础理论问题的研究,提供了新的思路、途径和方法     

融合先验物理信息的高精度智能可控源电磁反演算法

可控源电磁反演利用人工信号获取地下结构信息,为地质勘探和资源开发提供准确的数据支持。然而,传统电磁反演方法面临低分辨率的挑战,主要是由于简化处理和观测数据的限制,导致模型平滑、细节丢失,从而削弱了反演的准确性,影响了电磁勘探的效率。为了解决这一问题,本文提出将传统反演结果与响应数据同时作为深度网络的输入数据,为深度网络反演提供先验物理信息,并结合深度学习算法提升可控源电磁反演的计算效率。通过模型试验,对合成的电阻率模型分别进行了传统反演、智能反演以及融合先验物理信息的智能反演。结果表明,融合先验物理信息的智能反演能够更好地刻画异常体结构特征,有效提升反演效率,并且得到的电阻率参数更符合实际。最后,将该反演技术应用于金川铜镍矿床的可控源数据反演解释,取得了较为可靠的应用效果。     

Investigations into the thermal non-equilibrium of W UMa-type contact binaries

Traditionally, some physical details(e.g., magnetic braking, energy transfer, angular momentum loss, etc.) have to be taken into consideration during investigations into the evolution of contact binaries. However, the real evolutionary processes which usually contain several of these physical mechanisms are very complicated as a result of strong interaction between components. To avoid dealing with these factors, a linear relationship is applied to the temperatures of components. It is found that the higher the mass ratio(M_2/M_1) of a contact system, the weaker the deviation from thermal equilibrium.On this basis, a variation trend of fill-out factor(f) changing with mass ratio can be inferred, which is consistent with observations. Moreover, if we stick to this point of view, it should be natural that the number of semi-detached binaries in the predicted broken-contact phase of relaxation oscillations is less than the number in the contact phase.     

1–100 μm energy spectra and 2.3–4 μm spectrophotometry of MSC stars

The JHKL' photometry and 2.3–4 μm spectrophotometry of some M giants, S type stars and carbon stars are presented in this paper. It is found that in combination with IRAS data, the energy spectra in 1–100 μm of S type stars are intermediate between those of M giants and carbon stars, which are obviously different. The spectrophotometry in the near infrared shows that, besides carbon stars, which have HCN and C₂H₂ strong absorptions at 3.1 μm, some S type stars have the similar but weaker absorption in the same spectral region. However, no trace of any absorption at 3.1 μm can be seen in M giants. These results probably provide more evidence for the M-S-C sequence in the late stage of stellar evolution.     

Analysis on the interplanetary causes of the great magnetic storms in solar maximum (2000-2001)

In this paper, we analyze the interplanetary causes of eight great geomagnetic storms during the solar maximum (2000-2001). The result shows that the interplanetary causes were the intense southward magnetic field and the notable characteristic among the causal mechanism is compression. Six of eight great geomagnetic storms were associated with the compression of southward magnetic field, which can be classified into (1) the compression between ICMEs (2) the compression between ICMEs and interplanetary medium. It suggests that the compressed magnetic field would be more geoeffective. At the same time, we also find that half of all great storms were related to successive halo CMEs, most of which originated from the same active region. The interactions between successive halo CMEs usually can lead to greater geoeffectiveness by enhancing their southward field B_s interval either in the sheath region of the ejecta or within magnetic clouds (MCs). The types of them included: the compression between the fast speed transient flow and the slow speed background flow, the multiple MCs, besides shock compression. Further, the linear fit of the D_st versus gives the weights of and Δt as α=2.51 and β=0.75, respectively. This may suggest that the compression mechanism, with associated intense B_s, rather than duration, is the main factor in causing a great geomagnetic storm.     

CERES-Wheat模型在我国小麦区的应用效果及误差来源

气候模型与作物模型耦合是评价未来气候变化对作物生产影响的常用方法之一, 但当两者结合时, 存在着空间和时间尺度差异问题, 将作物模型升尺度到区域是解决该差异的一种方法。将CERES-Wheat模型升尺度进行区域模拟, 利用区域校准后的CERES-Wheat模型, 模拟了1981—2000年全国各网格小麦产量, 与同期农调队调查产量相比较, 以探讨CERES-Wheat模型在我国小麦区的模拟效果及误差来源。结果表明:全国小麦产量的区域模拟值与农调队调查产量的相对均方根误差为27.9%, 符合度为0.75, 全国59.2%的模拟网格相对均方根误差在30%以内, 其中相对均方根误差小于15%的占26.3%;各区的效果不同, 种植面积最大的小麦种植生态2区, 模拟效果最好。总体来说, CERES-Wheat的区域模拟, 可以反映产量变化规律, 能为宏观决策提供相应信息, 尤其是在主产区; 但区域模拟中还存在一系列误差, 今后还需进一步研究。