Torsional oscillations of magnetized relativistic stars

Strong magnetic fields in relativistic stars can be a cause of crust fracturing, resulting in the excitation of global torsional oscillations. Such oscillations could become observable in gravitational waves or in high-energy radiation, thus becoming a tool for probing the equation of state of relativistic stars. As the eigenfrequency of torsional oscillation modes is affected by the presence of a strong magnetic field, we study torsional modes in magnetized relativistic stars. We derive the linearized perturbation equations that govern torsional oscillations coupled to the oscillations of a magnetic field, when variations in the metric are neglected (Cowling approximation). The oscillations are described by a single two-dimensional wave equation, which can be solved as a boundary-value problem to obtain eigenfrequencies. We find that, in the non-magnetized case, typical oscillation periods of the fundamental     torsional modes can be nearly a factor of 2 larger for relativistic stars than previously computed in the Newtonian limit. For magnetized stars, we show that the influence of the magnetic field is highly dependent on the assumed magnetic field configuration, and simple estimates obtained previously in the literature cannot be used for identifying normal modes observationally.     

Amplification of primordial magnetic fields by anisotropic gravitational collapse

If a magnetic field is frozen into a plasma that undergoes spherical compression, then the magnetic field B varies with the plasma density ρ according to   B ∝ρ^2/3  . In the gravitational collapse of cosmological density perturbations, however, quasi-spherical evolution is very unlikely. In anisotropic collapses the magnetic field can be a much steeper function of gas density than in the isotropic case. We investigate the distribution of amplifications in realistic gravitational collapses from Gaussian initial fluctuations using the Zel'dovich approximation. Representing our results using a relation of the form   B ∝ρ^α  , we show that the median value of α can be much larger than the value  α= 2/3  resulting from spherical collapse, even if there is no initial correlation between magnetic field and principal collapse directions. These analytic arguments go some way towards understanding the results of numerical simulations.     

Impact demagnetization of the martian crust

The lack of magnetic anomalies within the giant martian impact basins, Hellas, Argyre, and Isidis suggests that the impacts demagnetized the crust. Our analysis of the magnetic anomaly intensity shows that the interior parts of the basins are completely demagnetized, while the outer parts and surroundings are partially demagnetized. We investigate the shock pressure and impact heating resulting from the impacts. The crust has been completely demagnetized within ∼0.8 basin radius by a combination of thermal and shock effects, and the surroundings have been partially demagnetized by shock to a distance of at least 1.4 radii. We also investigate magnetic signatures of intermediate-size craters. From the pressures generated by both the large and intermediate-sized impacts, we conclude that the remanent magnetization is carried at least in part by high coercivity rocks. Since the crust beneath the basins does not appear to have been remagnetized as it cooled following the impacts, we conclude that the martian core dynamo was inactive or very weak for at least 100 Myr following the Hellas impact.     

图根支导线测角中误差计算公式之讨论

本文结合实例讨论了小地区平面控制测量中多条图根支导线测角中误差m角平的三种计算方法,其中方法二全面考虑多条图根支导线的测量误差,其计算测角中误差m角平的公式也是最值得推广的。按照方法二可计算出各条图根支导线的测站点圆周角闭合差是否超过±40″,各条支导线的角度闭合差fβj是否超过40 n1″,测角中误差m角平是否超过21.2″,由此可以判断测角精度是否合格,在测量工作中具有一定的实用性。     

油气勘探开发数据体平均值代表性分析

油气勘探开发涉及各类数据体,同一数据体可得多种平均值,目前尚无明确而有效的方法以判断何种平均值能客观反映数据体的典型水平。运用数据统计平均分析方法,对勘探开发实践中的孔隙度、渗透率、产量、成本等数据体进行系统分析,确立了加权中位数计算公式和平衡中位数法则。加权中位数计算公式适于分析不同领域正常有序数据体的基本特征,加权中位数为正常有序数据体的平衡点;平衡中位数法则适于确定有足够大数据容量、能满足统计分析基本要求、能选择合理权衡指标的正常有序数据体的典型水平;有明确物理意义的加权平均值也可确定数据体的典型水平。     

我国油气资源潜力、分布及重点勘探领域

我国地质结构具有3大板块、3大构造域多旋回构造演化特征,造就多种类型叠合沉积盆地,构成克拉通+前陆、断陷+坳陷、前陆+坳陷3种主要类型。大型叠合盆地是油气资源分布与勘探开发主体。我国常规与非常规油气资源十分丰富,常规石油地质资源量1 075×10⁸ t,常规天然气地质资源量83×10¹² m³;致密油地质资源量134×10⁸ t,致密砂岩气地质资源量21×10¹² m³,页岩油地质资源量335×10⁸ t,页岩气地质资源量56×10¹² m³。陆上油气资源主要分布于渤海湾(陆上)、松辽、鄂尔多斯、塔里木、四川、准噶尔、柴达木7大盆地。海域油气资源主要分布于渤海湾(海域)、东海及南海北部的珠江口、北部湾、莺歌海、琼东南6大盆地。未来我国油气勘探应始终坚持“资源战略,稳油增气”战略,坚持“非常并进、海陆统筹”积极进取勘探思路;常规勘探领域,陆上地层-岩性、前陆、海相碳酸盐岩与潜山领域;海域为渤海海域构造与基岩潜山,深水构造与岩性;非常规油气主要是立足陆上7大含油气盆地,立足致密油气与页岩油气,强化勘探开发与技术配套。     

基于CMIP6模式的黄河上游地区未来气温模拟预估

利用第六次国际耦合模式比较计划（CMIP6）提供的5个气候模式,并结合基于地面气象站的CN05.1气象资料,评估了CMIP6模式对黄河上游地区1961—2014年气温变化的模拟能力。基于7个共享社会经济路径及代表性浓度路径（SSP-RCP）组合情景,结合多模式集合平均预估了2015—2100年黄河上游地区年均气温和季平均气温的时空变化规律。结果表明：多模式集合平均能较好地模拟黄河上游地区历史平均气温的空间分布格局与年变化。7个未来情景一致表明,2015—2100年黄河上游地区年平均气温呈现波动上升趋势［0.03～0.82 ℃?（10a）^-1］。其中,低辐射强迫情景下（SSP1-1.9、SSP1-2.6及SSP4-3.4）气温先呈现增加趋势,21世纪中期到达增幅峰值,之后增温呈现放缓趋势;而中、高辐射强迫情景下（SSP2-4.5、SSP3-7.0、SSP4-6.0及SSP5-8.5）气温表现为持续上升态势。空间上,未来气温增幅显著的区域位于黄河上游西部地区;时间上,呈现夏季增温快,春季增温慢。四季增温的空间分布呈现出一致特征,表现为西部增温强于东部,北部增温强于南部。研究结果可为黄河流域水资源管理及气候变化的适应性研究提供科学依据。     

方差分量估计在高速铁路铺轨控制网中的应用

在处理边角网平差时,由于测边、测角相互独立,通常只能根据经验按观测类型不同进行验前方差估计,不能准确确定测边、测角观测量的权,影响了控制网的精确度。以高铁铺轨控制网(CPIII)数据处理为例,采用方差分量估计方法对控制网进行了数据处理和精度分析,并与等权处理方法做了比较,对边角网或其它不同类型的复杂控制网数据处理具有一定的参考价值。     

基于中性集对北川羌族自治县新城人工建设用地的识别

人工建设用地(包括建筑物、道路、广场等社会服务设施)的识别一直是用来监测地区发展速度的一个有效途径。针对目前在人工建设用地识别领域中对在建建筑物的忽视问题,利用中性集、均值漂移以及绿度因子等概念将在建建设用地信息进行增强,进而将其成功识别出来。实验证明,该方法对高分辨率遥感影像的人工建设用地识别是可行的。通过分析2009—2013年期间北川新城的建设工地面积及分布的变化情况可以看出,北川新城在2010—2013年期间完工面积占2009—2010年新建工程总面积的98.17%,在北川新城拓展区又新建0.6 km2的工程,施工迅速,为受灾居民提供了良好的居住和生活保障。