引力无需时间传播——“由固体潮发现引力以光速传播的观测证据”不成立

重力固体潮调和分析结果无法证明引力以光速传播。首先,根据固体潮理论,进行调和分析时固体潮理论值和观测值的时间序列是同步的,不存在时差;其次,天体起潮力仅与万有引力有关,与光速无关;第三,调和分析得到的潮汐因子仅反映地球介质的物性变化,相位滞后则反映地球介质的粘滞弹性,两者与天体引力及光到达观测点的时差无关;第四,汤克云和骆鸣津在论证过程中作了过多的人为改正,有些改正使用不当;第五,万有引力与引力波是两个不同的概念,万有引力是相互作用的两个物体之间的一种空间性质,它与两个彼此相互作用的物体同在,无需时间传播,而引力波是一种时空涟漪,需要在特定条件下产生,通过波的形式从辐射源以光速向外传播,并以引力辐射的形式传输能量,两者不可混淆。汤克云与骆鸣津认为,重力固体潮理论值隐含两个假设：1）引力以光速传播;2）引力及光的时差等于重力固体潮调和分析结果的时差。这两个假设并不成立,汤克云与骆鸣津关于引力是以光速传播的论证是一个误会,引力不需要时间传播。     

2006年夏季珠江冲淡水驱动的上升流

根据珠江口及其附近海域2006年夏季（7-8月）航次水文调查资料,发现调查期间,除了西南季风驱动下的冲淡水东向扩散外,粤西珠江口外冲淡水主要呈西向扩散趋势,并且西向扩散的冲淡水下存在上升流。已有的模型研究中,西南季风下珠江口外没有出现上升流,说明西南季风不是珠江口外上升流产生的主导因素。观测的温盐分布、潜标流速时间序列与走航ADCP流态表明,上升流产生的原因是:（1）口门外冲淡水南向扩展驱动了垂向重力环流;（2）密度跃层以下东北向沿岸流的底边界层Ekman效应;（3）口门外冲淡水团之间的气旋型中尺度涡旋作用。     

引力透镜类星体SDSS J1001+5027吸收线证认

基于斯隆数字化巡天(Sloan Digital Sky Survey,SDSS)第12期数据(data release 12,DR12)的光谱,分析引力透镜类星体SDSS J1001+5027的A, B两个像的光谱。两个像光谱的红移分别为1.84132±0.00024和1.84545±0.00012,透镜天体红移约为0.415。通过证认可靠的CⅣλλ1548, 1551或Mg Ⅱλλ2796, 2803窄吸收双线的方法,证认出A, B两个像的光谱中红移分别为1.60677±0.00012, 0.87140±0.00007和0.41455±0.00006的3个吸收系统。从3个吸收系统共证认出27条窄吸收线。测量27条窄吸收线的等值宽度,再通过分析、比较3个吸收系统在A, B两个像光谱中吸收线的数量及等值宽度的差异,给出了3个吸收系统在引力透镜类星体SDSS J1001+5027视线方向可能的分布示意图。     

KAGRA引力波探测器中频率相关压缩态实验进展

随着技术的发展,下一代引力波探测器的激光功率将得到进一步提高。大光斑半径的应用也将使探测器的热噪声进一步降低,因此,量子噪声将成为在全频段限制引力波探测器灵敏度的首要因素。作为目前最有保障的一种降低量子噪声的技术,频率相关压缩态很可能将被应用于下一代所有引力波探测器中^[1]。频率相关压缩态可以通过将频率不相关压缩态与滤波腔相结合而产生。基于滤波腔具有的频率响应特性,这一技术的应用可以使低频波段的辐射压噪声有效降低,同时实现高频波段散粒噪声的降低,从而实现全探测频段灵敏度的提升。基于日本KAGRA引力波探测器的设计,我们预计将9dB压缩度的压缩态与周损失为8×10^-5的300m滤波腔相结合,可以使探测器灵敏度在全探测频段提高1倍。此实验于2015年开始,目前滤波腔的安装调试已经基本完成,得到的结果基本与实验前的模拟相符合。与频率不相关压缩态光学实验台的安装过程也已经过半,通过温度和控制回路的调制,二次谐波腔的转化率已经超过50%。     

On a two-body problem with periodically changing equivalent gravitational parameter

Assigning to the equivalent gravitational parameter of a two-body dynamic system, a periodic change of a small amplitude B and arbitrary frequency and phase, the behaviour of an elliptic-type orbit is studied. The first order (in B) perturbations of the orbital elements are determined by using Delaunay's canonical variables. According to the value of the ratio between oscillation frequency and dynamic frequency, three cases (non-resonant (NR), quasi-resonant (QR), and resonant (R) ones) are pointed out. The solution of motion equations shows that only in the QR and R cases there are elements (argument of pericentre and mean anomaly) affected by secular perturbations. The solutions are valid over prediction times of order of pericentre and mean anomaly) affected by secular perturbations. The solutions are valid over prediction times of order B⁻¹ in the NR case and B^−1/2 in the QR and R cases.     

深浅构造的应力状态与运动特征

在活动构造调查中我们曾遇到地壳浅部构造与地壳深部构造不一致的情况,在地震烈度调查中我们也经常发现宏观震中与微观震中的空间位置不同。本文从地壳深浅部构造应力状态和运动特征的角度,对其可能的形成机制进行了分析。文中首先对地壳可能的应力状态进行了估计,然后结合对褶皱和断裂的深浅部构造应力状态与运动特征的分析,解释了地壳深浅部构造差异性的形成机制。在此基础上分析了宏观震中与微观震中存在差异的原因,最后对地壳应力场的影响因素进行了简单介绍。     

Meso-scale available gravitational potential energy in the world oceans

1 IntroductionThe oceanic general circulation takes place inthe environments of gravity. As a mechanical sys-tem, the oceanic circulation requires sources of me-chanical energy to overcome friction and dissipation.Although the ocean receives a huge amount…     

吉南浑江坳陷南缘重力滑覆构造特征

据军江地区１：５万区调资料,吉南浑江坳陷南缘发育一个由多个构造岩块组成的重力滑覆构造区,其内部自下而上可划分白山市,红旗,大梨树沟,横道河子四个滑覆体分别由新元古代一早古生代地层组成,滑覆于晚古生代地层之上,构成了所谓“四层楼”式的构造工,形成时代为早侏罗世。     

A measurement of the transverse velocity of Q2237+0305

Determination of microlensing parameters in the gravitationally lensed quasar Q2237+0305 from the statistics of high-magnification events will require monitoring for more than 100 years (Wambsganss, Paczynski & Schneider). However, we show that the effective transverse velocity of the lensing galaxy can be determined on a more realistic time-scale through consideration of the distribution of light-curve derivatives. The 10 years of existing monitoring data for Q2237+0305 are analysed. These data display strong evidence for microlensing that is not associated with a high-magnification event. An upper limit of v _t<500 km s⁻¹ is obtained for the galactic transverse velocity, which is smaller than previously assumed values. The analysis suggests that the observed microlensing variation may be predominantly due to stellar proper motions. The statistical significance of the results obtained from our method will be increased by the addition of data points from current and future monitoring campaigns. However, reduced photometric errors will be more valuable than an increased sampling rate.     

Identification of bright lenses from the astrometric observations of gravitational microlensing events

When a source star is gravitationally microlensed by a dark lens, the centroid of the source star image is displaced relative to the position of the unlensed source star, with an elliptical trajectory. Recently, routine astrometric follow-up measurements of these source star image centroid shifts by using high-precision interferometers have been proposed to measure the lens proper motion, which can resolve the lens parameter degeneracy in the photometrically determined Einstein time-scale. When an event is caused by a bright lens, on the other hand, the astrometric shift is affected by the light from the lens, but one cannot identify the existence of the bright lens from the observed trajectory because the resulting trajectory of the bright lens event is also an ellipse. As results, lensing parameters determined from the trajectory differ from those of a dark lens event, causing an incorrect identification of the lens population. In this paper, we show that although the shape and size of the astrometric centroid shift trajectory are changed because of the bright lens, the angular speed of centroid shifts around the apparent position of the unlensed source star is not affected by the lens brightness. Therefore, one can identify the existence of a bright lens and determine its brightness by comparing the lens parameters determined from the 'angular speed curve' with those determined from the trajectory of observed centroid shifts. Once the lens brightness is determined, one can correct for the lens proper motion. As the proposed method provides information about both the lens brightness (dark or bright) and the corrected values of the physical parameters of the lens, one can constrain the nature of massive compact halo objects (MACHOs) significantly better.