Simultaneous optical polarimetry and X-ray observations of the magnetic CV CP Tuc (AX J2315−592)

CP Tuc (AX J2315–592) shows a dip in X-rays which lasts for approximately half the binary orbit and is deeper in soft X-rays compared with hard X-rays. It has been proposed that this dip is due to the accretion stream obscuring the accretion region from view. If CP Tuc were a polar, as has been suggested, then the length of such a dip would make it unique amongst polars since in those polars in which a dip is seen in hard X-rays the dip lasts for only 0.1 of the orbit. We present optical polarimetry and RXTE observations of CP Tuc which show circular polarization levels of ∼10 per cent and find evidence for only one photometric period. These data confirm CP Tuc as a polar. Our modelling of the polarization data implies that the X-ray dip is due to the bulk of the primary accretion region being self-eclipsed by the white dwarf. The energy dependence of the dip is due to a combination of this self-eclipse and also the presence of an X-ray temperature gradient over the primary accretion region.     

IERS1996规范中地球引力势模型和测量模型的改进

简要而系统地介绍ＩＥＲＳ１９９６规范采用的地球引力势模型和各种测量模型,着重叙述了其与ＩＥＲＳ１９９２标准相比所作的改进。规范用ＪＧＭ－３地球引力势模型取代ＧＥＭ－Ｔ３模型,在计算地球潮汐形变产生的附加势时展开到３阶,并考虑了地幔的滞弹效应。在测站位移的计算中,规范引入了３倍洛夫数,计及地幔的滞弹性,引入了计算冰后期回弹的ＩＣＥ－４Ｇ模型,列出了改正ＶＬＢＩ观测中天线形变改正的公式。关于地球自转和     

银河系化学演化研究进展

银河系的形成与演化是天体物理学研究的重大前沿课题,银河系的化学演化在其中更具有极其重要的地位。随着观测资料的不断积累和理论工作的不断深入,银河系化学演化的研究取得了一系列进展。在观测方面,从太阳附近区域,整个银盘,银晕和核球等方面简要回顾了银河系化学演化模型主要观测约束的近期结果;在化学演化模型方面,回顾了银河系化学演化研究的发展历程和近期进展,并对未来的研究进行了展望。     

The ages of pre-main-sequence stars

The position of pre-main-sequence or protostars in the Hertzsprung–Russell diagram is often used to determine their mass and age by comparison with pre-main-sequence evolution tracks. On the assumption that the stellar models are accurate, we demonstrate that, if the metallicity is known, the mass obtained is a good estimate. However, the age determination can be very misleading, because it is significantly (generally different by a factor of 2 to 5) dependent on the accretion rate and, for ages less than about 10⁶ yr, the initial state of the star. We present a number of accreting protostellar tracks that can be used to determine age if the initial conditions can be determined and the underlying accretion rate has been constant in the past. Because of the balance established between the Kelvin–Helmholtz, contraction time-scale and the accretion time-scale, a pre-main-sequence star remembers its accretion history. Knowledge of the current accretion rate, together with an HR-diagram position, gives information about the rate of accretion in the past, but does not necessarily improve any age estimate. We do not claim that ages obtained by comparison with these particular accreting tracks are likely to be any more reliable than those from comparisons with non-accreting tracks. Instead, we stress the unreliability of any such comparisons, and use the disparities between various tracks to estimate the likely errors in age and mass estimates. We also show how a set of coeval accreting objects do not appear coeval when compared with non-accreting tracks. Instead, accreting pre-main-sequence stars of around a solar mass are likely to appear older than those of either smaller or larger mass.     

Differential astrometry over 15°

We observed the pair of radio sources 1150+812 and 1803+784 in November 1993 with a VLBI array, simultaneously recording at 8.4 and 2.3 GHz. We determined the angular separation between the two sources with submilliarcsecond accuracy by using differential techniques. This result demonstrates the feasibility of high precision differential astrometry for radio sources separated in the sky by almost 15°, and opens the avenue to its application to larger samples of radio sources.     

论CILa/CISm—CILa图解

通过对分离结晶作用和批式熔融作用C_l^y/C_l^x-C_l^y图解的数学分析,笔者认为,虽然C_l^La/C_l^sm-C_l^La图解在一定程度上能区分这两种不同岩浆作用过程,但是,Treuil等的解释是不完全的。直线的斜率和截距还极大地受参数C_o^x,C_o^y,D_x,D_y的影响。该图解并非总是有效。本文还给出了一般式C_l^y/C_l^x-C_l^y在其它方面的可能应用。     

早白垩世掘足类Dentalium属在我国首次发现

本文记述的掘足类（Scaphopods）系我国首次报道,化石产自西藏南部聂拉木县古错村北山下白垩统古错Ⅱ组中。计1属2种Dentalium jeffereysi Gardner,D.gucuoensis（sp.nov.）.     

大珠母贝Pinctada maxima(Jameson)亲贝人工促熟培育与诱导排放精卵的研究

用亚心形扁藻Platymonassubcoriformis,湛江等鞭藻Isochrysiszhanjiangensis及某些配合饲料培育大珠母贝pinctadamaxima(Jameson)亲贝,可以促进性腺发育成熟并保持易于诱导排放状态。在需要进行人工育苗时,给亲贝以一定的刺激,即可诱导产卵排精。采用这种方法进行大珠母贝人工育苗,受精率和活率都比剖贝取卵授精的方法高。而且不用杀死大珠母贝亲贝。     

概略坐标对GPS PWV解算的影响

利用GAMIT 10.6和2016年第101天至第160天南昌站的GPS观测资料,开展了13组概略坐标变化对GPS PWV解算的影响研究试验(南昌站概略坐标设置以10 m等间距从0~120 m逐渐向西偏移真实坐标)。其结果发现:当概略坐标与实际坐标偏离在60 m以内时,概略坐标的变化对GPSPWV的解算影响不大(长基线的相对误差和均方根残差NRMS分别维持在5.7×10~(-9)和0.24附近);但当概略坐标与真实坐标偏离超过60 m后,概略坐标的变化对GPS PWV的解算有着显著的影响,其中基线相对误差和GPS PWV与探空PWV的标准偏差随概略坐标偏离的增加而快速增大,NRMS和GPS PWV与探空PWV的相关系数也有明显的增加和减小,GPSPWV的成功解算日数则随概略坐标偏离的增加而快速减小(当偏离≥120 m时南昌无GPS PWV生成);概略坐标变化对基线相对误差、GPS PWV精度以及GPS PWV能否被成功解算的影响仅限于本站,某站概略坐标的偏离不会对其他站GPS PWV解算造成明显的影响。