新疆库车盆地钾盐科探1井含盐系地球化学特征及找钾指示

在盐湖沉积演化过程中,钾盐矿物在盐类沉积的中晚期阶段才开始析出。因此,研究含盐系盐类的沉积地球化学特征,不仅可以从侧面获取岩盐的沉积物源和成盐古卤水蒸发浓缩程度等地球化学信息,而且更能揭示古盐湖钾盐富集趋势。文章通过对库车盆地钾盐科探1井钻取的岩芯样品进行高精度采样测试,得出岩盐中Mg×103/Cl、K×103/Cl、Li×103/Cl与K+、Mg2+、Li+、Ca2+、Cl-含量的垂向变化规律。并与库车盆地其他钻孔中的岩盐含钾性进行对比,同时,依据钻井剖面岩性特征,与潜江凹陷和大汶口凹陷含盐系剖面进行对比,论述研究区成盐的地球化学特征,对其钾盐成矿前景进行分析和评价。     

几种天绘一号卫星影像分割方法及质量评价

为寻求更适合天绘一号卫星影像的分割方法,文章采用均值偏移分割、分水岭分割、数学形态学分割、连通分量分割4种图像分割方法对天绘一号卫星影像进行分割实验,并从视觉和定量两方面对分割结果进行评估.结果表明:均值偏移方法的分割质量更佳,且分割结果更有利于提升后续处理的效率;几何形态较规则、质地较均一、复杂度较低的地物类型分割质量较高,反之则较低.     

New limits on the orbital parameters of 1E 1048.1–5937 and 1E 2259+586 from RXTE observations

We report on two Rossi X-ray Timing Explorer ( RXTE ) observations of the anomalous X-ray pulsars 1E 1048.1–5937 and 1E 2259+586. Both sources have continued their almost constant spin-down during 1995/96. We carried out a search for orbital Doppler shifts, in their observed spin frequencies, deriving stringent limits on the projected semi-axis. Unless these systems have unlikely small inclinations, main-sequence companions can be excluded. If 1E 1048.1–5937 and 1E 2259+586 are indeed binary systems, their companion stars must be either white dwarfs, or helium-burning stars with M ≲ 0.8 M⊙, possibly underfilling their Roche lobe.     

基于压缩感知原理的L1范数AVO反演算法

基于压缩感知稀疏信号采样与重构理论,利用AVO反演方法将传统的L2范数改变为L1范数,反演地下地层在L1范数下的稀疏脉冲反射系数。反演得到的稀疏尖峰将局部地下结构通过有限数量的层状结构的叠加来表示,能够提高纵向精度,与传统的AVO反演算法相比提高了薄层的反演效果且具有一定的抗噪性。数值模型及实际数据的结果表明,基于压缩感知原理的L1范数AVO反演方法更加准确、分辨率更高。     

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Chandra observations of Comet 9P/Tempel 1 during the Deep Impact campaign

We present results from the Chandra X-ray Observatory's extensive campaign studying Comet 9P/Tempel 1 (T1) in support of NASA's Deep Impact (DI) mission. T1 was observed for ∼295 ks between 30th June and 24th July 2005, and continuously for ∼64 ks on July 4th during the impact event. X-ray emission qualitatively similar to that observed for the collisionally thin Comet 2P/Encke system [Lisse, C.M., Christian, D.J., Dennerl, K., Wolk, S.J., Bodewits, D., Hoekstra, R., Combi, M.R., Mäkinen, T., Dryer, M., Fry, C.D., Weaver, H., 2005b. Astrophys. J. 635 (2005) 1329-1347] was found, with emission morphology centered on the nucleus and emission lines due to C, N, O, and Ne solar wind minor ions. The comet was relatively faint on July 4th, and the total increase in X-ray flux due to the Deep Impact event was small, ∼20% of the immediate pre-impact value, consistent with estimates that the total coma neutral gas release due to the impact was 5×¹⁰⁶ kg (∼10 h of normal emission). No obvious prompt X-ray flash due to the impact was seen. Extension of the emission in the direction of outflow of the ejecta was observed, suggesting the presence of continued outgassing of this material. Variable spectral features due to changing solar wind flux densities and charge states were clearly seen. Two peaks, much stronger than the man-made increase due to Deep Impact, were found in the observed X-rays on June 30th and July 8th, 2005, and are coincident with increases in the solar wind flux arriving at the comet. Modeling of the Chandra data using observed gas production rates and ACE solar wind ion fluxes with a CXE mechanism for the emission is consistent, overall, with the temporal and spectral behavior expected for a slow, hot wind typical of low latitude emission from the solar corona interacting with the comet's neutral coma, with intermittent impulsive events due to solar flares and coronal mass ejections.     

An ultraluminous X-ray microquasar in NGC 5408?

We studied the radio source associated with the ultraluminous X-ray source in NGC 5408  ( L _X≈ 10⁴⁰ erg s⁻¹)  . The radio spectrum is steep (index  ≈−1  ), consistent with optically thin synchrotron emission, not with flat-spectrum core emission. Its flux density (≈0.28 mJy at 4.8 GHz, at a distance of 4.8 Mpc) was the same in the March 2000 and December 2004 observations, suggesting steady emission rather than a transient outburst. However, it is orders of magnitude higher than expected from steady jets in stellar-mass microquasar. Based on its radio flux and spectral index, we suggest that the radio source is either an unusually bright supernova remnant, or, more likely, a radio lobe powered by a jet from the black hole (BH). Moreover, there is speculative evidence that the source is marginally resolved with a radius ∼30 pc. A faint H  ii region of similar size appears to coincide with the radio and X-ray sources, but its ionization mechanism remains unclear. Using a self-similar solution for the expansion of a jet-powered electron–positron plasma bubble, in the minimum-energy approximation, we show that the observed flux and (speculative) size are consistent with an average jet power  ≈ 7 × 10³⁸ erg s⁻¹∼ 0.1 L _X∼ 0.1 L _Edd  , an age ≈10⁵ yr, a current velocity of expansion ≈80 km s⁻¹. We briefly discuss the importance of this source as a key to understand the balance between luminosity and jet power in accreting BHs.