新疆谢米斯台地区小岩体型矿化遥感探测

中酸性小岩体易被地质填图遗漏,严重制约了该类型矿化的发现。在新疆西准噶尔谢米斯台地区找矿工作中,首先利用ETM+数据进行小岩体扫面,进而选取重点区采用ETM+和中巴资源卫星02B HR数据进行分辨率融合后解译、识别中酸性小岩体,并利用主成分分析法提取蚀变遥感异常,结合地质、化探信息综合分析后确定重点检查区域。利用此方法共解译出14个钾质花岗岩和3个黑云母花岗岩小岩体,这些小岩体大多被野外检查所证实。经野外检查发现了5处铜、金矿化点,证实了该方法的有效性。本研究中采用的方法可以为西部地区地质填图和中酸性小岩体型矿产资源勘查提供借鉴。     

Variation of the 0+ ion density during low and high solar activity as measured by the SR0SS-C2 satellite

The O⁺ ion density measured by the SROSS-C2 satellite during solar minima (year 1995, F_10.7 = 77) and maxima (year 2000, F_10.7 = 181) has been analyzed for studying diurnal, seasonal, latitudinal and geomagnetic variations. The study region covers an area encompassed between 5-3 5° N latitude and 65-95° E longitude over India at a ~500 km altitude (F2 region). The year 2000 shows significant enhancement in the annual average of O⁺ ion density and attainment of post sunset secondary enhancement compared to 1995. Attributed to photoionization, daytime shows a maximum ionization compared to nighttime. However, attainment of post sunset secondary maxima is attributed to the strong pre-reversal enhancement in the vertical E x B drift. The effect of geomagnetic activity Kp through the E x B drift dynamic movement on O⁺ ion density distribution studies indicates periodicities of seven and nine days in 1995 and 2000, respectively, and polynomial dependency of the O⁺ ion density on geomagnetic activity Kp. Further on, stratification of the O⁺ ion density according to latitude (5-35° N) indicates high density in mid-latitudes (12-24° N) compared to high and low latitudes, except in the winter of 1995, which shows a distinct trend (i.e., density decreases with increasing latitude).     

“智慧利民”数字开发区建设及实际应用

＂数字开发区＂的理念就是把开发区作为一个生态系统,其中的居民、交通、能源、商业、通信、水资源等构成一个整体,各部分相互联系、彼此影响。本文简要介绍了＂智慧利民＂数字开发区建设及实际应用情况。     

Optical spectroscopy of the radio pulsar PSR B0656+14

We have obtained the spectrum of a middle-aged PSR B0656+14 in the 4300–9000 Å range with the ESO/VLT/FORS2. Preliminary results show that at 4600–7000 Å the spectrum is almost featureless and flat with a spectral index α _ν ??0.2 that undergoes a change to a positive value at longer wavelengths. Combining with available multiwavelength data suggests two wide, red and blue, flux depressions whose frequency ratio is about 2 and which could be the 1st and 2nd harmonics of electron/positron cyclotron absorption formed at magnetic fields ～10⁸ G in upper magnetosphere of the pulsar.     

Hubble Space Telescope imaging of the progenitor sites of six nearby core-collapse supernovae

The search for the progenitors of six core-collapse supernovae (CCSNe) in archival Hubble Space Telescope ( HST ) WFPC2 pre-explosion imaging is presented. These SNe are 1999an, 1999br, 1999ev, 2000ds, 2000ew and 2001B. Post-explosion imaging of the SNe, with the HST ACS/WFC, has been utilized with the technique of differential astrometry to identify the progenitor locations on the pre-explosion imaging. SNe 1999br, 1999ev, 2000ew and 2001B are recovered in late-time imaging, and estimates of the progenitor locations on the pre-explosion imaging, with subpixel accuracy, have been made. Only the progenitor of the Type II-P SN 1999ev has been recovered, on pre-explosion F555W imaging, at a 4.8σ significance level. Assuming a red supergiant progenitor, the pre-explosion observation is consistent with   M _ZAMS= 15–18 M_⊙  . The progenitors of the other five SNe were below the 3σ detection threshold of the pre-explosion observations. The detection thresholds were translated to mass limits for the progenitors by comparison with stellar evolution models. Pre-explosion observations of the peculiarly faint SN 1999br limit the mass of a red supergiant progenitor to   M _ZAMS < 12 M_⊙  . Analysis has been extended, from previous studies, to include possible detections of high- T _eff, high-mass stars by conducting synthetic photometry of model Wolf–Rayet star spectra. The mass limits for the Type II-P SNe 1999an and 1999br are consistent with previously determined mass limits for this type of SN. The detection limits for the progenitors of the Type Ibc SNe (2000ds, 2000ew and 2001B) do not permit differentiation between high-mass Wolf–Rayet progenitors or low-mass progenitors in binaries.