2019年沈阳一次凌晨气温骤升过程成因精细分析

2019年12月2日01时沈阳国家基本气象站(沈阳站)气温1 h内异常回升了6.5℃,利用常规和加密地面观测站实况、NCEP再分析及沈阳站逐小时风廓线雷达资料,从系统配置、热力学诊断、城市热岛效应等方面对此次异常升温事件成因进行精细分析。结果表明:沈阳站异常升温阶段,超低空到近地面暖脊过境造成辽宁大部分地区出现气温回升,暖脊过境是引发沈阳站午夜时分异常升温的原因之一;沈阳站位于沈阳市的东南部,当地面风为西北风时,风从温度相对较高的城区吹向郊区,造成沈阳南部郊区各站气温回升,与北部郊区对比得出升温幅度约为3—4℃。城市热岛中心向下风方漂移是沈阳站气温骤升又一原因。值得注意的是,气温回升前的温度基础值对气温回升幅度存在一定程度影响,回升前的基础温度越低,则回升后造成的升温幅度越大。     

深空摄影琐事谈

暗夜环境 深空天体大多数亮度不高,且有着丰富的色彩和细腻的层次,如果天空背景中存在着浓重的人工光源,那么细节上就会受到影响。所以深空摄影需要一个光污染弱、晴朗且高透明度、低湿度、基本生活有保障的地点,对绝大多数天文摄影的朋友来说,这却是个奢求。     

丽江观测站1.8米望远镜自适应光学系统性能初步理论估计

为了探讨丽江1.8 m自适应光学望远镜在天文或天体物理研究领域的可能应用,使用误差基本标度理论对其性能进行了初步的理论分析。结果表明,一般观测条件下,系统分辨力可以达到近似衍射极限。同时对在其上配置激光导星系统后可获得的性能进行了预测,结果表明,激光导星自适应光学系统将大幅度提高系统的天空覆盖率。     

利用青海湖水面辐射校正场对FY—1C气象卫星热红外传感器进行绝对辐射定标

利用青海湖水面场FY-1C气象卫星热红外窗区通道进行绝对辐射定标,由CE312野外热红外辐射计在水面测得辐亮度经大气订正传递到卫星入瞳处,考虑到大气吸收削弱影响,同时卫星观测路径大气产生热发散,这两部分对卫星信号的贡献由探空廓线和卫星观测几何输入MODTRAN37计算出来,同时进行CE312野外辐射计与卫星通道光谱响应匹配计算,最终得到卫星入瞳处的表观亮度.这个辐亮度与卫星通道的计数值比较得到该通道绝对定标系数.结果表明利用辐射校正场辐射定标与星上定标相差5%左右,相当于3K的亮温差.     

探宝梅西叶（4）

爱好者观测：M33的一大特点是弥散,表面亮度低,因此使用较小的放大倍率反而能取得非常好的观测效果,而若使用较大的放大倍率则难以看到它,即便你可以确定它就在你的视场内。在天气极好的情况下,M33可以用肉眼看见,若有～个小的双筒望远镜则可以看得更清楚;但如果使用中等口径以上的望远镜又不幸地用了一个高倍目镜,要看到它就不是一件容易的事情了。     

一种遥感图像信噪比评估和度量准则

对遥感图像信噪比的研究,能够很好地反映在轨运行的不同卫星遥感器辐射性能的变化与衰退情况。由于在轨成像环境的差异,如果直接比较不同遥感图像间的信噪比关系,将与实际结果产生较大分歧。通过对遥感图像进行图像块划分、匀值图像块选取以及图像灰度值与成像时传感器入瞳辐亮度的关系转换,提出一种遥感图像间信噪比的评估和度量准则,以进行不同遥感图像信噪比的比较,实现全自动的信噪比评估及度量。并对我国卫星传感器在不同时期所成图像信噪比的关系进行分析,验证该信噪比评估和度量准则的可靠性。     

月有阴晴圆缺——盈亏变化

月亮最引人注意的现象应该是它的盈亏变化了,古人很早就知道了月亮的这种奇妙的形态、亮度变化。并且发现这个变化有非常固定的周期,于是把这周期也称作“月”,成为后世历法的重要单位。     

Clustering Property of Wolf-Rayet Galaxies in the SDSS

We have analysed, for the first time, the clustering properties of Wolf-Rayet (W-R) galaxies, using a large sample of 846 W-R galaxies selected from the Data Release 4 (DR4) of the Sloan Digital Sky Survey (SDSS). We compute the cross-correlation function between W- R galaxies and a reference sample of galaxies drawn from the DR4. We compare the function to the results for control samples of non-W-R star-forming galaxies that are matched closely in redshift, luminosity, concentration, 4000-A break strength and specific star formation rate (SSFR). On scales larger than a few Mpc, W-R galaxies have almost the same clustering amplitude as the control samples, indicating that W-R galaxies and non-W-R control galax- ies populate dark matter haloes of similar masses. On scales between 0.1-1 h-1 Mpc, W-R galaxies are less clustered than the control samples, and the size of the difference depends on the SSFR. Based on both observational and theoretical considerations, we speculate that this negative bias can be interpreted by W-R galaxies residing preferentially at the centers of their dark matter haloes. We examine the distribution of W-R galaxies more closely using the SDSS galaxy group catalogue of Yang et al., and find that ～82% of our W-R galaxies are the central galaxies of groups, compared to ～74% for the corresponding control galaxies. We find that W-R galaxies are hosted, on average, by dark matter haloes of masses of 1012,3 M☉, compared to 1012,1 M? For centrally-located W-R galaxies and 1012,7 M☉ For satellite ones. We would like to point out that this finding, which provides a direct observational support to our conjecture, is really very crude due to the small number of W-R galaxies and the incom- pleteness of the group catalogue, and needs more work in future with larger samples.     

Comparison Between Four Methods for Data Fusion of ETM＋ Multispectral and Pan Images

Four data fusion methods, principle component transform (PCT), brovey transform (BT), smoothing filter-based intensity modulation(SFIM), and hue, saturation, intensity (HSI), are used to merge Landsat--7 ETMq- multispectral bands with ETM panchromatic band. Each of them improves the spatial resolution effectively but distorts the original spectral signatures to some extent. SFIM model can produce optimal fusion data with respect to preservation of spectral integrity. However, it results the most blurred and noisy image if the coregistration between the multispectral and pan images is not accurate enough. The spectral integrity for all methods is preserved better if the original multispectral images are within the spectral range of ETM pan image.