基于笛卡尔坐标的卫星地影模型解析

卫星地影的精确计算对于卫星的电源设计、定轨和定姿等方面具有重要意义。本文通过基于地心的笛卡尔坐标系,从向量的角度描述了日、地、卫之间的几何关系,针对不同轨道高度的卫星分别利用圆柱形模型和圆锥形模型对其进出地影的时间和位置进行了解算和分析,同时给出了圆锥形模型的计算程序。     

黑臭水体水面阴影提取的自适应阈值算法研究

黑臭水体水面阴影对水面光谱信息产生干扰,严重地影响了利用高空间分辨率遥感数据进行水质状况监测的精度,因此,在数据预处理中必须进行阴影剔除。本研究基于无人机高光谱遥感数据,通过分析各种波段组合下黑臭水体水面的阴影像元和水体像元的光谱特征空间,选择以492、666和792 nm处的反射率建立黑臭水体的河面阴影指数（RSSI）,并利用最大类间方差法（OTSU）自动确定划分本影、半影以及水体的阈值。利用南京金川河和龙江河的无人机高光谱遥感影像对算法进行测试,结果表明：RSSI阴影指数能突出显示阴影与水体的差异;OTSU自适应确定的阈值能较好地区分本影、半影和水体,阴影的总体识别精度达到85%以上。该算法能够有效地识别黑臭水体水面阴影,为后续开展水体的定性、定量遥感监测提供数据预处理的技术支持。     

Identification of SrF molecular lines in the spectrum of sunspot umbra

A high resolution spectrum of a sunspot umbra is used for identification of rotational lines due to (0, 0) band of the A ²Π–X ²Σ⁺ system and (0, 0), (1, 1), and (2, 2) bands of the B ²Σ⁺–X ²Σ⁺ system of the molecule SrF. The published sunspot umbral spectrum obtained with Fourier Transform Spectrometer and solar telescope of National Solar Observatory/National Optical Astronomy Observatory at Kitt Peak was used for the study. The new identification of more than 200 SrF lines in the umbral spectrum confirms that this molecule accounts for the majority of lines in the spectral range 15050 to 15360 cm⁻¹ and 17240 to 17300 cm⁻¹. Equivalent widths have been measured for well-resolved lines of these bands and the effective rotational temperatures have been estimated for which the presence is confirmed.     

The rotational temperatures of Silicon hydride isotopomer lines in sunspot umbrae

The published sunspot spectrum obtained with National Solar Observatory/Kitt Peak laboratory’s high signal to noise ratio telescope and high resolution Fourier Transform Spectrometer were used for the study. A search was made for the prominent lines of the (0, 0) and (1, 1) A²Δ − X²Π for Silicon hydride isotopomers which lie between 23500 cm⁻¹ and 24500 cm⁻¹. The presence of lines from the (0, 0) and (1, 1) A²Δ − X²Π transition of SiH molecule coincided with the sunspot umbral lines suggest that Silicon hydride appears to be a non-negligible component of sunspot umbrae. However, the presence of A²Δ − X²Π (0, 0) and (1, 1) bands of SiD was found to be doubtful because of the lack of number of well identified lines in sunspot umbral spectra. Equivalent widths have been measured for well-resolved lines and, thereby, the rotational temperatures have been estimated for the band systems for which the presence is confirmed.     

Search for magnetic field oscillations in a sunspot umbra

In order to search for oscillations in velocity and magnetic field strength within a sunspot umbra, a time series of spectra has been obtained through a circular analyzer and the Gregory-Coudé telescope at the Observatorio del Teide, Tenerife. The velocity oscillations clearly show peaks of power at periods between 2 and 7 minutes, with a maximum at 5 minutes. The apparent variations of the magnetic field strength, however, don't exhibit significant oscillations; these fluctuations are rather produced by the influence of parasitic stray light from the surrouding quiet sun which are also visible in the measured time variations of the umbral contrast of continuum intensity.