Relative Velocities and Linewidths in a Coronal Hole and Outside     

K. P. Raju 《Solar physics》2009,255(1):119-129

Relative Doppler velocities and spectral linewidths in a coronal hole and in the quiet Sun region outside have been obtained from Solar and Heliospheric Observatory (SOHO)/Coronal Diagnostic Spectrometer (CDS) observations. Five strong emission lines in the CDS wavelength range (namely, O? iii 599 Å, O?v 630 Å, Ne?vi 562.8 Å, He?ii 304 Å, and Mg?ix 368 Å), whose formation temperatures represent different heights in the solar atmosphere from the lower transition region to the inner corona, have been used in the study. As reported earlier, relative velocities in the coronal hole are generally blueshifted with respect to the quiet Sun, and the magnitude of the blueshifts increases with height. It has been found that the polar coronal hole has larger relative velocities than the equatorial extension in the inner corona. Several localized velocity contours have been found mainly on network brightenings and in the vicinity of the coronal hole boundary. The presence of velocity contours on the network may represent network outflows whereas the latter could be due to localized jets probably arising from magnetic reconnection at the boundary. All spectral lines have larger widths in the coronal hole than in the quiet Sun. In O?v 630 Å an extended low-linewidth region is seen in the coronal hole?–?quiet Sun boundary, which may indicate fresh mass transfer across the boundary. Also polar coronal holes have larger linewidths in comparison with the equatorial extension. Together with larger relative velocities, this suggests that the solar wind emanating from polar hole regions is faster than that from equatorial hole regions.  相似文献   

Electron Densities in Quiescent Prominences Derived from Eclipse Observations     

S. Jejčič  P. Heinzel 《Solar physics》2009,254(1):89-100

We develop a diagnostic tool for determination of the electron densities in solar prominences using eclipse data. The method is based on analysis of the hydrogen Balmer-line intensities (namely Hα and Hβ) and the white-light emission due to Thomson scattering on the prominence electrons. Our approach represents a generalization of the ratio method already used by Koutchmy, Lebecq, and Stellmacher (Astron. Astrophys. 119, 261, 1983). In this paper we use an extended grid of non-LTE prominence models of Gouttebroze, Heinzel, and Vial (Astron. Astrophys. Suppl. Ser. 99, 513, 1993) and derive various useful relations between prominence radiation properties and electron densities. Simultaneously, an effective geometrical thickness of the prominence can also be obtained. As an example we apply our general technique to original eclipse data of Koutchmy, Lebecq, and Stellmacher (Astron. Astrophys. 119, 261, 1983). Finally, we use our results to determine the color of prominences as it should be seen during total eclipses.  相似文献   

冬季蒙古高压的时空变化和突变特征研究   总被引：5，自引：0，他引：5       下载免费PDF全文

王力群  李崇银-  谭言科  严冬 《高原气象》2010,29(1):23-32

利用Hadley中心的155年全球月平均海平面气压资料(1850年1月—2004年12月),研究了冬季蒙古高压的振荡周期和突变特征。在定义冬季蒙古高压指数的基础上,通过EOF展开,分析了冬季北半球海平面气压的时空变率分布;应用奇异谱分析的方法重建了冬季蒙古高压主要周期振荡序列,并着重分析其年际和年代际变化特征。根据Mann-Kendall气候突变检测法,检测了冬季蒙古高压存在的气候突变点。研究表明:冬季蒙古高压具有显著的年际和年代际变化,主要存在准两年和3～4年的年际变化周期,以及13～14年、20～21年和35～36年的年代际变化周期,而且准两年周期的振幅也存在显著的年代际变化;蒙古高压20～21年的周期与阿留申低压变化的位相不甚一致,35～36年的周期与阿留申低压变化的位相极为相似。经突变检测,发现冬季蒙古高压在1927年前后为明显的气候突变点。  相似文献   

0.1~40 MHz地闪、 云闪及NBE事件的辐射场频谱特征分析          下载免费PDF全文

蓝渝  张义军  吕伟涛  郑栋  陈绍东 《高原气象》2009,28(5):1025-1033

利用宽带傅立叶分析法对2008年7月30日和8月4日两次雷暴过程中, 距离观测点5~20 km范围内的55次负地闪回击过程, 33次云内闪电过程以及20次双极性窄脉冲事件（NBE）的电磁辐射信号进行了观测分析, 得到地闪回击、 云闪放电初始阶段以及双极性窄脉冲事件在0.1~40 MHz频带宽度下的电磁辐射能量谱密度。结果表明, 这三类闪电放电过程的辐射频谱波形均呈现出随频率增加、 幅值减小的趋势, 但在辐射强度和衰减速率上存在一定的差异。负地闪回击幅频波形在6~28 MHz频段上衰减速率相对缓慢; 云闪初始阶段在全频带上始终遵循f-1.2~f-1.4之间的衰减率递减, 且其频谱幅值与地闪回击的辐射能量谱幅值相差不大; NBE事件在0.1~40 MHz频带中辐射能量谱幅值基本都明显大于其他两类闪电放电过程, 特别是在10 MHz以上的HF、 VHF频带上其差异可达到20 dB。  相似文献   

The far-ultraviolet albedo of Šteins measured with Rosetta-ALICE     

Michael F. A’Hearn  Lori M. Feaga 《Planetary and Space Science》2010,58(9):1088-1096

During Rosetta’s flyby of the asteroid (2867) Šteins in 2008, we used the ALICE instrument to measure the first far-ultraviolet (FUV) reflectivity spectrum of an asteroid (850-2000 Å). It is very dark in the FUV, ∼4%, compared to its very high reflectivity (40%) at optical wavelengths. The FUV albedo does not exhibit a systematic color trend across the spectral range, but there is a broad absorption feature, not yet identified with a specific mineral, with maximum depth near 1650 Å. The shape of this feature implies a very low abundance of Fe²⁺ ions in the surface minerals. The FUV brightness exhibits a significant opposition surge at phases below 10°. The visible/FUV color gets much redder with increasing phase angle inside the opposition surge and gets gradually redder at larger phase angles. We also conducted a deep search for an exosphere of atoms sputtered from the surface and set upper limits on any column densities of oxygen and hydrogen atoms at the time of our observations. The upper limit for H is comparable to that predicted by the only theoretical prediction of which we are aware, while that for O is higher than predicted by about an order of magnitude.  相似文献   

基于多相滤波器的宽带射电频谱仪设计     

陈林杰  颜毅华  刘飞  王威 《天文研究与技术》2010,7(2)

提出了一种基于多相滤波器的新型宽带射电频谱仪的设计方案。通过多相滤波器实现宽带射电信号的滤波,对滤波后的基带信号进行数字功率检波,再通过积分控制,最终得到射电信号的频谱强度。仿真分析表明,这一设计具有很好的效果,通过多相滤波器,使信号的速率大为降低,克服了传统频谱仪以及采用FFT实现频谱变换方法的缺点,可以实现对超宽带射电信号的实时频谱分析。  相似文献   

瑞利波测试技术用于剪切波速勘探之研究     

石玉成  蔡红卫 《高原地震》1995,(3)

本文根据瑞利波测量所得波形的变化特征，分析研究了地基参数对瑞利波弥散曲线的影响规律，提出了利用瑞利波测试剪切波速的方法。在研究过程中，对瑞利波测试技术进行了探讨，并引入了相关分析原理，以消除噪声、系统的非线性以及其它一些人为因素的干扰。最后结合实例，论证该技术用于实际勘探的可行性并指出其存在的问题和有待进一步完善的工作。  相似文献   

1982年6月12日耀斑的巴耳末线半宽特征     

胡菊 《地球物理学进展》1999,14(Z1):2