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321.
N. Kameswara Rao V. R. Venugopal A. R. Patnaik 《Journal of Astrophysics and Astronomy》1987,8(3):227-230
VLA observations at 6 cm have been obtained for three hydrogen-deficient objects υ Sgr, V 348 Sgr, and A bell 58. A bell 58
was also observed at 2 cm. Only upper limits to the flux density could be set for these sources. A new radio source at 6 cm
was found in the field of υ Sgr.
The upper limit for 6 cm flux density of V348 Sgr sets an upper limit to its reddening asE(B–V) ≤ 0.65. The hydrogen deficient planetary nebula A 58 shows much lower radio flux than expected from the infrared-radio flux
density relationship of planetary nebulae.
National Radio Astronomy Observatory’s Very Large Array is operated by Associated Universities Inc. under contract with National
Science Foundation, USA. 相似文献
322.
数字地图生产流程中质量的数据控制 总被引:1,自引:0,他引:1
高晓梅 《地球信息科学学报》2001,3(4):53-56
本文将着重讨论在ISO9001质量控制体系下、数字地图生产流程中影响地图质量的各类数据文件的设定与控制,从而进一步探讨在电子出版系统及CTP系统中,数字地图生产规范化、标准化、程序化作业的质量控制内容及方法。 相似文献
323.
Mark A. Bishop 《Icarus》2007,191(1):151-157
The geographic signature of dune distribution and self-organization as measured by the R-statistic offers a viewpoint on the geography of crescentic eolian systems and proposes an index from which to determine the degree of self-organization across a variety of spatial scales. Fields of simple dunes (dome, barchan, barchan-seif) are comparatively less regular in distribution than are those fields, or part thereof, that consist of compound (barchanoid) morphologies whose patterns are more highly regular. 相似文献
324.
GPS/LEO掩星技术中超折射效应的修正 总被引:4,自引:3,他引:1
在GPS掩星探测地球大气技术中,Abel积分变换要求大气折射指数n是折射半径a的单值函数,当大气折射率的垂直梯度达到小于一个极限值dN/dr≈-0.16N-unit m^-1上述单值性不成立,称其为超折射,此时Abel积分变换不再适用,如果还是在形式上应用经典的Abel变换,在反演结果中就会产生负大气折射率偏差.描述了低对流层中超折射现象的物理特性和数学表示;在广义Abel积分变换的基础上,讨论了超折射层内和超折射层下的大气剖面反演算法;选择了一个简单的采样间隔内等大气折射率垂直梯度假设,对英国高分辨率无线电探空观测资料进行模拟计算,验证了负超折射与大气折射率偏差的关系,并提出的广义Abel变换的合理性. 相似文献
325.
N.I. Rovenskaya 《Astrophysics and Space Science》2004,293(3):355-362
The density matrix equations of highly excited carbon are analytically solved as functions of line number and temperature.
Allowing for the series of the impact approximation theory and quadrupole interaction potential, the line widths are found
with the theoretical error less than 0.06 in the range of temperatures T
e = 25 − 100 K. To determine the medium temperature and density by using the experimental values of line widths, the Doppler,
radiational and impact broadening are calculated for the lines with the principal quantum numbers n > 300.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
326.
327.
For the rising branch of Cycle 22, 1987 January—1989 November, we plot the daily total flux S at each of the five wavelengths 2.0, 3.4, 6.0, 10.7 and 21.2 cm against the apparent sunspot area of the dominant sunspot Ay and find that, for several large active areas, the locus is located below the average regression line, and the increase in the radio flux is insignificant compared to the increase in the sunspot area. 相似文献
328.
GPS无线电掩星技术能提供高精度、高分辨率、全球覆盖的地球电离层和中性层大气剖面。它具有全天候、低费用、无系统长期漂移等优点。从1995年4月至1997年3月,首次GPS/MET试验的成功显示了GPS掩星技术对监测全球大气能够发挥重要的作用,从而成为当前空间探测技术的研究热点之一。该文主要叙述了无线电掩星技术的数据处理系统的有关情况,并介绍了美国UCAR的掩星数据处理系统CDAAC的概况,可作为我国开展无线电掩星计划有关工作的借鉴。 相似文献
329.
R. Soria R. P. Fender D. C. Hannikainen A. M. Read I. R. Stevens 《Monthly notices of the Royal Astronomical Society》2006,368(4):1527-1539
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. 相似文献
330.
Steven R. Furlanetto 《Monthly notices of the Royal Astronomical Society》2006,370(4):1867-1875
We examine the prospects for studying the pre-reionization intergalactic medium (IGM) through the so-called 21-cm forest in spectra of bright high-redshift radio sources. We first compute the evolution of the mean optical depth τ for models that include X-ray heating of the IGM gas, Wouthuysen–Field coupling, and reionization. Under most circumstances, the spin temperature T S grows large well before reionization begins in earnest; this occurs so long as the X-ray luminosity of high-redshift starbursts (per unit star formation rate) is comparable to that in nearby galaxies. As a result, τ≲ 10−3 throughout most of reionization, and background sources must sit well beyond the reionization surface in order to experience absorption that is measurable by square-kilometre class telescopes. H ii regions produce relatively large 'transmission gaps' and may therefore still be observable during the early stages of reionization. Absorption from sheets and filaments in the cosmic web fades once T S becomes large and should be rare during reionization. Minihaloes can produce strong (albeit narrow) absorption features. Measuring their abundance would yield useful limits on the strength of feedback processes in the IGM as well as their effect on reionization. 相似文献