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1.
山东惠民凹陷古近系湖泊地震涌浪记录的新发现 总被引：4，自引：4，他引：4
在陆相湖盆中,地震引起的各种作用力可以对各种先成沉积物进行改造而形成原地震积岩,同样地震可引发涌浪、浊流及碎屑流而形成地震涌浪沉积及震浊积岩.通过大量岩心观察描述和成像测井资料分析,首次提出惠民凹陷中央隆起带沙河街组含有丘状交错层理的碎屑岩与典型的原地震积岩(包括震裂岩、震褶岩、自碎屑角砾岩等)紧密共生,当属于地震作用引发涌浪的沉积产物.本区地震涌浪沉积中发育丘状及洼状层理、包卷层理、平行层理、块状层理、波痕、冲刷及截切面等沉积构造.根据沉积特征和分布位置,本区地震涌浪沉积划分为两种类型,即位于涌浪基面附近的含塑性泥砾的搅动型和涌浪基面与正常浪基面之间的回流型.垂向上地震涌浪沉积一般位于原地震积岩之上,震浊积岩之下,组成完整的原地震积岩—地震涌浪沉积—地震浊积岩序列或原地震积岩—地震涌浪沉积序列.本区地震涌浪沉积的发现和研究,将为地质学家识别陆相湖盆地震事件沉积提供对比标准. 相似文献
2.
Bruce T. Tsurutani Bruce E. Goldstein Alexander Bratenahl 《Planetary and Space Science》1976,24(10):995-999
High energy particles, with energies above those attainable by adiabatic or steady-state electric field acceleration, have been observed in and around the outer regions of planetary magnetospheres. Acceleration by large amplitude sporadic cross-tail electric fields over an order of magnitude greater than steady-state convection fields is proposed as a source of these particles. It is suggested that such explosive electric fields will occur intermittently in the vicinity of the tail neutral line in the expansive phases of substorms. We use laboratory Double Inverse Pinch Device (DIPD) and satellite evidence to estimate this electric potential for substorms at Earth; values of 500 kV to 2 MV are calculated, in agreement with particle observations. It is further suggested that these particles, which have been accelerated in the night side magnetosphere, drift to the dayside on closed field lines, and under certain interplanetary conditions can escape to regions upstream of the bow shock. 相似文献
3.
Thomas N. Woods Phillip C. Chamberlin W. K. Peterson R. R. Meier Phil G. Richards Douglas J. Strickland Gang Lu Liying Qian Stanley C. Solomon B. A. Iijima A. J. Mannucci B. T. Tsurutani 《Solar physics》2008,250(2):235-267
Solar soft X-ray (XUV) radiation is highly variable on all time scales and strongly affects Earth’s ionosphere and upper atmosphere;
consequently, the solar XUV irradiance is important for atmospheric studies and for space weather applications. Although there
have been several recent measurements of the solar XUV irradiance, detailed understanding of the solar XUV irradiance, especially
its variability during flares, has been hampered by the broad bands measured in the XUV range. In particular, the simple conversion
of the XUV photometer signal into irradiance, in which a static solar spectrum is assumed, overestimates the flare variations
by more than a factor of two as compared to the atmospheric response to the flares. To address this deficiency in the simple
conversion, an improved algorithm using CHIANTI spectral models has been developed to process the XUV Photometer System (XPS)
measurements with its broadband photometers. Model spectra representative of quiet Sun, active region, and flares are combined
to match the signals from the XPS and produce spectra from 0.1 to 40 nm in 0.1-nm intervals for the XPS Level 4 data product.
The two XPS instruments are aboard NASA’s Solar Radiation and Climate Experiment (SORCE) and Thermosphere, Ionosphere, Mesosphere, Energetics, and Dynamics (TIMED) satellites. In addition, the XPS responsivities have been updated for the latest XPS data processing version. The
new XPS results are consistent with daily variations from the previous simple conversion technique used for XPS and are also
consistent with spectral measurements made at wavelengths longer than 27 nm. Most importantly, the XPS flare variations are
reduced by factors of 2 – 4 at wavelengths shorter than 14 nm and are more consistent, for the first time, with atmospheric
response to solar flares. Along with the details of the new XPS algorithm, several comparisons to dayglow and photoelectron
measurements and model results are also presented to help verify the accuracy of the new XUV irradiance spectra. 相似文献
4.
We study the interplanetary features and concomitant geomagnetic activity of the two high-speed streams (HSSs) selected by the Whole Heliosphere Interval (WHI) campaign participants: 20 March to 16 April 2008 in Carrington rotation (CR) 2068. This interval was chosen to perform a comprehensive study of HSSs and their geoeffectiveness during this ??deep?? solar minimum. The two HSSs within the interval were characterized by fast solar-wind speeds (peak values >?600 km?s?1) containing large-amplitude Alfvénic fluctuations, as is typical of HSSs during normal solar minima. However, the interplanetary magnetic field (IMF) magnitude [B o] was exceptionally low (??3??C?5 nT) during these HSSs, leading to lower than usual IMF B z values. The first HSS (HSS1) had favorable IMF polarity for geomagnetic activity (negative during northern Spring). The average AE and Dst for the HSS1 proper (HSS1P) were +?258 nT and ??21 nT, respectively. The second HSS (HSS2) had a positive sector IMF polarity, one that is less favorable for geomagnetic activity. The AE and Dst index averages were +?188 nT and ??7 nT, both lower than corresponding numbers for the first event, as expected. The HSS1P geomagnetic activity is comparable to, and the HSS2P geomagnetic activity lower than, corresponding observations for the previous minimum (1996). Both events?? geomagnetic activities are lower than HSS events previously studied in the declining phase (in 2003). In general, V sw was faster for the HSSs in 2008 compared to 1996. The southward IMF B z was lower in the former. The product of these two parameters [V sw and IMF B z ] comprises the solar-wind electric field, which is most directly associated with the energy input into the magnetosphere during the HSS intervals. Thus the combined effects led to the solar wind energy input in 2008 being slightly less than that in 1996. A detailed analysis of magnetic-field variances and Alfvénicity is performed to explore the characteristics of Alfvén waves (a central element in the geoeffectiveness of HSSs) during the WHI. The B z variances in the proto-CIR (PCIR) were ???30 nT2 and <?10 nT2 in the high speed streams proper. 相似文献
5.
On September 22, 2001 the Deep Space 1 spacecraft performed a flyby at comet 19P/Borrelly at a solar distance of 1.36 AU leading the Earth by 74° in longitude. The spacecraft-comet distance at closest approach was 2171 km. The bow shock had a magnetic compression ratio of 2.5 at a distance of 147 100 km from the nucleus. Deep Space 1 first entered the sheath region essentially from the north polar region. Fluctuations from the cometary ion pickup were present throughout the sheath region and even well upstream of the shock, as expected. The magnetic field pileup region had a peak field strength of 83 nT and was shown to be consistent with a pressure equal to the solar wind ram pressure. The peak field location was offset from the time of closest approach. It is uncertain whether this is a spatial or temporal variation. Draping of magnetic fields around the nucleus was sought, but evidence for this was not apparent in the data. A possible explanation is that the interplanetary solar wind was composed of turbulent short-scale fields, and thus the fields were not symmetric about the point of closest approach. During the flyby phase there were in general few intervals of ACE data where there were large scale Parker spiral fields. With the addition of plasma data, the shock properties are investigated. The characteristics of magnetic draping, pileup and fluctuations are explored. These comet 19P/Borrelly results are contrasted with other cometary flyby results. 相似文献
6.
E. Echer B.T. Tsurutani F.L Guarnieri J.U. Kozyra 《Journal of Atmospheric and Solar》2011,73(11-12):1330-1338
The seven CAWSES interplanetary fast forward shocks and their geomagnetic effects during 2004–2005 have been analyzed. It is found that the arrival time of the shocks at Earth can be estimated within an accuracy of ～5 min. Furthermore, AL decreases are found to occur within 10 min of shock impingement on the magnetopause. It was also determined that there is a direct correlation between the interplanetary magnetic field southward directed (IMF Bs) prior to shock arrival and substorms triggered by the shocks. If the IMF is northward prior to shock arrival, the geomagnetic activity is present but is low. One interpretation of this result is that the preconditioning energy stored in the magnetotail leaks away rapidly. A correlation between substorm peak AL and shock strength (Mach number) has also been noted, which could imply that shock strength is important for the amount of energy released into the magnetosphere/ionosphere. 相似文献
7.
E. Costa E. Echer M.V. Alves B.T. Tsurutani F.J.R. Simões F.R. Cardoso G.S. Lakhina 《Journal of Atmospheric and Solar》2011,73(11-12):1405-1409
We present a new method of calculating cross-field diffusion of charged particles due to their interactions with interplanetary magnetic decreases (MDs) in high heliospheric latitudes. We use a geometric model that evaluates perpendicular diffusion to the ambient magnetic field as a function of particle's gyroradius, MD radius, ratio between fields outside and inside the MD, and a random impact parameter. We use Ulysses magnetic field data of 1994 to identify the MDs and get the empirical size and magnetic field decrease distribution functions. We let protons with energies ranging from 100 keV to 2 MeV interact with MDs. The MD characteristics are taken from the observational distribution functions using the Monte Carlo method. Calculations show that the increase in diffusion tends to saturate when particles' gyroradius becomes as large as MD radii, and that particles' gyroradius increases faster than diffusion distance as the energy of the particles is increased. 相似文献
8.
新疆西昆仑科库西里克铅锌矿床地质及元素地球化学特征 总被引：1，自引：0，他引：1
新疆西昆仑地区科库西里克铅锌矿床赋存于中元古界长城系大理岩层间断裂带内.本文阐述了该矿床区域地质和地球化学背景,矿体特征及矿石成分,微量元素及稀土元素变化特点,并与区内密西西比型塔木—卡兰古铅锌矿床进行了比较.研究表明,科库西里克铅锌矿床矿体围岩—大理岩微量元素和稀土元素含量高于矿石,Rb、Th明显富集,Ce略富集,Ti亏损;矿石微量元素含量变化较大,Rb正异常明显,Ba、Nb、Zr、Ti负异常,既继承了围岩特征,又保留了成矿热液的成分特点.而塔木—卡兰古铅锌矿床的矿石与围岩的元素地球化学特征一致.据此认为科库西里克铅锌矿床成矿作用受中元古界长城系大理岩和断裂构造控制,成矿过程中有岩浆热液的加入. 相似文献
9.
10.
This talk provides a brief summary of the first conference devoted entirely to magnetic storms. The conference was held in Pasadena, California, at the Jet Propulsion Laboratory, 12-16 February 1996. Topics covered the relevant time-varying phenomena at the sun/corona, propagation of these structures through interplanetary space, the response of the magnetosphere from its interaction with these interplanetary structures, the formation of the storm- time ring-current (in particular the oxygen content of the ring-current), and storm ionospheric effects and ground based effects. A complementary summary is provided by Gonzalez et al. in EOS, 1996. The full set of review articles will be published in an AGU monograph and many of the contributed articles will appear in a special section of the Journal of Geophysical Research, Space Physics. 相似文献