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介绍了成像式宇宙噪声接收机在中山站的部署,分析了首批观测数据,得出中山站区宇宙噪声静日曲线。分析表明,观测期间中山站区的宇宙噪声吸收事件夜间与白天显著不同。在夜间,吸收事件呈脉冲式,持续时间为数分钟,吸收区域常在站区北侧出现,沿东西方向伸展;在磁中午附近,吸收事件持续时间在１小时以上,吸收区域南北侧较强,中央较弱。可以认为,夜间吸收区域对应着极光带,其吸收由极光粒子沉降引起;在磁中午,吸收区域对应着极隙区,其吸收可能与极隙区粒子沉降和对流有关。 相似文献
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宇宙是无边无际、无始无终的
科学上所讲的宇宙概念,是空间和时间的总和,有一个发生、发展和衰亡的过程,它不同于哲学上的宇宙概念。哲学上的宇宙概念是无边无际、无始无终的。 相似文献
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加速器质谱仪 (AMS)的发展使高精度测量宇宙成因核素1 0 Be并应用于研究天文、地理和古气候成为可能。雪冰中的1 0 Be浓度可以指示古降水量的变化 ,其在大气中的产率变化则可以反映三个主要控制因素 :原始宇宙射线强度、地磁场强度和太阳活动的变化。此外 ,配合其它宇宙成因核素 ,1 0 Be还能用于定年 ,并利用特殊“峰”帮助一些古老冰芯建立年代表 ,提供可作为全球对比标志的特殊信息。青藏高原因其特有的高海拔地势而拥有丰富的中低纬山地冰川资源 ,其冰雪中的1 0 Be资料可能提供比极地高纬资料更清晰的1 0 Be与大气环流、地磁场屏蔽作用关系的信息 ,将是对1 0 Be现有认识的极好补充。 相似文献
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甘肃省农田生态系统碳收支动态 总被引：2，自引：0，他引：2
量化分析了甘肃省兰州、天水、庆阳、定西、金昌和嘉峪关及甘南藏族自治州7个地区的农田生态系统主要作物碳吸收、排放的动态变化。结果显示:研究区2007—2014年的农田生态系统碳吸收总量为1.67~61.18万t,年均增加率3.31%~18.10%。农田生态系统的碳吸收强度最大的是嘉峪关,其次是兰州;碳吸收强度最小的是定西,为0.62 t·hm-2·a-1。2007—2014年,兰州、天水、庆阳、定西、金昌、嘉峪关、甘南的农田生态系统的年均净碳源强度分别为-0.254、-0.241、-0.196、-0.221、-0.005、0.163、-0.042 t·hm-2。 相似文献
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宇宙万物中,唯有生命是最积极、最活跃、最生机勃勃、最神秘莫测的了。自从来到这个星球上以后,它便以其坚强的意志生存．下来,以其磅礴的气势扩展开去,分化繁衍,以至无穷,这是多么神奇的力量啊!如果没有生命,地球只能是一个死气沉沉的星球,宇宙也只能是一个毫无生气的宇宙,即令其空间无限,时间永恒,又有什么实际意义呢? 相似文献
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在中国第28次南极科学考察期间,利用“雪龙号”科考船载SIMRAD EK500（38kHz）科学渔探仪对南极半岛附近海域的南极大磷虾资源量进行了调查。原始声学数据经过信噪比估算和背景噪声剔除数据后处理方法剔除背景噪声以及手动剔除表面混响、海底反射和坏数据之后,在200 m以浅水层中,以1n mile间隔进行积分,并应用Matlab软件编程对积分结果进行后处理,得出调查海域中南极大磷虾的资源分布情况。结果表明：（1）“雪龙号”的平均噪声功率值为-146.47dB re 1W;(2)空白水体的噪声平均剔除百分比为88.3%;（3）调查区域内的南极大磷虾平均密度为27.30 g·m-2（62.95 ind·m-2）。 相似文献
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Using the ground observation data at Zhongshan Station of Antarctica during July 13 to 17, 2000, the intense absorption events associated with the activities of the solar active region R9077 are analyzed. It was shown that an intense polar cap absorption event lasted more than 3 days, which was caused by the solar proton event associated with the X5/3B major flare at 1024 UT on July 13. The polar cap event started at about 1040 UT on July 14, and lasted to about 1940 UT on July 17, with a typical day night variation. At the same time, the intense solar activities extremely disturbed the magnetosphere, therefore aurora substorms occurred frequently. The energetic particle precipitation from the magnetosphere caused several absorption spikes superposing on the background of polar cap absorption. One distinct event is the absorption enhancement that started at about 0300 UT on July 15, reached its peak of 26 dB at about 0645 UT and recovered at about 1110 UT on the same day, which was the strongest absorption event observed at Zhongshan Station since the imaging riometer installed in February, 1997. Another outstanding absorption spike with pulsation occurred at about 1753 UT on 14th, its peak reached to 6 dB. 相似文献
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Ionospheric absorption at Zhongshan Station, Antarctica during magnetic storms in early May, 1998 
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下载免费PDF全文 In the paper the high latitude ionospheric absorption events, monitored by an imaging riometer at Zhongshan Station, Antarctica, are examined during magnetic storms in early May, 1998. The storm absorption at ~0639 UT on May 2 was mainly an equatorward progressing absorption event, which were associated with a strong negative bay of the magnetic H component and with a large Pc3 range pulsation. There was a time lag of about 1. 5 hours between the onset of the ionospheric disturbance and the IMF southward turning in the solar wind. The event at 2222 UT on May 2 was a typical midnight absorption spike event. The absorption region took the form of an elongated strip with the length of 100 - 150 km and the width of 30 - 40 km. The absorption during 0830 - 1200 UT on May 6 was a polar cap absorption (PCA) event,caused by intense precipitation of high-energy protons erupted after a large solar flare explosion. 相似文献
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Post-noon ionospheric absorption observed by the imaging riometers at polar cusp/cap conjugate stations 总被引：1，自引：1，他引：0 下载免费PDF全文
下载免费PDF全文 An example of post-noon ionospheric absorption observed by the imaging riometers at Ny-Alesund / Danmarkshavn in the arctic region and Zhongshan Station in Antarctic is presented. The post-noon absorption observed simultaneously between the hemispherical stations was a spike-type with weak intensity (<1 dB) during the high solar wind dynamic pressure. The absorption spikes might be caused by precipitation of highrenergy electrons (30 - 300 keV) in the closed dayside magnetosphere. It should be noted that the precipitation region of the absorption spike associated with the steep pressure increase (~ 13 nPa) was localized and shifted equatorward. 相似文献
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Monika Breitzke Olaf Boebel Saad El Naggar Wilfried Jokat Berthold Werner 《Geophysical Journal International》2008,174(2):505-524
Air guns and air-gun arrays of different volumes are used for scientific seismic surveys with R/V Polarstern in polar regions. To assess the potential risk of these research activities on marine mammal populations, knowledge of the sound pressure field of the seismic sources is essential. Therefore, a broad-band (0–80 kHz) calibration study was conducted at the Heggernes Acoustic Range, Norway. A GI (2.4 l), a G (8.5 l) and a Bolt gun (32.8 l) were deployed as single sources, 3 GI (7.4 l), 3 G (25.6 l) and 8 VLF™ Prakla-Seismos air guns (24.0 l) as arrays. Each configuration was fired along a line of 3–4 km length running between two hydrophone chains with receivers in 35, 100, 198 and 263 m depth. Peak-to-peak, zero-to-peak, rms and sound exposure levels (SEL) were analysed as functions of range. They show the typical dipole-like directivity of marine seismic sources with amplitude cancellation close to the sea surface, higher amplitudes in greater depths, and sound pressure levels which continuously decrease with range. Levels recorded during the approach are lower than during the departure indicating a shadowing effect of Polarsterns's hull. Backcalculated zero-to-peak source levels range from 224–240 dB re 1 μPa @ 1 m. Spectral source levels are highest below 100 Hz and amount to 182–194 dB re 1 μPa Hz–1 . They drop off continuously with range and frequency. At 1 kHz they are ∼30 dB, at 80 kHz ∼60 dB lower than the peak level. Above 1 kHz amplitude spectra are dominated by Polarstern's self-noise. From the rms and sound exposure levels of the deepest hydrophone radii for different thresholds are derived. For a 180 dB rms-level threshold radii maximally vary between 200 and 600 m, for a 186 dB SEL threshold between 50 and 300 m. 相似文献
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THE INFLUENCE OF THE COSMIC RAY FORBUSH DECREASE ON THE LOW IONOSPHERE IN THE POLAR REGION 下载免费PDF全文
下载免费PDF全文 Used the ionization theory of the cosmic ray charged particles in the polar ionosphere, the influence of the cosmic ray Forbush decrease on the low ionosphere in the polar region is studied in this paper. The relationship between the Forbush decrease and the cosmic noise absorption during the polar night is analysed based on the data recorded by a Riometer at Antarctic Zhongshan Station (69° 22′24″S, 76°22′40″E). The relation of between the cosmic ray Forbush decrease and the cosmic noise absorption is well interpreted by means of the ionizaiotn theory. 相似文献
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Richard S. Gross 《Geophysical Journal International》1986,85(1):161-177
Summary. A direct calculation is made of the effect on the Chandler wobble of 1287 earthquakes that occurred during 1977–1983. The hypocentral parameters (location and origin time) and the moment tensor representation of the best point source for each earthquake as determined by the 'centroidmoment tensor' technique were used to calculate the change in the Chandler wobble's excitation function by assuming this change is due solely to the static deformation field generated by that earthquake. The resulting theoretical earthquake excitation function is compared with the 'observed' excitation function that is obtained by deconvolving a Chandler wobble time series derived from LAGEOS polar motion data. Since only 7 years of data are available for analysis it is not possible to resolve the Chandler band and determine whether or not the theoretical earthquake excitation function derived here is coherent and in phase with the 'observed' excitation function in that band. However, since the power spectrum of the earthquake excitation function is about 56 dB less than that of the 'observed' excitation function at frequencies near the Chandler frequency, it is concluded that earthquakes, via their static deformation field, have had a negligible influence on the Chandler wobble during 1977–1983. However, fault creep or any type of aseismic slip that occurs on a time-scale much less than the period of the Chandler wobble could have an important (and still unmodelled) effect on the Chandler wobble. 相似文献
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A series of solar flare and coronal mass ejection (CME) event occurred in July 2000, particularly the largest flare (X5.7/3B) with CME on 14th of July since 1989, which stimulated a great geomagnetic storm with D st index reaching -300 nT. A number of data have been obtained from the Chinese Antarctic Zhongshan Station (ZHS, INT Lat. 74.5°, L≈14), which is located at cusp latitude, and from the ACE satellite. After analyzing these data we have got the results as follows: a lot of solar high energy particles penetrated into the polar ionosphere and ionized it, which significantly increased the cosmic noise absorption (CNA) and blanked the DPS-4 data for more than two days. The magnetic pulsation in Pc 3/5 frequency band on the ground has a high relation with the fluctuation of interplanetary magnetic field (IMF) B z, which shows the contribution of interplanetary magnetohydrodynamical (MHD) waves to the Pc 3/5 pulsation on the ground. The Pc 3/5 pulsation was intensified much during the great magnetic storm. The H component of the magnetic field at ZHS varied with the southern value of IMF B z but lagged behind for about 8 10 h. While D st index responded to the variation of the IMF B z very quickly, which suggested that the magnetic storm occurred at low latitude firstly and then effected the ionospheric current at high latitude. 相似文献
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Palaeomagnetism of the Lower Ordovician Orthoceras Limestone, St. Petersburg, and a revised drift history for Baltica in the early Palaeozoic 总被引：2，自引：0，他引：2
MarkA.Smethurst AlexeyN.Khramov Sergei Pisarevsky 《Geophysical Journal International》1998,133(1):44-56
Palaeomagnetic investigation of Lower Ordovician limestone in the vicinity of St. Petersburg yields a pole position at latitude 34.7°N, longitude 59.1°E ( dp / dm =5.7°/6.4°). A probable primary remanence origin is supported by the presence of a field reversal. The limestone carries one other remanent magnetization component associated with a Mesozoic remagnetization event.
An apparent polar wander path is compiled for Baltica including the new result, ranging in age from Vendian to Cretaceous. Ages of the published Lower to mid-Palaeozoic palaeomagnetic pole positions are adjusted in accordance with the timescale of Tucker & McKerrow (1995). The new Arenig result is the oldest of a series of Ordovician and Silurian palaeomagnetic pole positions from limestones in the Baltic region. There are no data to constrain apparent polar wander for the Tremadoc, Cambrian and latest Vendian. If the Fen Complex results, previously taken to be Vendian in age ( c . 565 Ma), are reinterpreted as Permian remagnetizations, an Early Ordovician–Cambrian–Vendian cusp in the polar wander path for Baltica is eliminated. The apparent polar wander curve might then traverse directly from poles for Vendian dykes on the Kola peninsula ( c . 580 Ma) towards our new Arenig pole ( c . 480 Ma). The consequence of this change in terms of the motion of Baltica in Cambrian times is to reduce significantly a rotational component of movement.
The new Arenig pole extends knowledge of Ordovician apparent polar wander an increment back in time and confirms the palaeolatitude and orientation of Baltica in some published palaeogeographies. Exclusion of the Fen Complex result places Baltica in mid- to high southerly latitudes at the dawn of the Palaeozoic, consistent with faunal and sedimentological evidence but at variance with some earlier palaeomagnetic reconstructions. 相似文献
An apparent polar wander path is compiled for Baltica including the new result, ranging in age from Vendian to Cretaceous. Ages of the published Lower to mid-Palaeozoic palaeomagnetic pole positions are adjusted in accordance with the timescale of Tucker & McKerrow (1995). The new Arenig result is the oldest of a series of Ordovician and Silurian palaeomagnetic pole positions from limestones in the Baltic region. There are no data to constrain apparent polar wander for the Tremadoc, Cambrian and latest Vendian. If the Fen Complex results, previously taken to be Vendian in age ( c . 565 Ma), are reinterpreted as Permian remagnetizations, an Early Ordovician–Cambrian–Vendian cusp in the polar wander path for Baltica is eliminated. The apparent polar wander curve might then traverse directly from poles for Vendian dykes on the Kola peninsula ( c . 580 Ma) towards our new Arenig pole ( c . 480 Ma). The consequence of this change in terms of the motion of Baltica in Cambrian times is to reduce significantly a rotational component of movement.
The new Arenig pole extends knowledge of Ordovician apparent polar wander an increment back in time and confirms the palaeolatitude and orientation of Baltica in some published palaeogeographies. Exclusion of the Fen Complex result places Baltica in mid- to high southerly latitudes at the dawn of the Palaeozoic, consistent with faunal and sedimentological evidence but at variance with some earlier palaeomagnetic reconstructions. 相似文献