共查询到20条相似文献，搜索用时 31 毫秒
1.
Residual meteoritic material has been detected on the surface of crater interiors on lunar samples 60315,29 and 65315,68. Iron-nickel micrometeoroid residues are present in the form of mettallic spherules embedded in or attached to the crater glass-linings; stony-iron meteorite residual material is homogeneously mixed with the glass-linings.Crater simulation experiments show the dependence of crater diameter to depth ratio on projectile density. On the other hand, the projectile velocities exceeding 4 km/s have no measurable influence on the D/T ratios of microcraters. As a result, diameter-to-depth measurements on lunar microcraters yield three groups of micrometeorites in the size range between 1 μm and 1 mm: iron-nickel, stony-iron and low-density particles. The measured D/T values correspond directly to the kind of determined projectile residues: craters showing residues of iron-nickel meteorites have ratios of D/T = 1.3–1.4 and craters with stony-iron residues have ratios ofD/T = 1.9–2.1.Craters with diameters ?30 μm seem to have been formed predominantly by iron-nickel micrometeorites, whereas craters with diameters ?80 μm predominantly by stony meteorites. 相似文献
2.
During the initial explosive phase of the eruption of Arenal volcano small projectiles were thrown a maximum distance of 5 km. Considering the effect of atmospheric drag these projectiles must have had initial velocities of at least 600 m/sec. For this velocity, the gas pressure in the magma chamber must have reached at least 4700 bars and the kinetic energy of the initial explosion is estimated as 2.4 ± 1.2 × 10a ergs. Had the effect of aerodynamic braking been ignored in making these calculations, as has always been done in the past, the calculated initial velocity would have been 220 m/sec; chamber pressure and kinetic energy estimates would thus be substantially lower. Clearly, velocities of ejecta, chamber pressures and kinetic energies for many explosive volcanic events have been seriously underestimated in the recent past, as has been the ability of overlying materials to contain, in certain cases, tremendous overpressures for short periods of time. A projectile with an initial velocity of 600 m/sec would have a maximum range of more than 200 km on the moon. Thus, the presence of far-reaching secondary crater fields on the moon cannot, at this time, be considered evidence for an impact origin of the parent crater. 600 m/sec is not the upper limit for initial velocities of volcanic ejecta. There is some indication that such velocities could reach values greater than 2 km/sec, suggesting that volcanic as well as impact mechanisms may be able to impart escape velocity to lunar materials. 相似文献
3.
Friedrich H rz Jack B. Hartung Donald E. Gault 《Earth and Planetary Science Letters》1971,10(4):381-386
Craters in the 0.4 mm and larger size class were observed on six Apollo 12 whole rock surfaces (12017, 12021, 12038, 12047, 12051 and 12073). Craters on crystalline surfaces are characterized by a central, glass-lined cavity, a concentric zone of shock fractured, high albedo material and a concentric spallation area. The crater geometries observed are similar to craters produced on glasses and crystalline materials in the laboratory with projectile velocities exceeding 10 km/sec. The high projectile velocities required and the presence of a distinct demarcation line between cratered and uncratered surfaces on individual rocks indicate that most of the microcraters are produced by primary cosmic particles. These discrete impact events account for most of the erosion and fragmentation of lunar surface rocks. 相似文献
4.
L.J. Srnka G. Martelli G. Newton S.M. Cisowski M.D. Fuller R.B. Schaal 《Earth and Planetary Science Letters》1979,42(1):127-137
The impact of aluminum projectiles onto high-alumina terrestrial basalt blocks at 13–15 km s?1 in the presence of a variable magnetic field has been studied. Low-frequency search coil data show that plasma is produced. causing local compression of the ambient field. Although field production is expected, it was not detectable with the existing apparatus. Measurements of the remanence of the shocked basalt show that magnetization was acquired in the material near the craters. The acquired remanence is predominantly soft, but also contains a component not demagnetized by 500 Oe AC field treatment. Material shocked in a 10-Oe vertical field exhibits inverse dependence of magnetization upon distance from the crater center. Examination of the shocked basalt in thin section reveals a general lack of shock metamorphism in the material surrounding the crater, except for the presence of a high-pressure melt glass which was splashed onto the crater walls. Micro-probe analyses show that the glass is a whole-rock melt of fairly uniform composition, and is contaminated with aluminum from the projectile. The mineralogical data support the view that the acquired magnetization is shock remanence, since negligible shock heating occurred in the magnetized material. These results bear on the problem of lunar magnetism, suggesting that shock effects or possibly thermoremanence in ejecta fragments may be responsible for part of the magnetization of the lunar surface. 相似文献
5.
Wataru Kanda Yoshikazu Tanaka Mitsuru Utsugi Shinichi Takakura Takeshi Hashimoto Hiroyuki Inoue 《Journal of Volcanology and Geothermal Research》2008
The 1st crater of Naka-dake, Aso volcano, is one of the most active craters in Japan, and known to have a characteristic cycle of activity that consists of the formation of a crater lake, drying-up of the lake water, and finally a Strombolian-type eruption. Recent observations indicate an increase in eruptive activity including a decrease in the level of the lake water, mud eruptions, and red hot glows on the crater wall. Temporal variations in the geomagnetic field observed around the craters of Naka-dake also indicate that thermal demagnetization of the subsurface rocks has been occurring in shallow subsurface areas around the 1st crater. Volcanic explosions act to release the energy transferred from magma or volcanic fluids. Measurement of the subsurface electrical resistivity is a promising method in investigating the shallow structure of the volcanic edifices, where energy from various sources accumulates, and in investigating the behaviors of magma and volcanic fluids. We carried out audio-frequency magnetotelluric surveys around the craters of Naka-dake in 2004 and 2005 to determine the detailed electrical structure down to a depth of around 1 km. The main objective of this study is to identify the specific subsurface structure that acts to store energy as a preparation zone for volcanic eruption. Two-dimensional inversions were applied to four profiles across the craters, revealing a strongly conductive zone at several hundred meters depth beneath the 1st crater and surrounding area. In contrast, we found no such remarkable conductor at shallow depths beneath the 4th crater, which has been inactive for 70 years, finding instead a relatively resistive body. The distribution of the rotational invariant of the magnetotelluric impedance tensor is consistent with the inversion results. This unusual shallow structure probably reflects the existence of a supply path of high-temperature volcanic gases to the crater bottom. We propose that the upper part of the conductor identified beneath the 1st crater is mainly composed of hydrothermally altered zone that acts both as a cap to upwelling fluids supplied from deep-level magma and as a floor to infiltrating fluid from the crater lake. The relatively resistive body found beneath the 4th crater represents consolidated magma. These results suggest that the shallow conductor beneath the active crater is closely related to a component of the mechanism that controls volcanic activity within Naka-dake. 相似文献
6.
根据近场小孔径观测台网记录的余震序列资料，研究了2000年1月15日云南姚安MS6.4地震序列的地震物理过程. 用地震标定律关系估算主震的地震矩M0=1.58×1018N·m，矩震级MW=6.0，平均位错=0.63m，断层长度L=16.6km，断层宽度W=5.6km. 余震序列的高精度定位结果和能量分布走向，很好地证实了主震的断层破裂走向为N50°W，震区马尾菁断裂为主震发震构造，断层错动性质以右旋走滑为主. 用横波记录资料及波谱分析方法估算出余震的震源参数: 地震矩范围为1010～1016N·m，震源破裂半径a为80～500m，地震应力降范围为0.01～9.5MPa. 较大应力降(Δσ>1.0MPa)沿主断层线性排列，大应力降(Δσ>2.0MPa)与ML≥3.0级地震相关. 余震能量释放和高应力降的地震多发生在6.0～11km的深度范围，说明在这一深度范围内最大程度地集中了地壳中的应力. 相似文献
7.
Eiji Ohtani 《Earth and Planetary Science Letters》1984,67(2):261-272
The densities of silicate liquids with basic, picritic, and ultrabasic compositions have been estimated from the melting curves of minerals at high pressures. Silicate liquids generated by partial melting of the upper mantle are denser than olivine and pyroxenes at pressures higher than 70 kbar, and garnet is the only phase which is denser than the liquid at pressures from 70 kbar to at least 170 kbar. In this pressure range, garnet and some fraction of liquid separate from ascending partially molten diapirs. It is therefore suggested that aluminium-depleted komatiite with a high Ca/OAl2O3 ratio may be derived from diapirs which originated in the deep upper mantle at pressures from 70 kbar to at least 140 kbar (200–400 km in depth), where selective separation of pyropic garnet occurs effectively. On the other hand, aluminium-undepleted komatiite is probably derived from diapirs originating at shallower depths (< 200 km). Enrichment of pyropic garnet is expected at depths greater than 200 km by selective separation of garnet from ascending diapirs. The 200-km discontinuity in the seismic wave velocity profile may be explained by a relatively high concentration of pyropic garnet at depths greater than 200 km. 相似文献
8.
D.C. Presnall 《Physics of the Earth and Planetary Interiors》1980,23(2):103-111
For a lherzolite mantle with about 0.1 wt.-percent CO2 or less, and a CO2/H2O mole ratio greater than about one, the mantle solidus curve in P-T space will have two important low-temperature regions, one centered at about 9 kbar (30 km depth) and another beginning at about 28 kbar (90 km depth). It is argued that the depth of generation of primary tholeiitic magmas beneath ridge crests is about 9 kbar, and that the geotherm changes from an adiabatic gradient at greater pressures to a strongly superadiabatic gradient at lesser pressures. Such a ridge geotherm would intersect the solidus at two separate depth intervals corresponding to the two low-temperature regions on the solidus. With increasing age and cooling of the lithosphere, the shallow partial melt zone would pinch out and the thickness of the deep partial melt zone would decrease. With increasing depth in a mature oceanic lithosphere, the rock types would consist of depleted harzburgite from directly beneath the crust to about 30 km depth, fertile spinel lherzolite from about 30 km to 50–60 km, and fertile garnet lherzolite from about 50–60 km to the top of the deep partial melt zone at about 90 km. 相似文献
9.
A.W. Gerhard Kunze 《Physics of the Earth and Planetary Interiors》1974,8(4):375-387
The settling trends of 318 lunar mare craters are compared with predictions of numerical finite-element models in order to determine the creep response of the upper lunar mare crust. No settling is evident in craters smaller than 5 km in diameter. Settling rates of larger craters increase as function of crater size in a manner suggesting a non-linear lunar creep response corresponding to the power law where έ is the strain rate and σ is the differential stress. However, the observed nonlinearity is probably an apparent nonlinearity resulting from the temperature induced viscosity decrease with depth due to a lunar crustal temperature gradient of 3° C/km and a creep activation energy of 20 kcal/mole. It is concluded that creep in the lunar medium is essentially Newtonian, and that the effective viscosity of the upper lunar mare crust is (1.6 ± 0.3) · 1025 poise. 相似文献
10.
P. Lambert 《Earth and Planetary Science Letters》1977,35(2):258-268
Rochechouart crater (France) occurs in crystalline rocks of the northwestern French Massif Central. The crater is deeply eroded and the present ground level is exactly (±50m) tangent to the crater floor. No morphologic evidence of the crater has been preserved. A complete range of shock effects is known on the scale of rocks and minerals, which permitted a study of shock zoning. Shock level was determined in thin section from petrographic analysis of each specimen. A systematic sampling was done on all the structure. Shock zones were determined at the same time in the fall-back unit and in the target. Correlations between rock types or shock level in allochthonous and autochthonous materials were observed. They imply restrictions for the late excavation stage: part of the material lying above the crater floor limit was never ejected, but only mixed with small relative displacement. Shock level is relatively higher in allochthonous breccias than in the target. The distribution of shock effects is very complicated at all scales, even at the scale of the whole structure. However, shock level is relatively high around the center of the structure defined from the breccia geometry. The most probable impact point is located about 4 km west of Rochechouart. The breccia unit is extremely thin (less than 60 m). The crater floor is extremely flat; its elevation does not vary more than±50m over the whole structure (about 300 km2). The lack of circular symmetry in particular in the distribution of impact melts could suggest a pronounced anisotropic structure of the target and/or an inclinated trajectory of the projectile. The original crater size is most probably between 20 and 25 km in diameter, determined from the actual extent of differents rock types or shock effects. A rapid post-crater readjustment is proposed to explain the flat floor. There was no important vertical displacement since the flat shape of the crater floor was attained. 相似文献
11.
The active Karthala volcano is found on Grande Comore, the most westerly of four volcanic islands comprising the Comores Archipelago, between northern Madagascar and Mozambique. The caldera, roughly elliptical in outline, is 4 km long and 3 km wide, with outer walls around 100 m high. It is dominated by a large central pit crater, Chahale, which is 1300 m long, 800 m wide, and 300 m deep. A smaller cylindrical pit crater 250 m in diameter and 30 m deep, Changomeni, is found one km north of Chahale. The vertical walls of both pit craters show excellent sections of the ponded flows which form the caldera floor, and the minor faults and intrusions which affected these flows. The youngest lava on the island was produced on July 12th, 1965, as single aa basalt flow emitted from a fissure halfway between the two pit craters. Small fumaroles are still active on this flow, as well as in the pit craters and at several small cinder cones in the caldera. Alignment of pyroclastic cones and fissure eruptions forms a radial pattern centering on Chahale pit crater, suggesting that these radial fissures are locally controlled. Location of the caldera at the intersection of two regional fissure systems implies that its location is controlled by regional stresses. The present size and form of the caldera is a result of the coalescence of at least four smaller calderas. Although the visible walls of these smaller calderas do not show any outward dip, the theoretical considerations ofRobson andBarr (1964), if applicable, require that at depth these are outward-dipping ring dyke type of fractures. 相似文献
12.
We have investigated crustal deformations associated with the 1986 eruption of Izu-Oshima volcano, Japan, which was accompanied by an intensive fissure eruption. Two fissure crater chains, with NW-SE trend were created in the northern part of the caldera and on its northwestern flank. Their trend is consistent with the direction of compressive stress in this region. Depression of > 30 cm in the central zone including the caldera, and in the northwestern and southeastern parts in the island, was detected by precise leveling. On the other hand, uplifts up to 20 cm in the northeastern and southwestern parts were observed. Tide observations revealed that the Okada tide station, the leveling datum in Izu-Oshima, may have subsided by 5 cm after the eruption. An 1 m opening of fissure craters was detected by distance measurements of the baselines which cross fissure craters. Horizontal displacements obtained by reoccupation of control points showed a symmetrical pattern which was consistent with the opening of fissure craters. Anomalous strain changes were also observed in the surrounding regions—contractions were observed in the Boso and the Miura peninsula, northeast of Izu-Oshima, and extensions in the Izu peninsula.
To interpret these crustal deformations, a model which consists of a nearly vertical tensile fault and a deflation source is presented. The tensile fault lies parallel to the fissures and is divided into two parts according to depth. The deeper part of the tensile fault is 12 km long, 10 km wide, and has 2 km burial depth and 2.7 m opening displacement. The shallower part, which may represent the fissure craters, is 4 km long, 2 km wide, and the amount of opening is estimated to be 1 m. However, the deflation source may be located at a depth of 10 km beneath the northwestern flank of the caldera and depression just above the source is estimated to be 30 cm. A deflation source is required to explain the subsidence at the Okada tide station and the extension in the Izu peninsula. This model suggests that the eruption might have released tensile stresses in and around the Izu region which result from bending of the subducting Philippine Sea plate. 相似文献
13.
Most of the known pit craters in Hawaii occur along the East and Southwest Rift Zones of Kilauea volcano. The pit craters typically are either astride a single rift zone fracture or between a pair of rift zone fractures. These fractures are prominent in the pit crater walls. The pit craters are elliptical in plan view, with their major diameters ranging from 8 to 1140 m. They range in depth from 6 m to 186 m. They typically develop with initially steep, locally overhanging walls, but as the walls collapse, the craters fill with talus and become shaped like inverted elliptical cones. None of the craters apparently formed as eruptive vents, although some have been subsequently filled by lava. Devil's Throat is the best-exposed pit crater along the East Rift Zone. It is sited at a `waist' between two east-striking zones of ground cracks; the spacing between the crack zones decreases towards Devil's Throat. East-striking fractures are also prominent in the pit crater walls. Pit craters along the Southwest Rift Zone typically are elongate in plan view along the direction of the rift, have large caves at their bases along the long axes of the craters, and are smaller than those of the East Rift Zone. Some closely spaced pits there have coalesced to form a trough. Based on our observations and mechanical considerations, we infer that pit craters form by stoping over an underlying large-aperture rift zone fracture, and not by piston-like collapse over broad magma bodies or voids. Flow of magma along the underlying fracture may remove stoped blocks and prevent the fracture from being choked with debris. This mechanism is consistent with pit crater location, ground crack patterns, the preferred orientation of fractures in pit crater walls, and pit crater geometry (both in map view and cross-section). The mechanism also fits with observations of stoping into a gaping rift fracture that conducted lava from Kilauea caldera during the 1920s. Additionally, the ratio of pit crater width to depth of 0.5 to 2 is consistent with pit craters forming over a nearly vertical opening mode fracture. 相似文献
14.
In this paper a theory is evaluated to describe the development of the lunar crater population with time under the bombardment by meteoroids and solar wind. Starting from a general mass distribution law a differential equation has been established and solved separately for meteoroid impact and solar wind bombardment. The theory permits the calculation of absolute formation ages of the lunar surface as well as the particle flux, supposing the crater distributions on the moon have been measured. As an important result it includes a D−2 equilibrium crater distribution law (D =crater diameter), actually measured in Mare Tranquillitatis and Oceanus Procellarum. Additionally, the exponential decrease of particle flux with time is confirmed. 相似文献
15.
L. F. Chernogor 《Geomagnetism and Aeronomy》2018,58(1):119-126
This paper is concerned with the study of the possibility of products of a meteoroid explosion in the atmosphere (meteoroid plume) to reach ionospheric altitudes. It has been shown that, in the case of meter-sized or larger space bodies entering the atmosphere, the plume is able to reach the lower ionosphere. The plume can be one of the sources of the formation of nacreous and noctilucent clouds. The aerosols ejected by the plume to lower ionospheric altitudes can lead to the formation of dust plasma, significantly changing the electrodynamic properties of the medium. The motion of the plume with a velocity of ~1 km/s is accompanied by the generation of a ballistic shock with a radius of 1–10 km. The relative excess pressure in the shock front can cause relative disturbances in the electron content at the altitudes of D, E, and F1 layers by ~10–100%. The geomagnetic effect of the plume and ballistic shock can reach ~1–10 nT. 相似文献
16.
Extensive computer simulations aimed at testing a hypothesis that impact craters may explain the scaling behaviour of surface
spectra are presented. The simulations show that indeed crater effects alone may explain the spectral scaling of Mars’ topography
revealed from MOLA data. The range of the scaling exponents obtained for a wide range of simulation parameters does not exceed
the limits observed for Mars. The simulations suggest that the shape of large craters is the key factor leading to the two
scaling ranges in the surface spectra. Particular values of the scaling exponents may additionally depend on the depth-diameter
relationship and the crater size distribution. 相似文献
17.
综合利用玉树震区应急流动台站观测数据和青海地震台网固定台站观测数据,依据最新的人工地震宽角反射/折射剖面的速度模型,采用Hypo2000地震定位法,对2010年4月18日至4月29日期间玉树震区发生的部分余震进行了重新定位.重新定位后,震源位置的水平和垂直方向平均误差分别为1.35 km和4.68 km,走时残差为0.49 s.震源深度分布范围为1.48～19.85 km,平均震源深度为10.28 km.定位研究结果表明:玉树地震余震沿北西-南东向的甘孜-玉树断裂带的北支,即玉树-隆宝断裂分布,长约97 km.余震分布特征在主震(微观震中)两侧存在差异,可能反映了两侧构造特征存在差异.截止到4月29日,主震东南仍是应力的主要释放区域,余震强度大且活动密集的区域位于主震东南距主震约5 km、横向范围约20 km.主震破裂区的大部分应力在主震过程中得以释放,主震时应力未释放的区域成为主要的余震分布区.余震的连续发生可能已造成主震破裂区相互连通,且破裂范围向西北方向扩展.玉树主震及余震的发震构造为甘孜-玉树断裂的北支,即玉树-隆宝断裂段,断层性质为北东倾向的高角度左旋走滑断层.发震断层的倾角和宽度在帮洞两侧有所不同,帮洞以东发震断层宽度约为12 km,倾角约为83°;而帮洞以西发震断层宽度约为6.5 km,断层倾角约减缓为63°. 相似文献
18.
利用71个远震的波形资料,用接收函数方法提取了布设在长白山—镜泊湖火山区的34个宽频带流动数字地震台站的接收函数,通过对接收函数反演,获得了台站下方的S波速度结构.研究结果表明,沈阳—敦化一线莫霍面深度32～33km,向西地壳厚度加厚,到长春附近地壳厚度约为36km.在天池火山口莫霍面深度为达38km,而镜泊湖火山口森林的莫霍面深度约为39km.总体看研究区的地壳厚度是南浅北深.长白山天池火山口附近地下10km左右有一明显的低速层存在;镜泊湖火山口森林附近30km也可能有低速体存在;研究发现莫霍面上S波速度梯度在火山口附近和远离火山口有明显区别.在火山口附近其莫霍面的S波速度梯度比非火山口地区的S波速度梯度明显小,说明火山口下与一般的地壳莫霍面结构有差别.研究发现沈阳—敦化一线两侧的莫霍面深度有较大变化,其位置与地表的敦化—密山断裂基本一致,说明敦化—密山断裂是研究区的一条非常重要的地质构造带. 相似文献
19.
2008年5月12日我国四川省汶川地区发生了震惊世界的MS8.0地震.历史上,同类地震在大陆内部极为罕见.该地震深部构造背景的研究对理解其成因极为重要.本文利用中国地震局地质研究所地震动力学国家重点实验室在川西地区布设的大规模密集流动宽频带地震台阵记录的远震P波波形数据和接收函数非线性反演方法,得到了沿北纬31°线的19个台站下方120 km深度范围内的S波速度结构及台站下方地壳的平均泊松比.该观测剖面穿越了主震区,总长度约为420 km.
我们的结果揭示了川滇地块、松潘-甘孜地块和四川盆地三个不同地块构造差异.上述三个地块的地壳结构特征可以概括为：（1）四川盆地前陆壳幔界面向西侧倾斜并有较为明显的横向变形,地壳厚度存在46～52 km的横向变化,中下地壳S波速度存在横向变化,地壳平均泊松比值较高（0.28～0.31）,但在龙门山断裂带附近,显示了坚硬地壳的特征,地壳平均泊松比仅为0.2;（2）松潘-甘孜地块地壳厚度由西侧靠近鲜水河断裂的60 km,向东减薄为52 km,在14～50 km深度范围内存在S波速度2.75～3.15 km/s的楔状低速区,其厚度由西侧的～30 km向东逐渐减薄为～15 km,相应区域的地壳平均泊松比高达0.29～0.31; （3）鲜水河断裂西侧,川滇地块地壳结构相对简单,地壳厚度为58 km,并在26 km深度存在约10 km厚度的高速层,地壳内平均泊松比约为0.25;（4）汶川大震区在12～23 km深度上具有近乎4.0 km/s的S波高速结构,而其下方的地壳为低速结构,地壳平均泊松比0.31～0.32,汶川大震的余震序列主要分布在高速介质区域内.
本文的结果表明松潘-甘孜地块的地壳相对软弱;而且并不存在四川盆地向西侧的俯冲.我们认为在青藏高原东向挤压的长期作用下,四川盆地强硬地壳的阻挡作用可导致松潘-甘孜地块内部蓄积很大的应变能量以及上、下地壳在壳内低速层顶部边界的解耦,在龙门山断裂带附近形成上地壳的铲形逆冲推覆.汶川大地震及其邻近区域所具有的坚硬上地壳和四川盆地的阻挡作用为低应变率下的高强度应力积累创造了必要条件,而松潘-甘孜地块长期变形积累的高应变能构成了孕育汶川大地震的动力来源. 相似文献
20.