用自然伽马测井数据估算桑托斯盆地的地层生热率     

孙旭东  郭兴伟  郑求根  温珍河  张训华  王锦洲  李子渊 《海洋科学》2021,45(9)

岩石生热率是研究地球内热的一个重要的参数。本文根据自然伽马与岩石生热率的关系,利用盆地4口钻井的自然伽马测井曲线,计算出桑托斯盆地主要岩石或矿物及地层的生热率。本文统计了2964个自然伽马测井数据值,主要岩石或矿物的生热率从大到小依次为：泥岩、砂岩、页岩、玄武岩、石灰岩、硬石膏和盐岩;盆地地层的生热率随深度增加显著降低,生热率体现出受控于岩性变化的特征。以S1井为例,根据岩石生热率和热流的关系,计算出盆地中各个组的生热率,Marambaia组、Itajai-Acu组、Itanhaem组、Ariri组、Guaratiba群、Camboriu组生热率分别是1.36±0.16μW/m3、1.52±0.15μW/m3、1.30±0.3μW/m3、0.46±0.18μW/m3、0.64±0.23μW/m3、0.37±0.07μW/m3,盆地沉积地层产生的热量占表层大地热流的13.62%,因此沉积地层具有一定的产热潜力,对区域有机质的成熟度有一定的影响。建立了岩石圈分层生热模型,其中地壳热流贡献为15.38mW/m2,占表层大地热流的30.76%,地幔热流贡献值为34.62mW/m2,地壳和地幔的热流比例为0.44,具有“冷壳热幔”的特征。  相似文献   

The Review of γ-ray Astronomical Observing Techniques     

《Chinese Astronomy and Astrophysics》2021,45(3):281-300

$\gamma$-ray is a unique probe for extreme events in the universe. Detecting the $\gamma$-ray provides an important opportunity to understand the composition of universe, the evolution of stars, the origin of cosmic rays, etc. $\gamma$-ray astronomy involves in various frontier scientific issues, and the observed energy spectrum spans over a wide range from a few hundreds of keV to a few hundreds of TeV. Different $\gamma$-ray telescopes are in need for different scientific goals and spectral bands. In this work, 5 kinds of space- and ground-based $\gamma$-ray observing techniques were summarized, including the Coded-aperture telescopes, Compton telescopes, Pair-production telescopes, Imaging Atmospheric Cherenkov Telescopes, and Extensive Air Shower Arrays. The progress in $\gamma$-ray astronomy in the past 70 years, motivated by the observation capability, was reviewed. Great achievements have been made in the high-energy domain and very-high-energy domain, while because of the limited missions conducted, as well as a lower sensitivity comparing with other domains, discoveries in low- and medium-energy are few, and due to the high observation difficulty, as well as the late start, relevant scientific yields in ultra- and extremely-high energy are limited. Moreover, the future planned missions and capabilities of the $\gamma$-ray telescopes and their possible scientific outputs were discussed. Among these missions, low- and medium-energy space telescopes e-ASTROGAM (enhanced-ASTROGAM), AMEGO (All-sky Medium Energy Gamma-ray Observatory), and very-high-energy ground-based arrays LHAASO (Large High Altitude Air Shower Observatory) and CTA (Cherenkov Telescope Array) greatly improve sensitivity than their corresponding last generation, thus expect very likely to further expand our knowledge on the $\gamma$-universe.  相似文献   

Simultaneous optical polarimetry and X-ray observations of the magnetic CV CP Tuc (AX J2315−592)     

Gavin Ramsay  S. B. Potter  David A. H. Buckley  Peter J. Wheatley 《Monthly notices of the Royal Astronomical Society》1999,306(4):809-814

CP Tuc (AX J2315–592) shows a dip in X-rays which lasts for approximately half the binary orbit and is deeper in soft X-rays compared with hard X-rays. It has been proposed that this dip is due to the accretion stream obscuring the accretion region from view. If CP Tuc were a polar, as has been suggested, then the length of such a dip would make it unique amongst polars since in those polars in which a dip is seen in hard X-rays the dip lasts for only 0.1 of the orbit. We present optical polarimetry and RXTE observations of CP Tuc which show circular polarization levels of ∼10 per cent and find evidence for only one photometric period. These data confirm CP Tuc as a polar. Our modelling of the polarization data implies that the X-ray dip is due to the bulk of the primary accretion region being self-eclipsed by the white dwarf. The energy dependence of the dip is due to a combination of this self-eclipse and also the presence of an X-ray temperature gradient over the primary accretion region.  相似文献   

Detection of X-ray emission from the host clusters of 3CR quasars     

C. S. Crawford  I. Lehmann  A. C. Fabian  M. N. Bremer  G. Hasinger 《Monthly notices of the Royal Astronomical Society》1999,308(4):1159-1172

We report the detection of extended X-ray emission around several powerful 3CR quasars with redshifts out to 0.73. The ROSAT HRI images of the quasars have been corrected for spacecraft wobble and compared with an empirical point-spread function. All the quasars examined show excess emission at radii of 15 arcsec and more, the evidence being strong for the more distant objects and weak only for the two nearest ones, which are known from other wavelengths not to lie in strongly clustered environments. The spatial profile of the extended component is consistent with thermal emission from the intracluster medium of moderately rich host clusters to the quasars. The total luminosities of the clusters are in the range ∼4×10⁴⁴–3×10⁴⁵ erg s⁻¹, assuming a temperature of 4 keV. The inner regions of the intracluster medium are, in all cases, dense enough to be part of a cooling flow.  相似文献   

Regional‐scale sedimentation process models from airborne gamma ray remote sensing and digital elevation data     

Geoff Pickup  Alan Marks 《地球表面变化过程与地形》2001,26(3):273-293

Airborne gamma ray survey data were used to provide information on potassium, thorium and uranium concentrations in surface soil and rock in arid central Australia. Spatial patterns in these radioelements allow tracing of paths of sediment at catchment scale. Survey elevation data are combined with contour data to produce digital elevation models for terrain analysis, tracing of sediment flow paths and modelling of extreme floods. Gamma ray data show consistent variation with slope, a limited range of drainage areas, and erosion/deposition models derived from the conservation of mass equation. Supply‐limited sediment transport models give a reasonable reproduction of observed radioelement distribution but some elements of the distribution pattern reflect the area inundated by 500–1000 year floods rather than the effects of simple downslope movement. Partial area sediment supply models are derived by downstream accumulation of erosion and deposition rates calculated using the conservation of mass equation with transport laws based on slope alone and stream power. Comparison with observed radioelement patterns suggests that both transport laws apply in different parts of the landscape. Regional‐scale sediment transport models will require a range of models depending on location in the landscape and event frequency. This approach may allow estimation of sediment delivery ratios. Copyright © 2001 John Wiley & Sons, Ltd.  相似文献   

A ‘superoutburst’ in XTEJ1118+480     

E. Kuulkers 《Astronomische Nachrichten》2001,322(1):9-14

I propose that the properties of the two outbursts observed in the X‐ray transient XTEJ1118+480 in 2000 are akin to superoutbursts of SU UMa stars. In these systems a ‘normal’ outburst immediately precedes a 5–10 times longer (‘super’) outburst. The optical light curve of the outbursts of XTEJ1118+480 is remarkably similar to that seen in some SU UMa stars, such as UVPer and TLeo, where the precursor outburst is distinct from the superoutburst, but the time scales are a factor of ∼15 different. The first outburst of XTEJ1118+480 was relatively short (∼1 month) while the second outburst was ∼5 times longer. During the second outburst superhumps were seen, a feature characteristic for superoutbursts. The gap of about a month between the two outbursts is longer in X‐rays with respect to the optical, a feature not previously recognized for X‐ray transients. Also in SU UMa stars the precursor outburst becomes more distinct at shorter wavelengths. Finally, I show that the time of appearance of the superhumps in XTEJ1118+480 is consistent with the expected superhump growth time, if the superhump mechanism was triggered during the first outburst. I conclude that the similarity in outburst behaviour in the two types of systems provides further support that a common mechanism is at work to start the long (‘super’) outbursts.  相似文献   

ROSAT HRI observations of P Cyg and surrounding area     

T.W. Berghfer  H.J. Wendker 《Astronomische Nachrichten》2000,321(4):249-253

We present a detailed analysis of deep ROSAT HRI observations of the luminous blue variable P Cyg and its surrounding radio nebula. The HRI image provides a point source at the position of P Cyg. However, we show that this emission can be attributed to the ultraviolet leak of the ROSAT HRI. The X‐ray flux upper limit derived from the HRI data of this star is discussed in the context of X‐ray emission from hot stars. Furthermore, we present a search for diffuse X‐ray emission possibly associated with the radio nebula surrounding P Cyg. We compare our results to model predictions and X‐ray fluxes observed for shells around other hot stars. Additionally, we detect 10 X‐ray sources in the field of view. All but one of these X‐ray emitters have stellar counter parts in the Palomar Sky Survey. We suggest that they are active late‐type stars possibly belonging to Cyg OB1.  相似文献   

Reservoir architecture and heterogeneity distribution in floodplain sandstones: Key features in outcrop,core and wireline logs     

Luis Miguel Yeste  Augusto N. Varela  César Viseras  Neil D. Mcdougall  Fernando García-García 《Sedimentology》2020,67(7):3355-3388

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基于单能窄束伽马射线算法计算高分辨率屏蔽自然伽马探测器的三维测井响应          下载免费PDF全文

商庆龙  汪建勋  汪宏年  刘长伟  姚东华  陶宏根 《地球物理学报》2014,57(3):979-990

本文应用单能窄束伽马射线理论建立高分辨率屏蔽自然伽马探测器三维测井响应的数值模拟算法.首先利用单能窄束原理,用稳态扩散方程描述伽马光子密度的空间分布,根据扩散方程基本解、放射源空间分布、探测器位置和屏蔽情况,将屏蔽探测器上的总伽马通量表示成放射性地层中的有效探测区域上的体积分和晶体表面上有效接收面的面积分形式.并根据伽马射线传播路径和探测器屏蔽情况,给出有效探测区域的解析表达式,通过数值积分法计算任意复杂情况下探测器上的自然伽马通量,获得伽马测井响应的3D数值模拟算法.并通过数值模拟结果与模型井数据的对比验证了该算法的有效性.最后通过3D数值模拟算法系统研究考察晶体形状（圆柱形晶体、方形晶体）、晶体长度、仪器在井轴中的位置（居中屏蔽探测器、贴井壁屏蔽探测器）、以及测速等不同情况下自然伽马测井响应,设计出新型高分辨率自然伽马测井仪器.  相似文献   

Radiolysis of sulfuric acid, sulfuric acid monohydrate, and sulfuric acid tetrahydrate and its relevance to Europa     

M.J. Loeffler  R.L. Hudson  R.W. Carlson 《Icarus》2011,215(1):370-380

We report laboratory studies on the 0.8 MeV proton irradiation of ices composed of sulfuric acid (H₂SO₄), sulfuric acid monohydrate (H₂SO₄·H₂O), and sulfuric acid tetrahydrate (H₂SO₄·4H₂O) between 10 and 180 K. Using infrared spectroscopy, we identify the main radiation products as H₂O, SO₂, (S₂O₃)_x, H₃O⁺, , and . At high radiation doses, we find that H₂SO₄ molecules are destroyed completely and that H₂SO₄·H₂O is formed on subsequent warming. This hydrate is significantly more stable to radiolytic destruction than pure H₂SO₄, falling to an equilibrium relative abundance of 50% of its original value on prolonged irradiation. Unlike either pure H₂SO₄ or H₂SO₄·H₂O, the loss of H₂SO₄·4H₂O exhibits a strong temperature dependence, as the tetrahydrate is essentially unchanged at the highest irradiation temperatures and completely destroyed at the lowest ones, which we speculate is due to a combination of radiolytic destruction and amorphization. Furthermore, at the lower temperatures it is clear that irradiation causes the tetrahydrate spectrum to transition to one that closely resembles the monohydrate spectrum. Extrapolating our results to Europa’s surface, we speculate that the variations in SO₂ concentrations observed in the chaotic terrains are a result of radiation processing of lower hydration states of sulfuric acid and that the monohydrate will remain stable on the surface over geological times, while the tetrahydrate will remain stable in the warmer regions but be destroyed in the colder regions, unless it can be reformed by other processes, such as thermal reactions induced by diurnal cycling.  相似文献