全新世高温期气候不稳定性记录   总被引：13，自引：0，他引：13  

陈云  李铮华  赵景波  张俊牌  贾艳琨 《海洋地质与第四纪地质》1999,19(3):97-103

对黄土高原黄土剖面中的黑垆进行了植物孢粉植物硅酸体,碳同位素和化学分析测试,结果表明,黑垆土良好地记录了全新世高温期气候不稳定性,在大致９－６ｋａＢ．Ｐ．期间,曾发生数次强度不等的快速变化。  相似文献   

基于显著性分析的SAR溢油图像中暗斑区域检测方法研究     

吕新荣  李云  温春苗  任鹏 《海洋科学》2021,45(4):90-96

为了提高合成孔径雷达(syntheticapertureradar,SAR)图像中海上溢油的检测精度,设计了一种图像显著性和均值偏移分割相结合的暗斑检测方法,验证了该方法在SAR溢油图像暗斑识别中的有效性,为溢油区域的准确检测奠定了基础。针对SAR溢油图像中暗斑区域在人类视觉中属于感兴趣区域的特性,利用图像显著性检测方法对整幅SAR图像进行处理生成显著性图像,然后利用均值偏移方法在SAR图像的Lab空间将图像分割成不同区域,最后在显著性图像上利用每个区域的平均显著性值与动态阈值之间的关系确定溢油图像中的暗斑区域。实验结果表明,该方法不需要人工交互,且能够有效地提取出SAR图像溢油中的暗斑区域。  相似文献   

宇宙大尺度结构空洞的演化研究     

赵飞  罗煜  韦成亮 《天文学报》2019,60(4):87-102

为了研究空洞的演化以及暗物质空洞和星系空洞的差别,使用一组高精度的N体模拟数据以及基于此给出的半解析模拟星系数据,在红移2.03到红移0之间取了6个红移的数据,并使用VIDE (Void Identification and Examination toolkit)算法来找空洞,对星系空洞和暗物质空洞的统计性质比如丰度、数目、大小、形状、叠加密度轮廓等演化的比较的结果表明,随着红移的减小,空洞的数目逐渐减少、内部密度逐渐变小、体积逐渐增大、空洞的形状越来越扁.暗物质空洞和星系空洞的数目、平均大小、平均椭率的比值与红移呈线性关系.此外,不论是暗物质空洞还是星系空洞,小的空洞密度比在分布上比大空洞的低,更容易贯通并合,演化效应更明显.另外由于星系总是形成于暗物质密度场的高密度区域,使其不容易示踪暗物质空洞的一些薄弱的墙结构,导致星系空洞提前贯通.而对于已经形成的星系空洞而言,即便是其墙上最薄弱的地方也往往堆积着显著的暗物质,使得星系的位置保持稳定,甚至形成新的星系,从而抑制星系空洞的贯通.整体上暗物质空洞的演化要比星系空洞的演化更加明显.  相似文献   

Probing dark matter,galaxies and the expansion history of the Universe with Lyα in absorption and emission     

M.G. Haehnelt 《Astronomische Nachrichten》2010,331(5):541-548

Lyα radiation is an important diagnostic tool in a wide range of astrophysical environments. I will first describe here how measurements of the matter power spectrum on small scales from Lyα forest data constrain the mass of dark matter particles. I then will report on an ambitious program of searching for very faint spatially extended Lyα emission at z ∼ 3 which has led to the discovery of a new population of faint Lyα emitters which I will argue should be identified with the long searched for host galaxies of damped Lyα absorbers. Finally, I will discuss the possibility of measuring the redshift drift of Lyα absorption features and therefore the change of the expansion rate of the Universe in real time with the ultra‐stable high‐resolution spectrograph CODEX proposed for the E‐ELT (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Tidal tails of star clusters     

Andreas H. W. Küpper  Pavel Kroupa  Holger Baumgardt  Douglas C. Heggie 《Monthly notices of the Royal Astronomical Society》2010,401(1):105-120

Based on recent findings of a formation mechanism of substructure in tidal tails by Küpper et al., we investigate a more comprehensive set of N -body models of star clusters on orbits about a Milky Way like potential. We find that the predicted epicyclic overdensities arise in any tidal tail no matter which orbit the cluster follows as long as the cluster lives long enough for the overdensities to build up.
The distance of the overdensities along the tidal tail from the cluster centre depends for circular orbits only on the mass of the cluster and the strength of the tidal field, and therefore decreases monotonically with time, while for eccentric orbits the orbital motion influences the distance, causing a periodic compression and stretching of the tails and making the distance oscillate with time. We provide an approximation for estimating the distance of the overdensities in this case.
We describe an additional type of overdensity which arises in extended tidal tails of clusters on eccentric orbits, when the acceleration of the tidal field on the stellar stream is no longer homogeneous. Moreover, we conclude that a pericentre passage or a disc shock is not the direct origin of an overdensity within a tidal tail. Escape due to such tidal perturbations does not take place immediately after the perturbation but is rather delayed and spread over the orbit of the cluster. All observable overdensities are therefore of the mentioned two types. In particular, we note that substructured tidal tails do not imply the existence of dark matter substructures in the haloes of galaxies.  相似文献   

Constrained simulations of the local universe – II. The nature of the local Hubble flow     

Luis A. Martinez-Vaquero  Gustavo Yepes  Yehuda Hoffman  Stefan Gottlöber  Mira Sivan 《Monthly notices of the Royal Astronomical Society》2009,397(4):2070-2080

Using a suite of N -body simulations in different cold dark matter (CDM) scenarios, with cosmological constant (ΛCDM) and without (OCDM, SCDM), we study the Hubble flow (σ_H) in Local Volumes (LV) around Local Group (LG) like objects found in these simulations, and compare the numerical results with the most recent observations. We show that ΛCDM and OCDM models exhibit the same behaviour of σ_H. Hence, we demonstrate that the observed coldness of the Hubble flow is not likely to be a manifestation of the dark energy, contrary to previous claims. The coldness does not constitute a problem by itself but it poses a problem to the standard ΛCDM model only if the mean density within the LV is greater than twice the mean matter cosmic density. The lack of blueshifted galaxies in the LV, outside of the LG can be considered as another manifestation of the coldness of the flow. Finally, we show that the main dynamical parameter that affects the coldness of the flow is the relative isolation of the LG, and the absence of nearby Milky Way like objects within a distance of about  3 Mpc  .  相似文献   

Stellar velocity profiles and line strengths out to four effective radii in the early-type galaxies NGC 3379 and 821     

Anne-Marie Weijmans  Michele Cappellari  Roland Bacon  P. T. de Zeeuw  Eric Emsellem  Jesús Falcón-Barroso  Harald Kuntschner  Richard M. McDermid  Remco C. E. van den Bosch  Glenn van de Ven † 《Monthly notices of the Royal Astronomical Society》2009,398(2):561-574

We use the integral-field spectrograph SAURON to measure the stellar line-of-sight velocity distribution and absorption line strengths out to four effective radii ( R _e) in the early-type galaxies NGC 3379 and 821. With our newly developed observing technique, we can now probe these faint regions in galaxies that were previously not accessible with traditional long-slit spectroscopy. We make optimal use of the large field-of-view and high throughput of the spectrograph: by adding the signal of all ∼1400 lenslets into one spectrum, we obtain sufficient signal-to-noise in a few hours of observing time to reliably measure the absorption line kinematics and line strengths out to large radius.
We find that the line strength gradients previously observed within 1 R _e remain constant out to at least 4 R _e, which puts constraints on the merger histories of these galaxies. The stellar halo populations are old and metal poor. By constructing orbit-based Schwarzschild dynamical models, we find that dark matter is necessary to explain the observed kinematics in NGC 3379 and 821, with 30–50 per cent of the total matter being dark within 4 R _e. The radial anisotropy in our best-fitting halo models is less than in our models without halo, due to differences in orbital structure. The halo also has an effect on the  Mg  b – V _esc  relation: its slope is steeper when a dark matter halo is added to the model.  相似文献   

Galaxy clustering and galaxy–galaxy lensing: a promising union to constrain cosmological parameters     

Marcello Cacciato †  Frank C. van den Bosch  Surhud More  Ran Li  H. J. Mo  Xiaohu Yang 《Monthly notices of the Royal Astronomical Society》2009,394(2):929-946

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Cosmology with the cluster mass function: mass estimators and shape systematics in large weak lensing surveys     

Virginia L. Corless  Lindsay J. King 《Monthly notices of the Royal Astronomical Society》2009,396(1):315-324

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Dark stars at the Galactic Centre – the main sequence     

Pat Scott  Malcolm Fairbairn  Joakim Edsjö 《Monthly notices of the Royal Astronomical Society》2009,394(1):82-104

In regions of very high dark matter density such as the Galactic Centre, the capture and annihilation of WIMP dark matter by stars has the potential to significantly alter their evolution. We describe the dark stellar evolution code D ark S tars , and present a series of detailed grids of WIMP-influenced stellar models for main-sequence stars. We describe the changes in stellar structure and main-sequence evolution which occur as a function of the rate of energy injection by WIMPs, for masses of  0.3–2.0 M_⊙  and metallicities   Z = 0.0003–0.02  . We show what rates of energy injection can be obtained using realistic orbital parameters for stars at the Galactic Centre, including detailed consideration of the velocity and density profiles of dark matter. Capture and annihilation rates are strongly boosted when stars follow elliptical rather than circular orbits. If there is a spike of dark matter induced by the supermassive black hole at the Galactic Centre, single solar mass stars following orbits with periods as long as 50 yr and eccentricities as low as 0.9 could be significantly affected. Binary systems with similar periods about the Galactic Centre could be affected on even less eccentric orbits. The most striking observational effect of this scenario would be the existence of a binary consisting of a low-mass protostar and a higher mass evolved star. The observation of low-mass stars and/or binaries on such orbits would either provide a detection of WIMP dark matter, or place stringent limits on the combination of the WIMP mass, spin-dependent nuclear-scattering cross-section, halo density and velocity distribution near the Galactic Centre. In some cases, the derived limits on the WIMP mass and spin-dependent nuclear-scattering cross-section would be of comparable sensitivity to current direct-detection experiments.  相似文献