排序方式： 共有115条查询结果，搜索用时 21 毫秒
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Z. Fan J. Ma R. de Grijs Y. Yang X. Zhou 《Monthly notices of the Royal Astronomical Society》2006,371(4):1648-1658
The large majority of extragalactic star cluster studies performed to date essentially use multicolour photometry, combined with theoretical stellar synthesis models, to derive ages, masses, extinction estimates and metallicities. M31 offers a unique laboratory for studies of globular cluster (GC) systems. In this paper, we obtain new age estimates for 91 M31 GCs, based on improved photometric data, updated theoretical stellar synthesis models and sophisticated new fitting methods. In particular, we used photometric measurements from the Two Micron All Sky Survey (2MASS), which, in combination with optical photometry, can partially break the well-known age–metallicity degeneracy operating at ages in excess of a few Gyr. We show robustly that previous age determinations based on photometric data were affected significantly by this age–metallicity degeneracy. Except for one cluster, the ages of our other sample GCs are all older than 1 Gyr. Their age distribution shows populations of young- and intermediate-age GCs, peaking at ∼3 and 8 Gyr, respectively, as well as the 'usual' complement of well-known old GCs, i.e. GCs of similar age as the majority of the Galactic GCs. Our results also show that although there is significant scatter in metallicity at any age, there is a notable lack of young metal-poor and old metal-rich GCs, which might be indicative of an underlying age–metallicity relationship among the M31 GC population. 相似文献
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Perihelion motion, i.e. a secular change of longitude of perihelion, of interplanetary dust particles is investigated under the action of solar gravity and solar electromagnetic radiation. As for spherical particle [Kla?ka, J., 2004. Electromagnetic radiation and motion of a particle. Cel. Mech. Dynam. Astron. 89, 1-61]: (i) perihelion motion is of the order ( is heliocentric velocity of the meteoroid and c is the speed of light in vacuum), if a component of electromagnetic radiation acceleration is considered as a part of central acceleration; (ii) perihelion motion is of the first order in if the total electromagnetic radiation force is considered as a disturbing force. The new facts presented in this paper concern irregular dust particles. Detailed numerical calculations were performed for the grains ejected at aphelion of comet Encke. Perihelion motion for irregular interplanetary dust particles exists already in the first order in for both cases of central accelerations. Moreover, perihelion motion of irregular particles exhibits both positive and negative directions during the particle orbital motion. Irregularity of the grains causes not only perihelion motion, but also dispersion of the dust in various directions, also normal to the orbital plane of the parent body. 相似文献
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The large Area Detectors (LADs) of the BATSE experiment aboard the Compton Gamma-ray Observatory have been used recently as the first hard X-ray all-sky imager at energies between 20 keV and 300 keV. The Earth occultation process is formulated in terms of a curved Radon transform convoluted by a step transform in a selected field of view (FOV) ranging from 5°×5° to 40°×40°. The Maximum Entropy Method is then used to reconstruct an image in the hard X-ray sky. Multiple images of different regions of the sky can be produced simultaneously. A source location accuracy of 0.1° for strong sources and a sensitivity limit of 100 mCrab have been achieved in an one-day integration period.Invited Paper on Imaging in High Energy Astronomy, Sept., 1994, Capri, Italyalso Universities Space Research Association 相似文献
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W. Pietsch 《Astronomische Nachrichten》2008,329(2):170-173
First studies of the X‐ray source population of M 31 were performed with the Einstein Observatory and ROSAT. High resolution Chandra Observatory images not only spatially resolved the center area but also supernova remnants (SNRs) in the galaxy. Source catalogues of restricted areas were presented with high astrometric accuracy. Also luminosity function studies and studies of individual sources based on Chandra and XMM‐Newton observations led to a better knowledge of the X‐ray source population. An XMM‐Newton source catalog based on archival observations revealed more than 850 sources down to a 0.2–4.5 keV luminosity of 1035 erg s–1. EPIC hardness ratios as well as informations from earlier X‐ray, optical, and radio catalogues were used to distinguish between different source classes (SNRs, supersoft sources (SSSs), X‐ray binaries (XRBs), globular cluster sources within M 31, and foreground stars and objects in the background). However, many sources could only be classified as “hard”. These sources may either be XRBs or Crab‐like SNRs in M 31 or background sources. Two of the globular cluster sources could be identified as low mass XRBs with a neutron star as compact object as they showed type I X‐ray bursts. Many of the SSSs were identified as optical novae. Inspired by these results an XMM‐Newton survey of the entire D25 disk of M 31 and a dedicated program to monitor X‐ray counterparts of optical novae in M 31 was started. We discuss implications for further nearby galaxy studies. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
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应用国家气象中心全球谱模式T213L31(简称T213) 及其升级版本T639L60(简称T639) 对2009—2010年西北太平洋热带气旋数值预报的结果进行对比。结果表明:T213与T639模式24～120 h预报平均距离误差基本相近,但由于T639模式分辨率较高,T639模式的热带气旋强度预报明显好于T213模式。从分类误差来看,T639模式对于西北行登陆及转向热带气旋的路径预报好于T213模式,但对西行及北上热带气旋预报误差偏大。对于异常路径热带气旋预报,T639模式能较好预报环流形势的突然调整,对路径突变的热带气旋预报比T213模式有明显优势;从登陆类热带气旋预报的移向误差来看,T213模式存在东北偏北向系统性偏差,T639模式存在东北偏东向系统性偏差。 相似文献
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Andrew Fittingoff J. Xavier Prochaska Jasonjot S. Kalirai Jay Strader † Puragra Guhathakurta Kyle F. Kaplan 《Monthly notices of the Royal Astronomical Society》2009,399(2):728-736
We have performed a wide-area ultraviolet (UV) imaging survey using the GALaxy Evolution eXplorer to search for bright, point-like UV sources behind M31's extended halo. Our survey consisted of 46 pointings covering an effective area of ≈50 deg2 , in both the far-UV and near-UV channels. We combined these data with optical R -band observations acquired with the WIYN Mosaic-1 imager on the Kitt Peak National Observatory 0.9-m WIYN telescope. An analysis of the brightness and colours of sources matched between our photometric catalogues yielded ≈100 UV-bright quasar candidates. We have obtained discovery spectra for 76 of these targets with the Kast spectrometer on the Lick 3-m telescope and confirmed 30 active galactic nuclei and quasars, 29 galaxies at z > 0.02 including several early-type systems, 16 Galactic stars (hot main-sequence stars) and one featureless source previously identified as a BL Lac object. Future UV spectroscopy of the brightest targets with the Cosmic Origins Spectrograph on the Hubble Space Telescope will enable a systematic search for diffuse gas in the extended halo of M31. 相似文献
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Yu. N. Efremov 《Astronomy Letters》2009,35(8):507-517
The fragmentation of gaseous spiral arms in the outer Galaxy into superclouds has been studied using recently published data on the HI distribution in the Galactic disk. Regular chains of superclouds have been found or confirmed in the Cygnus (Outer) and Carina arms, with the spacings between the superclouds being concentrated near 0.1 and 0.2 of the solar Galactocentric distance. The star complexes in the northwestern arm of the galaxy M31 are spaced, on average, 1.2 kpc apart, with the most distinct chain of complexes being located in the arm region where Beck et al. (1989) detected a strong and wavy (along the arm) magnetic field. Its wavelength turns out to be related to the spacing between the complexes. In this arm, the HII regions lie inside the star complexes, which, in turn, are located inside the gas-dust lane. In contrast, the southwestern arm of M31 is split into a gas-dust lane and a dense stellar arm, which is not fragmented into star complexes. Here, the HII regions are located along the boundary between the gas-dust and stellar components of the arm; other evidence for the presence of a spiral shock wave triggering star formation is also observed, which is probably attributable to the large pitch angle of this segment of the southwestern arm. It may be suggested that the shock wave rapidly leads to star formation everywhere in this arm, while in the northwestern arm, where the shock wave is absent, star formation begins in the superclouds formed along the arm by the magneto-gravitational instability. This is how the chains of star complexes in the northwestern arm of M31 and, obviously, the chains of superclouds in the Carina and Cygnus arms of our Galaxy have been formed. The detection of a regularmagnetic field in the corresponding segments of these arms can be predicted. 相似文献
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福建省天湖山煤矿区F31推覆断层及找煤方向探讨 总被引：1，自引：0，他引：1
福建省天湖山煤矿区处于闽西南坳陷东条带,推覆构造极其发育,以F31和F1两条推覆断层表现最为突出。据矿区开采资料证实,F31断层下盘童子岩组为—总体向西倾斜向南倾伏、轴向NNE的紧密线状褶皱,断层较稀少;上盘构造复杂,断层发育,由F31所派生的低序次断层往往为逆掩或逆冲断层,与主断层面组成“入”字型构造,造成童子岩组地层多次重复,同时派生了更低序次的断层组成羽毛状构造。通过对F31推覆断层特征以及应力场分析研究,认为其演进过程为：童子岩期前后的成岩沉积—印支期侧向挤压形成褶皱—印支运动及其后由于侧向挤压形成软弱滑动面及断裂—燕山早期侧向挤压造成低角度推覆断层。根据该矿区构造研究成果,提出了矿区外围及深部的5个找煤方向。 相似文献
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T213L31全球模式的云和对流参数化方案改进试验 总被引：1，自引：0，他引：1
针对中国业务中期数值预报模式T213对中雨最级以上的降水预报空报比较明显的问题,文中对此模式预报的降水进行了诊断分析.发现T213模式预报的总降水分布主要是由可分辨尺度降水决定的,且在降水偏多最明显的地区,可分辨尺度的降水即超过或达到了观测的总降水,表明降水空报的主要原因在于可分辨尺度降水偏多.可分辨尺度降水偏多的可能原因有:土壤湿度初始化、云变量的初始化和直接产生降水的云与对流参数化方案存在一定的缺陷.鉴于前两者是目前国际上的难点,文中针对第3个方面的可能原因进行了分析和相应的改进.包括在对流方案之前增加一次云方案的调用;对流参数化办案的闭合由"动力型"改为对流有效化能调整闭合;更复杂的对流触发机制;改进冰沉降和降水通量计算.改进的主要目的是使对流参数化方案更活跃,从而减少格点尺度对流的发生.采用改进的方案,进行了敏感性试验和2005年夏季的连续滚动同化预报试验,并与中国区域400个标准站的降水观测和GPCP的全球降水观测进行了比较.结果表明,改进的方案无论是对中国区域还是全球夏季平均的降水分布预报都好于业务,但四川省和赤道东太平洋降水偏多的问题依然存在.中国区域的降水统计检验还表明,除小雨外,其他量级在大部分时效七降水的Ts评分增加,预报偏差降低. 相似文献