排序方式： 共有44条查询结果，搜索用时 156 毫秒
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Yi-Zhong Fan Zi-Gao Dai Yong-Feng Huang Tan Lu Department of Astronomy Nanjing University Nanjing 《中国天文和天体物理学报》2002,2(5):449-453
The optical flash accompanying GRB 990123 is believed to be powered by the reverse shock of a thin shell. With the best-fit physical parameters for GRB 990123 and the assumption that the parameters in the optical flash are the same as in the afterglow, we show that: 1) the shell is thick rather than thin, and we have provided the light curve for the thick shell case which coincides with the observation; 2) the theoretical peak flux of the optical flash accounts for only 3×10~-4 of the observed. In order to remove this discrepancy, the physical parameters, the electron energy and magnetic ratios, εe and εB, should be 0.61 and 0.39, which are very different from their values for the late afterglow. 相似文献
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分析IP电话的国内外发展状况,探讨IP电话的发展趋势,研究中国政府及IP电话运营商应采用的应对策略,通过研究和分析,为IP电话下一步发展战略提供参考作用。 相似文献
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基于我国对湿地的认知变化及保护历程,结合第二次全国湿地普查结果,分析当前我国湿地保护中存在的主要问题,并提出针对性建议,主要包括:落实保护红线、创新保护格局;完善法律法规、推进湿地保护绩效考核;实施生态补偿机制、提升湿地造血功能;加强科技支撑及人才建设、建立智能管理体系;宣扬湿地文化,推进社会主流生态价值观形成等。 相似文献
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当奇异星表面的电场不足以支撑整个壳层的时候,壳层就有可能全部落入奇异核中.对这一过程的研究,可以为观测上证认奇异星提供一些可能的理论线索.数值计算表明,底部密度为-8.3×1010gcm-3,亦即质量为-3 4×10-6M(?)的壳层在约5.4×10-3s时间内塌缩到奇异核中,可导致一次持续约0.15s的爆发事件.在过程中平均每个重子释放约6.3 MeV的能量,总辐射能则可高达-1046-1047ergs.这可以用来解释宇宙中一些爆发现象. 相似文献
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Fast radio bursts(FRBs) are bright radio pulses from the sky with millisecond durations and Jansky-level flux densities. Their origins are still largely uncertain. Here we suggest a new model for FRBs. We argue that the collision of a white dwarf with a black hole can generate a transient accretion disk, from which powerful episodic magnetic blobs will be launched. The collision between two consecutive magnetic blobs can result in a catastrophic magnetic reconnection, which releases a large amount of free magnetic energy and forms a forward shock. The shock propagates through the cold magnetized plasma within the blob in the collision region, radiating through the synchrotron maser mechanism,which is responsible for a non-repeating FRB signal. Our calculations show that the theoretical energetics, radiation frequency, duration timescale and event rate can be very consistent with the observational characteristics of FRBs. 相似文献
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Yu Yu Yong-Feng Huang 《中国天文和天体物理学报》2007,7(5):669-674
With the successful launch of Swift satellite,more and more data of early X-ray afterglows from short gamma-ray bursts have been collected.Some interesting features such as unusual afterglow light curves and unexpected X-ray flares are revealed.Especially,in some cases,there is a fiat segment in the X-ray afterglow light curve.Here we present a simplified model in which we believe that the flattening part is due to energy injection from the central engine.We assume that this energy injection arises from the magnetic dipole radiation of a millisecond pulsar formed after the merger of two neutron stars.We check this model with the short GRB 060313.Our numerical results suggest that energy injection from a millisecond magnetar could make part of the X-ray afterglow light curve flat. 相似文献
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Using the generic hydrodynamic model of gamma-ray burst(GRB) afterglows, we calculate the radio afterglow light curves of low luminosity, high luminosity,failed and standard GRBs in different observational bands of FAST’s energy window.The GRBs are assumed to be located at different distances from us. Our results rank the detectability of GRBs in descending order as high luminosity, standard, failed and low luminosity GRBs. We predict that almost all types of radio afterglows except those of low luminosity GRBs could be observed by a large radio telescope as long as the domains of time and frequency are appropriate. It is important to note that FAST can detect relatively weak radio afterglows at a higher frequency of 2.5 GHz for very high redshift up to z = 15 or even more. Radio afterglows of low luminosity GRBs can only be detected after the completion of the second phase of FAST. FAST is expected to significantly expand the sample of GRB radio afterglows in the near future. 相似文献
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为确定高邮凹陷北斜坡戴南组油藏的成藏期次,采用流体包裹体测温技术,对研究区3口井的流体包裹体特征和均一温度进行了分析。结果表明,该区戴南组储层流体包裹体分为盐水包裹体和有机包裹体;均一温度呈1期连续分布,主峰温在90～100℃。根据包裹体均一温度、地层埋藏史和热史,推测该区戴南组油气成藏时对应的地质年代约为垛二段沉积末期。结合圈闭发育史和烃源岩生排烃史等分析,最终确定研究区戴南组为1期成藏,时间为垛二段沉积末期。 相似文献