古代诗歌与太阳（二）——日出：壮景与豪情

在以前讲述“诗意的月球”篇章中,我们提到：银白色的月亮,皎洁的月光常被古代诗人作为“美的象征”用于诗词的意象中,那么太阳是否也常被诗人们当作“美的象征”呢？答案是肯定的。     

A modified stratified model for the 3C 273 jet

We present a modified stratified jet model to interpret the observed spectral energy distributions of knots in the 3C 273 jet. Based on the hypothesis of the single index of the particle energy spectrum at injection and identical emission processes among all the knots, the observed difference of spectral shape among different 3C 273 knots can be understood as a manifestation of the deviation of the equivalent Doppler factor of stratified emission regions in an individual knot from a characteristic one. The summed spectral energy distributions of all ten knots in the 3C 273 jet can be well fitted by two components: a low-energy component (radio to optical) dominated by synchrotron radiation and a high-energy component (UV, X-ray and γ-ray) dominated by inverse Compton scattering of the cosmic microwave background. This gives a consistent spectral index of α= 0.88 (Sv α v-α) and a characteristic Doppler factor of 7.4. Assuming the average of the summed spectrum as the characteristic spectrum of each knot in the 3C 273 jet, we further get a distribution of Doppler factors. We discuss the possible implications of these results for the physical properties in the 3C 273 jet. Future GeV observations with GLASTcould separate the γ-ray emission of 3C 273 from the large scale jet and the small scale jet (i.e.the core) through measuring the GeV spectrum.     

Magnetic interactions during sympathetic solar eruptions

We present the first evidence for occurrences of magnetic interactions between a jet, a filament and coronal loops during a complex event, in which two flares sequen-tially occurred at different positions of the same active region and were closely associated with two successive coronal mass ejections (CMEs), respectively. The coronal loops were located outside but nearby the filament channel before the flares. The jet, originating from the first flare during its rise phase, not only hit the filament body but also met one of the ends of the loops. The filament then underwent an inclined eruption followed by the second flare and met the same loop end once more. Both the jet and the filament erup- tion were accompanied by the development of loop disturbances and the appearances of brightenings around the meeting site. In particular, the erupting filament showed clear manifestations of interactions with the loops. After a short holdup, only its portion passed through this site, while the other portion remained at the same place. Following the fila-ment eruption and the loop disappearance, four dimmings were formed and located near their four ends. This is a situation that we define as "quadrupolar dimmings." It appears that the two flares consisted of a sympathetic pair physically linked by the interaction between the jet and the filament, and their sympathy indicated that of the two CMEs.Moreover, it is very likely that the two sympathetic CMEs were simultaneously associ-ated with the disappearing loops and the quadrupole dimmings.     

High energy neutron and pion-decay gamma-ray emissions from solar flares

Solar flare gamma-ray emissions from energetic ions and electrons have been detected and measured to GeV energies since 1980. In addition, neutrons produced in solar flares with 100 MeV to GeV energies have been observed at the Earth. These emis-sions are produced by the highest energy ions and electrons accelerated at the Sun and they provide our only direct (albeit secondary) knowledge about the properties of the acceler-ator(s) acting in a solar flare. The solar flares, which have direct evidence for pion-decaygamma-rays, are unique and are the focus of this paper. We review our current knowl-edge of the highest energy solar emissions, and how the characteristics of the acceleration process are deduced from the observations. Results from the RHESSI, INTEGRAL and CORONAS missions will also be covered. The review will also cover the solar flare ca-pabilities of the new mission, FERMI GAMMA RAY SPACE TELESCOPE, launched on 2008 June 11. Finally, we discuss the requirements for future missions to advance this vital area of solar flare physics.     

X-ray plateaus followed by sharp drops in GRBs 060413, 060522, 060607A and 080330： Further evidences for central engine afterglow from gamma-ray bursts

The X-ray afterglows of GRBs 060413, 060522, 060607A and 080330 are characterized by a plateau followed by a very sharp drop. The plateau could be explained within the framework of the external forward shock model but the sharp drop can not.We interpret the plateau as the afterglows of magnetized central engines, plausibly magnetars. In this model, the X-ray afterglows are powered by the internal magnetic energy dissipation and the sudden drop is caused by the collapse of the magnetar. Accordingly,the X-ray plateau photons should have a high linear polarization, which can be tested by future X-ray polarimetry.     

一个复杂大爆发的分析

本文分析了2002.7.23国家天文台云南天文台射电频谱仪在625～1500 MHz、2600～3800 MHz和5200～7600 MHz记录到的复杂型大爆发,将此爆发与Hα耀斑、日冕物质抛射(CME)、硬X射线爆发及地球物理参数作了相关分析,得到这个事件的一些显著特征,认为这一事件电子的加速区在日冕的外层,接近625 MHz的地方,并且多次发生磁重联.磁重联以后的衰变相是湍流加速过程.     

博州地区196 1—2006年太阳能资源的分析评估

根据太阳总辐射估算模型Q=Q0（a＋bS1）按月确定了博州地区邻近站伊宁的a、b系数,将其对应于博州地区4个站点1961～2006年逐月太阳辐射的计算,据此分析了全地区太阳总辐射的时空分布状况,并对太阳能资源按行业标准进行了评估。结果表明,46a来博州地区的太阳总辐射呈明显下降趋势,整体上冬季减少的贡献率最大;太阳总辐射与总、低云量、相对湿度、雨雪日数具有较好的相关性;造成博州地区太阳总辐射呈下降趋势的重要气候原因是：平均总、低云量,相对湿度,雨雪日数增加的综合作用;博州地区的太阳能资源较丰富,其开发利用的．综合条件较好。     

大棚小气候特征及其与大气候的关系

为了提高大棚揭闭膜气象服务的针对性,对武汉城郊冬春季棚内外气温、地温进行了逐时对比观测试验,利用相关分析及逐步回归分析方法,分3种天气类型对棚内气温、地温观测数据进行了计算分析.结果表明,在晴好天气下大棚、双层膜最高气温分别比棚外大气最高气温高20、24℃左右,夜间温度分别比棚外大气高0.8～3.5℃、3.5～6.5℃,棚内温度日较差在晴好天气下高达30～35℃,气温变化剧烈,一天内可能既要防范高温热害,又要防御低温危害.白天棚内气温与大气温度、太阳高度角关系密切,夜间气温以及10cm地温与大气温度相关显著,并由此建立了棚内气温、地温统计数学模型.利用该模型可以准确地推算或预测大棚内逐时气温、地温变化,为菜农提供大棚揭闭膜气象服务.     

加拿大科学家：海平面温度上升导致飓风大量增加

据《温哥华太阳报》2008年1月31日报道,加拿大BC省科学家通过对1996—2005年10年间北美发生的飓风进行研究,发现海平面温度的上升,增加了北美40％的飓风。该研究报告发表在最近一期《自然》杂志上。     

机载微波辐射计反演云液水含量的云物理方法

用一维层状云模式产生云样本,通过统计回归求得机载对空微波辐射计测云中路径积分液态水含量的反演系数,与用历史探空统计资料作相对湿度诊断产生云样本的反演方法进行了比较,并通过因素分析、数值模拟检验等方法对机载微波辐射计的探测误差进行估计。对2001年7月8日的个例分析表明,用云模式得到的统计样本,由于加入了对层状云物理过程的考虑,较为符合当天的实际天气情况,在一定程度上减小了由于背景大气条件、云温、云内含水量的垂直分布等的不确定性所引起的反演误差。对反演精度的数值模拟检验表明,各高度层的均方根相对误差在9.5%～12.7%之间,反演精度在所有高度上都高于原方法。对探测误差的因素分析表明,与仪器漂移及背景场引起的误差相比,由云液水垂直分布的不确定所引起的误差是不可忽略的。因此为进一步提高反演精度,根据实际宏观观测资料,对云模式产生的大量样本进行筛选,从中选取与实际云况较为符合的云样本进行拟合,结果表明,采用这一措施可以使反演精度得到进一步改善。