脉冲星的射电发射

脉冲星的射电辐射与其他天体物理辐射源有很大的不同，因为它们有着极高的亮温度和高度的线或圆偏振。极高的亮温度意味着起作用的发射机制一定是相干的。至今尚无对这种辐射普遍接受的模型。本文讨论了关于脉冲星的射电辐射产生和传播研究中的新进展。     

交调干扰引起的可能被认为是射电爆发的假象

本强调动态范围是太阳射电望远镜的关键指标，以海淀区青少年科技馆的２１ｃｍ射电望远镜，１９９１年５月１６日及６月１５日的强太阳射电爆发观测资料的频谱和噪声分析结果为例，讨论了其重要性。     

微波Ⅲ型爆发与日冕物质抛射的统计分析

对国家天文台2.6～3.8GHz频谱仪在第23太阳活动周上升段(1996～1998)记录到的Ⅲ型爆发,与日冕物质抛射(CME)作了统计分析。发现微波Ⅲ型爆发可能是CME的先兆现象,并讨论了它们的辐射机制。     

毫秒级快速尖峰辐射事件的时间和频率特性

介绍了太阳22周峰年期间云南天文台米波射电频谱仪的观测结果。主要对1557个单个Spike的时间和频率分布作了统计分析，着重指出太阳快速精细结构的观测特征并定性地指出其产生机制。     

彗木碰撞期间3.6和12cm射电观测

本文介绍了1994年7月SL－9彗星撞击木星期间3．6cm和12cm射电连续谱观测的结果．在3．6cm波长上，撞击事件无明显的视效应，在12cm波长上，木星的射电平均视流量增加约20％．     

山东威海太阳物理国际研讨会(2002年8月5～12日,威海)

以国家自然科学基金委员会“九五”重点项目“太阳射电爆发频谱及其物理机制”、国家重点基础研究发展规划项目“太阳剧烈活动与空间灾害天气”子课题“太阳高能粒子的起源与输出”等研究为背     

太阳微波脉冲事件中原区加热的证据

本对具有一定空间分辨率（￣４＇）和高灵敏度（０．００４ｓｆｕ）特性的１３．７ｍ射电望远镜，在１．３５ｃｍ（２２ＧＨｚ）波段上观测到的两个脉冲事件前的周期性脉动和吸收现象进行了分析，并认为这种观测特征，可用源区局部区域的加热得到合理解释。     

日冕物质抛射的中性电流片及边源辐射对

利用日本阳光卫星上的软X－射线望远镜，硬X－射线望远镜和野边山射电日像仪1998年4月23日观测资料，对软X－射线日冕物质抛射和射电Ⅳ型爆发进行了综合研究，获得了下列有意义的结果。在2个磁偶极源之间发现了磁容带和少数的激活源。激活源将磁容带变成磁能带的过程，正是中性电流片的形成过程以及激发能量和发亮物质向它集中的过程。当2个磁偶极源被磁能带接通时，则中性电流片形成，并且发生软X－射线日冕物质抛射。物质抛射不仅从中性电流片处升起，也从整个磁能带上升起。软X－射线日冕物质抛射环具有2个足点，它们正是2个磁偶极源。膨胀环的头总是倾向于弱源的足点，因为它是来自2个足点磁压的平衡点。因此它的轨迹是中性线，由中性线便可确定中性电流片的位置。最后，发现了磁能带上中性电流片的边缘辐射对。     

Optical Flash of GRB 990123: Constraints on the Physical Parameters of the Reverse Shock

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.     

Sequences in the Hardness Ratio-Peak Energy Plane of Gamma-Ray Bursts

The narrowness of the distribution of the peak energy of the vFv spectrum of gamma-ray bursts (GRBs) and the unification of GRB populations are great puzzles yet to be solved. We investigate the two puzzles based on the global spectral behaviors of different GRB populations, the long GRBs, the short GRBs, and the X-ray flashes (XRFs), in the HR - Ep plane (HR the spectral hardness ratio) with BATSE and HETE-2 observations. It is found that the long GRBs and the XRFs observed by HETE-2 seem to follow the same sequence in the HR-Ep plane, with the XRFs at the low end of this sequence. We fit the sequence by a universal Band function, and find that this sequence is mainly defined by the low energy index α, and is insensitive to the high energy index,β. With fixed β=-5, a best fit is given by α=-1.00 with X^2min/dof=2.2. The long and short GRBs observed by BATSE follow significantly different sequences in the HR-Ep plane, with most of the short GRBs having a larger hardness ratio than the long GRBs at a given Ep. For the long GRBs a best-fit yields α=-0.30 and β=-2.05. For the short GRBs, a best fit gives α=-0.60 with x^2min=1.1 (withβfixed at-2.0 because it is numerically unstable). The α value for the short GRBs is significantly greater than that for the long GRBs. These results indicate that the global spectral behaviors of the long GRB sample and the XRF sample are similar, while that of the short GRBs is different. The short GRBs seem to be a unique subclass of GRBs, and they are not the higher energy extension of the long GRBs.