太阳活动研究的现状和未来

简要介绍了国内外太阳活动研究的现状 ,指出由于太阳活动对地球和人类生活的影响 ,尤其是随着空间探测和技术的发展 ,对太阳活动研究的需求更加迫切 ,太阳活动研究受到各国政府和社会更大的重视。在这样的背景下 ,加上各种高新技术和卫星探测的进步 ,2 1世纪将迎来太阳活动研究的新时代。文中对我国未来太阳活动研究的方向、重点和措施也提出了建议。     

Ultraluminous X-ray source populations in normal galaxies: a preliminary survey with Chandra

We present results of a Chandra survey of the ultraluminous X-ray sources (ULX) in 13 normal galaxies, in which we combine source detection with X-ray flux measurement. 22 ULX were detected, i.e. with   L _x > 1 × 10³⁹ erg s⁻¹ ( L ₁₀)  and 39 other sources were detected with   L _x > 5 × 10³⁸ erg s⁻¹ ( L ₅)  . We also use radial intensity profiles to remove extended sources from the sample. The majority of sources are not extended, which for a typical distance constrains the emission region size to less than 50 pc. X-ray colour–colour diagrams and spectral fitting results were examined for indicators of the ULX nature. In the case of the brighter sources, spectral fitting generally requires two-component models. In only a few cases do colour–colour diagrams or spectral fitting provide evidence of a black hole nature. We find no evidence of a correlation with stellar mass, however, there is a strong correlation with star formation as indicated by the 60-μm flux as found in previous studies.     

Sgr A*的结构和变化:银河中心的超大质量黑洞

银河中心为我们提供了一个唯一的天体物理实验室来用以研究各式各样的天体物理过程。在文中 ,我们总结和归纳了关于SgrA 观测的最新结果 ,主要涉及源的结构和在流量密度方面的变化。SgrA 现象代表着在低光度活动星系核中围绕一个超大质量黑洞的低辐射率的吸积盘外流的典型例子。从SgrA 观测得到的许多天体物理中悬而未决的问题对现存的天体物理理论是一个挑战。对SgrA 的最新理论模型也作了综述。     

The unusual supernova remnant surrounding the ultraluminous X-ray source IC 342 X-1

We report the results of an observation of a large-diameter (110 pc) supernova remnant (SNR) found to encircle the position of the ultraluminous X-ray source (ULX) IC 342 X-1. The inferred initial energy input to the SNR is at least 2–3 times greater than the canonical energy for an 'ordinary' SNR. Two regions on the inside of the shell are bright in [O iii ]λ5007 emission, possibly as the result of X-ray photoionization by the ULX. If this is the case, then the morphology of this nebulosity implies that the X-ray emission from the ULX is anisotropic. The presence of the ULX, most probably a black hole X-ray binary, within an unusually energetic SNR suggests that we may be observing the aftermath of a gamma-ray burst, although other origins for the energetic nebula are discussed.     

Magnetic aggregation: II. Laboratory and microgravity experiments

In a previous publication (Dominik and Nübold, 2002, Icarus 157, 173-186), we presented analytical expressions and theoretical considerations concerning preplanetary dust aggregation with magnetized grains in the solar nebula. The present work is dedicated to the experimental study of magnetic aggregation in a ground-based laboratory as well as under microgravity conditions on parabolic flights. We conducted aggregation experiments with dust analogues in order to study the temporal evolution and the structural outcome of grain growth processes dominated by or comprising exclusively magnetic grains. Within aggregation times ranging from a couple of seconds to a few minutes only, formation of huge chain-like and/or web-like dust aggregates was observed. After aggregate retrieval we were able to study the sizes and structures of the aggregates in great detail. We established the fractal dimension of the aggregates as D_fs=1.20±0.05 for single chains and D_fc=1.50±0.21 for inter-connected web-like structures. This is considerably lower than for non-magnetic grain growth. The dynamic exponent z for the mass increase with time according to t^z was found to be z=2.7 from in-situ video images of the microgravity aggregation runs. The results are compared with the theoretical considerations presented earlier as well as with previous experimental work on the same and on related topics, respectively.     

Discovery of Five Narrow－Line Seyfert 1 Galaxies and Implications on the NLS1 Model

We report the discovery of five Narrow-Line Seyfert 1 galaxies (NLSls) identified from the ROSAT All-Sky Survey bright sources. One of them has a quasarlike luminosity and two, including the quasar-like one, have close companions and/or show interacting features. We calculate the central black hole masses and Eddington ratios for the five NLSls. In combination with the objects of Kaspi et al., we find that NLSls have smaller central black hole masses and higher accretion rate than normal Seyfert ls.     

A quasi-spherical inner accretion flow in Seyfert galaxies?

We study a phenomenological model for the continuum emission of Seyfert galaxies. In this quasi-spherical accretion scenario, the central X-ray source is constituted of a hot spherical plasma region surrounded by spherically distributed cold dense clouds. The cold material is radiatively coupled with the hot thermal plasma. Assuming energy balance, we compute the hard X-ray spectral slope Γ and the reflection amplitude R . This simple model enables us to reproduce both the range of observed hard X-ray spectral slopes and the reflection amplitude R . It also predicts a correlation between R and Γ that is very close to what is observed. Most of the observed spectral variations from source to source would be caused by differences in the cloud covering fraction. If some internal dissipation process is active in the cold clouds, darkening effects may provide a simple explanation for the observed distributions of reflection amplitudes, spectral slopes and ultraviolet to X-ray flux ratios.