γ暴辐射谱吸收特征的电子回旋共振吸收模型

运用半径典量子理论的电子回旋共振吸收系数,由辐射转移方程计算了通过磁中子星表面附近等离子休后的辐射谱,与γ射线暴的观测谱符合得很好。结果表明,有吸收特征辐射谱的γ射线暴可能是由强磁场的中子星产生的。     

老年中子星的核闪及宇宙γ爆

本文对老年中子星吸积星际介质而可能产生的核闪作了初步计算,得出可能爆发核闪的条件,对于吸积表层中的富氢层、富氦层、富碳层和富氧层,临界密度分别等于1.7×10~6、6.6×10~8、4.2×10~(10)和2.6×10~(11)克/厘米~3。对于质量M=1M的典型中子星所作的计算表明,在富氢层中爆发一次核闪释放的能量约为10~(41)尔格,相邻两次核闪的时间间隔约为10~3年。这与观测到的宇宙γ爆的某些特征相符。     

宇宙γ射线爆的恒星“耀斑”模型

对宇宙γ射线爆提出了如下的模型:宇宙γ射线爆发类似于太阳耀斑过程,但猛烈程度大得多;爆发时贮存在“耀斑”内的磁能转化为电子的动能;大量的高能电子在一个很短的时间内从“耀斑”飞出;这些高能电子在通过恒星周围的光子气体时,与光子气体相互碰撞,产生逆康普顿光子,形成γ射线爆。根据这一模型推导了γ射线爆的时间轮廓、能谱等的表达式,并对1972年4月27日事件作了应用。计算结果表明:在磁白矮星和O、B型热星上都可能出现γ射线爆。     

γ爆与星系群、星系对及射电星系的交叉相关分析

分析了强γ爆和弱γ爆分别与星系群、星系对及射电星系之间的交又相关特性,发现强γ爆与星系群在中心角距离θ=15°的间隔内有1σ以上的交叉相关,而弱γ爆与星系群在中心角距离θ=5°、15°的间隔内发现有1σ以上的负交叉相关。分析结果还表明:强γ爆和弱γ爆与星系对、射电星系之间都不存在交叉相关。     

1978年3月25日γ射线爆源区特性

釆用3种辐射分量来拟合典型的γ爆GB780325的观测能谱.这3种辐射分量分别是:起源于同一辐射区的同步辐射谱和正负电子对湮灭谱,以及从源区逃逸出来的正电子所形成的成束粒子系的同步辐射谱.由拟合参数,获得以下源区物理特性:磁场B=4.3×10~8T,电子密度n_(?)≈6.12×10~(28)cm~(-3),源区厚度τ≈2.45×10~(-5)cm,源距离d≈0.975Mpc.     

γ射线爆(GRB)研究进展及其几种模型的讨论

观测结果表明，γ射线爆源空间分布是各向同性但不均匀的，说明γ射线爆起源于宇宙学距离。本文介绍γ射线爆的观测情况和分类，并讨论了几种比较流行的γ射线爆理论模型。     

γ爆与不同深度的星系团子样本的交叉相关特性

我们分析了强γ爆和弱γ爆分别与不同深度的星系团子样本的交叉相关特性.发现强γ爆与D≤4、0=5 6的星系团子样本在中心距离θ=5°的间隔内都存在1σ以上的交叉相关,而弱爆与这两个星系团子样本之间则没有发现任何交叉相关.     

Blazar的γ射线和低频射电6cm波段辐射关系研究

给出了一个带有射电5 GHz和γ射线辐射流量密度的含有94个γ噪Blazar的大样本,其中有66个FSRQs,20个BL Lac天体,利用该样本研究了射电5 GHz和γ射线流量最大值,最小值以及平均值之间的辐射相关.结果表明:γ射线流量最大值和平均值与射电5GHz辐射有较强的相关,最大相关系数r=0.651,置信度均好于10-4;γ射线流量最小值与射电辐射之间没有相关;3C273辐射的最大值不是爆发态时的观测值,若令γ射线谱指数αG=1.0,则3C273的最大辐射流量为(450.8±39.4)×10-8photon.cm-2.s-1.因此,Blazar的γ射线辐射与低频射电辐射确有关联,γ射线的辐射应来自同步加速自康普顿辐射过程.     

γ暴能谱硬度系数的分布及其分类特征

采用非参量化线性相关性分析方法分析康顿空间天文台（CGRO）上的BATSE仪器观测到的γ暴不同能道流量间的相关性，提出新的γ暴能谱硬度系数的定义，并分析其分布特征，进一步证实了γ蛤谱硬度系数与持续时间之间的反相关性，并对这个反相关性提出新的解释，软谱长暴，短暴硬谱，同时，从定量上给出按谱硬度系数对γ暴进行分类的依据，提出了γ暴新的分类方法。     

14.9MeV中子和天然铜相互作用中γ辐射的精细研究

利用快中子核反应的全γ辐射测量技术研究了 14 9MeV中子与天然铜反应在 5 5°和90°这 2个角度上的分立γ射线谱 ,由高分辨γ分析程序识别了 10 7条谱线 ;定出了每条谱线在这 2个角度上的微分截面以及相应的反应类型和跃迁能级 ,发现谱线主要来自6 3 Cu(n ,2nγ) 6 2 Cu ,6 5Cu(n ,2nγ) 6 4Cu ,6 3 Cu(n ,n′γ) 6 3 Cu等反应道 .通过分析天然铜的活化本底谱 ,可以看出它是快中子核反应中的最理想的屏蔽材料之一 .     

A neutron-star-driven X-ray flash associated with supernova SN 2006aj

Supernovae connected with long-duration gamma-ray bursts (GRBs) are hyper-energetic explosions resulting from the collapse of very massive stars ( approximately 40 M\circ, where M\circ is the mass of the Sun) stripped of their outer hydrogen and helium envelopes. A very massive progenitor, collapsing to a black hole, was thought to be a requirement for the launch of a GRB. Here we report the results of modelling the spectra and light curve of SN 2006aj (ref. 9), which demonstrate that the supernova had a much smaller explosion energy and ejected much less mass than the other GRB-supernovae, suggesting that it was produced by a star whose initial mass was only approximately 20 M\circ. A star of this mass is expected to form a neutron star rather than a black hole when its core collapses. The smaller explosion energy of SN 2006aj is matched by the weakness and softness of GRB 060218 (an X-ray flash), and the weakness of the radio flux of the supernova. Our results indicate that the supernova-GRB connection extends to a much broader range of stellar masses than previously thought, possibly involving different physical mechanisms: a 'collapsar' (ref. 8) for the more massive stars collapsing to a black hole, and magnetic activity of the nascent neutron star for the less massive stars.     

A new gamma-ray burst classification scheme from GRB 060614

Gamma-ray bursts (GRBs) are known to come in two duration classes, separated at approximately 2 s. Long-duration bursts originate from star-forming regions in galaxies, have accompanying supernovae when these are near enough to observe and are probably caused by massive-star collapsars. Recent observations show that short-duration bursts originate in regions within their host galaxies that have lower star-formation rates, consistent with binary neutron star or neutron star-black hole mergers. Moreover, although their hosts are predominantly nearby galaxies, no supernovae have been so far associated with short-duration GRBs. Here we report that the bright, nearby GRB 060614 does not fit into either class. Its approximately 102-s duration groups it with long-duration GRBs, while its temporal lag and peak luminosity fall entirely within the short-duration GRB subclass. Moreover, very deep optical observations exclude an accompanying supernova, similar to short-duration GRBs. This combination of a long-duration event without an accompanying supernova poses a challenge to both the collapsar and the merging-neutron-star interpretations and opens the door to a new GRB classification scheme that straddles both long- and short-duration bursts.     

The unusual gamma-ray burst GRB 101225A explained as a minor body falling onto a neutron star

The tidal disruption of a solar-mass star around a supermassive black hole has been extensively studied analytically and numerically. In these events, the star develops into an elongated banana-shaped structure. After completing an eccentric orbit, the bound debris falls into the black hole, forming an accretion disk and emitting radiation. The same process may occur on planetary scales if a minor body passes too close to its star. In the Solar System, comets fall directly into our Sun or onto planets. If the star is a compact object, the minor body can become tidally disrupted. Indeed, one of the first mechanisms invoked to produce strong gamma-ray emission involved accretion of comets onto neutron stars in our Galaxy. Here we report that the peculiarities of the 'Christmas' gamma-ray burst (GRB 101225A) can be explained by a tidal disruption event of a minor body around an isolated Galactic neutron star. This would indicate either that minor bodies can be captured by compact stellar remnants more frequently than occurs in the Solar System or that minor-body formation is relatively easy around millisecond radio pulsars. A peculiar supernova associated with a gamma-ray burst provides an alternative explanation.     

A very energetic supernova associated with the gamma-ray burst of 29 March 2003

Over the past five years evidence has mounted that long-duration (>2 s) gamma-ray bursts (GRBs)-the most luminous of all astronomical explosions-signal the collapse of massive stars in our Universe. This evidence was originally based on the probable association of one unusual GRB with a supernova, but now includes the association of GRBs with regions of massive star formation in distant galaxies, the appearance of supernova-like 'bumps' in the optical afterglow light curves of several bursts and lines of freshly synthesized elements in the spectra of a few X-ray afterglows. These observations support, but do not yet conclusively demonstrate, the idea that long-duration GRBs are associated with the deaths of massive stars, presumably arising from core collapse. Here we report evidence that a very energetic supernova (a hypernova) was temporally and spatially coincident with a GRB at redshift z = 0.1685. The timing of the supernova indicates that it exploded within a few days of the GRB, strongly suggesting that core-collapse events can give rise to GRBs, thereby favouring the 'collapsar' model.     

An origin for short gamma-ray bursts unassociated with current star formation

Two short (< 2 s) gamma-ray bursts (GRBs) have recently been localized and fading afterglow counterparts detected. The combination of these two results left unclear the nature of the host galaxies of the bursts, because one was a star-forming dwarf, while the other was probably an elliptical galaxy. Here we report the X-ray localization of a short burst (GRB 050724) with unusual gamma-ray and X-ray properties. The X-ray afterglow lies off the centre of an elliptical galaxy at a redshift of z = 0.258 (ref. 5), coincident with the position determined by ground-based optical and radio observations. The low level of star formation typical for elliptical galaxies makes it unlikely that the burst originated in a supernova explosion. A supernova origin was also ruled out for GRB 050709 (refs 3, 31), even though that burst took place in a galaxy with current star formation. The isotropic energy for the short bursts is 2-3 orders of magnitude lower than that for the long bursts. Our results therefore suggest that an alternative source of bursts--the coalescence of binary systems of neutron stars or a neutron star-black hole pair--are the progenitors of short bursts.     

γ射线暴火球模型的光学余辉辐射

按照γ射线暴火球模型的动力学演化规律,利用相对论电子在磁场中作同步加速辐射时谱分布的特点,用求峰值频率辐射的方法,计算了γ射线暴红光波段余辉辐射流量随时间的变化与γ射线暴GRB970228的观测结果比较,符合甚好,说明同步加速辐射是γ射线暴余辉主要的辐射机制,也进一步证明了火球模型的正确。     

掺杂的有机薄膜电致发光

用DCM染料和香豆素染料掺杂,成功地实现了有机薄膜电致发光颜色的改变,得到了从蓝绿到红色的发光,同时提高了器件的发光亮度,用不同区域掺杂方法,分析讨论了电致发光的机理,探讨了激子的产生区域和复合区域。     

Δ共振态存在于中子星内部的可能性探讨

本文通过相对论平均场理论和Tolman-Oppenheimer-Volkoff方程来研究中子星的微观和宏观性质。与最新的脉冲星J1614-2230的观测数据作比照,可以发现除了传统的中子星物质外,Δ共振态中的Δ-和Δ0粒子也很可能大量存在于PSR J1614-2230的内部。另外,也进一步探讨了Δ共振态对中子星所产生的影响。     

MEVVA源引出离子束流分布均匀性的初步研究

通过采用加会切磁场、增大离子源阴极与阳极距离并限制源等离子体发射角，从而使源阳极电位高于等离子体电位和采用改变源阳极结构──仅用阳极筒──从而改变弧放电路径这３种方法，对改善ＭＥＶＶＡ源引出离子束流密度分布的均匀性进行了初步的研究。第３种方法从根本上改变了ＭＥＶＶＡ源引出束分布的高斯分布特性，在合适的条件下可能得到更为均匀的束流密度分布。