X射线和射电的暂现源

X射线和射电的暂现源可能是一个密近双星体系,子星A具有弱磁场,子星B为中子星。当子星A的物质抛射率大大增强时,子星B的吸积率也相应地大大增强而引起X射线耀;如果子星A同时抛出相对论性电子,它们在子星A的磁场中将产生同步加速辐射,因而同时出现射电耀。     

新核素263Hs,260Bh及其α衰变链上核素的半衰期

运用推广的液滴模型(GLDM)并结合量子力学中的WKB方法计算了新核素263Hs,260Bh及其α衰变链上各核素的势垒贯穿概率,对该链上各原子核的α衰变半衰期进行了研究.计算结果表明:利用推广的液滴模型结合WKB方法计算出的α衰变半衰期可以很好地符合在超重核区的实验值,验证了推广的液滴模型在超重核区的适用性,能够很好地描述超重核的α衰变.同时,计算表明新核素260Bh和263Hs的合成及其半衰期的测量是可靠的.     

2维和4维时空温度弦模型中暗能量玻色子星质量和物态参量的计算

通过2维和4维温度弦模型研究暗能量玻色子星的质量和物态参量,推导高亏格黎曼面上的玻色弦自由能,获得引力场方程和dilaton暗能量场方程的表达式,给出玻色子星的质量和物态参量的推导过程.另外,还分析和比较了不同时空中计算结果所具有的特点.     

星体自转动力的推导

利用经典力学,对做公转运动的子星进行受力分析,揭示了星体自转动力的产生。首先对无液核固态小星体进行受力分析,得出这种固态小星体在自转力矩作用下,最终将使小星体的自转周期与公转周期达到同步运行。并得出月球轻的一面朝向地球的结论。应用该特性,将大大简化同步通信卫星姿态指向的控制装置。纠正了潮汐力将使月球远离的错误观点。其次是对有液核的类似球体的大星体进行分析,得出作用在子星上的引力差和子星的公转运动使子星产生自转力矩,且其力矩使子星加速自转。并推导出自转加速方程。揭示了宇宙诸天体几乎都沿同一方向转动的原因。考虑自转力矩随星体半径增大而略有增加,对有液核大星体内部的涡旋运动的形成机理进行了简要阐述。     

前身星与Ⅱ型超新星爆发的数值模拟

利用考虑物质回落与混合效应的前身星输入数据,在一维球对称瞬时爆发模型下数值模拟了质量为12～15 M⊙Ⅱ型超新星的星核坍缩、激波传播、爆发能量等过程.计算结果表明:前身星的星核质量、密度、温度、物质构成等对Ⅱ型超新星爆发有重要影响,不过,数值模拟仍不能实现超新星的瞬时爆发.     

高能天体物理对某些物理基础的检验及启示

首先简要介绍天文学中的某些新探索;其次讨论天体磁场和天文学中可能存在的电磁广义相对论;第三研究高能天体物理和Pauli不相容原理(PEP)的适用性;第四探讨天文学中能够提供的信息,提出太阳系中各个行星的偏心率、天体演化方向等问题,并且讨论太阳中微子和新模型;第五探索γ射线暴(GRB)和轻子星;最后讨论宇宙时间,探讨地球的最终命运和人类可能的宇航.     

密近双星的Roche势的计算

文章对密近双星的Roche势进行分析,并计算出3个内、外拉格朗日点及其相应的Roche势.根据Roche势对密近双星进行分类,这对于探寻3类密近双星的演化联系起重要作用.当子星充满内(或外)临界等势面必定会发生质量和角动量的转移或损失,从而引起质量和角动量在两子星间的重新分布并最终导致双星并合.Roche势的计算对于密近双星的观测、分析和研究具有重要意义.     

基于强化学习的能量采集物联网视频编码技术

物联网设备的视频压缩码率和量化参数等编码方案决定着视频质量和物联网设备的使用寿命.针对未知视频传输模型和能量采集模型的物联网设备,提出一种基于强化学习的视频编码方案,能够动态优化视频编码码率和量化参数.该技术根据物联网设备的无线信道带宽、电池水平和采集的能量,结合反馈的视频质量和时延等信息,采用强化学习算法优化选择视频编码码率和量化参数.在动态的网络环境下,物联网设备不需预知视频传输模型就可以综合优化视频质量和设备能量损耗.仿真结果表明,该方案可以提高视频质量,降低设备能量损耗和时延,改善物联网设备效益.     

绳系卫星的动态释放变轨

动态释放变轨是绳系卫星特有的变轨方式,变轨结果好于静态释放,但相应控制还未有深入的研究.该文利用Kelvin-Tait-Chatayev定理设计了线性控制律,可以在数小时内动态释放子星.并进一步分析了圆轨道下动态释放和静态释放后的变轨结果,证明了子星动态释放后,远地点改变比静态释放大.数值仿真的结果是动态释放变轨的远地点升高是静态释放变轨的2.5倍.结果表明,此控制律可以实现动态释放变轨,并使子星轨道发生较大变化,具有重要的应用价值.     

强钡星和弱钡星的比较

利用星风吸积模型,计算了钡星的初始质量和AGB伴星的金属丰度对弱钡星和强钡星超丰因子的影响,计算了弱钡星和强钡星重元素(Y,Nd)丰度随轨道周期终值的变化,并和观测值作了比较.由此得出结论:强钡星和弱钡星的区别主要是金属丰度不同(即年代不同),而不是轨道距离;弱钡星和强钡星相比,属于较年轻、质量较大、金属丰度较丰富的星族;这就意味,s-元素的核合成在低金属丰度星族更有效产生.     

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.     

Suppression of star formation in early-type galaxies by feedback from supermassive black holes

Detailed high-resolution observations of the innermost regions of nearby galaxies have revealed the presence of supermassive black holes. These black holes may interact with their host galaxies by means of 'feedback' in the form of energy and material jets; this feedback affects the evolution of the host and gives rise to observed relations between the black hole and the host. Here we report observations of the ultraviolet emissions of massive early-type galaxies. We derive an empirical relation for a critical black-hole mass (as a function of velocity dispersion) above which the outflows from these black holes suppress star formation in their hosts by heating and expelling all available cold gas. Supermassive black holes are negligible in mass compared to their hosts but nevertheless seem to play a critical role in the star formation history of galaxies.     

Birth of a relativistic outflow in the unusual γ-ray transient Swift J164449.3+573451

Active galactic nuclei, which are powered by long-term accretion onto central supermassive black holes, produce relativistic jets with lifetimes of at least one million years, and the observation of the birth of such a jet is therefore unlikely. Transient accretion onto a supermassive black hole, for example through the tidal disruption of a stray star, thus offers a rare opportunity to study the birth of a relativistic jet. On 25 March 2011, an unusual transient source (Swift J164449.3+573451) was found, potentially representing such an accretion event. Here we report observations spanning centimetre to millimetre wavelengths and covering the first month of evolution of a luminous radio transient associated with Swift J164449.3+573451. The radio transient coincides with the nucleus of an inactive galaxy. We conclude that we are seeing a newly formed relativistic outflow, launched by transient accretion onto a million-solar-mass black hole. A relativistic outflow is not predicted in this situation, but we show that the tidal disruption of a star naturally explains the observed high-energy properties and radio luminosity and the inferred rate of such events. The weaker beaming in the radio-frequency spectrum relative to γ-rays or X-rays suggests that radio searches may uncover similar events out to redshifts of z?≈?6.     

Rapid X-ray flaring from the direction of the supermassive black hole at the Galactic Centre.

The nuclei of most galaxies are now believed to harbour supermassive black holes. The motions of stars in the central few light years of our Milky Way Galaxy indicate the presence of a dark object with a mass of about 2.6 x 106 solar masses (refs 2, 3). This object is spatially coincident with the compact radio source Sagittarius A* (Sgr A*) at the dynamical centre of the Galaxy, and the radio emission is thought to be powered by the gravitational potential energy released by matter as it accretes onto a supermassive black hole. Sgr A* is, however, much fainter than expected at all wavelengths, especially in X-rays, which has cast some doubt on this model. The first strong evidence for X-ray emission was found only recently. Here we report the discovery of rapid X-ray flaring from the direction of Sgr A*, which, together with the previously reported steady X-ray emission, provides compelling evidence that the emission is coming from the accretion of gas onto a supermassive black hole at the Galactic Centre.     

Energy input from quasars regulates the growth and activity of black holes and their host galaxies

In the early Universe, while galaxies were still forming, black holes as massive as a billion solar masses powered quasars. Supermassive black holes are found at the centres of most galaxies today, where their masses are related to the velocity dispersions of stars in their host galaxies and hence to the mass of the central bulge of the galaxy. This suggests a link between the growth of the black holes and their host galaxies, which has indeed been assumed for a number of years. But the origin of the observed relation between black hole mass and stellar velocity dispersion, and its connection with the evolution of galaxies, have remained unclear. Here we report simulations that simultaneously follow star formation and the growth of black holes during galaxy-galaxy collisions. We find that, in addition to generating a burst of star formation, a merger leads to strong inflows that feed gas to the supermassive black hole and thereby power the quasar. The energy released by the quasar expels enough gas to quench both star formation and further black hole growth. This determines the lifetime of the quasar phase (approaching 100 million years) and explains the relationship between the black hole mass and the stellar velocity dispersion.     

对粒子物理标准模型的重新审视

 鉴于当前实验研究结果不断地给基本粒子标准模型提出疑难,揭示轻子、夸克存在亚结构的迹象,例如EMC效应预示轻核与重核之间存在差异,pp碰撞单举截面分布在横能E_T>200 GeV时与QCD计算发生较大偏差,发现了反轻子-夸克共振事例,先后发现了夸克的味变中性流和轻子的味变中性流,轻子的"反常量"等等.这些实验迹象都迫使我们有必要及时对基本粒子标准模型进行一番全面、系统的审视.     

An ultraviolet-optical flare from the tidal disruption of a helium-rich stellar core

The flare of radiation from the tidal disruption and accretion of a star can be used as a marker for supermassive black holes that otherwise lie dormant and undetected in the centres of distant galaxies. Previous candidate flares have had declining light curves in good agreement with expectations, but with poor constraints on the time of disruption and the type of star disrupted, because the rising emission was not observed. Recently, two 'relativistic' candidate tidal disruption events were discovered, each of whose extreme X-ray luminosity and synchrotron radio emission were interpreted as the onset of emission from a relativistic jet. Here we report a luminous ultraviolet-optical flare from the nuclear region of an inactive galaxy at a redshift of 0.1696. The observed continuum is cooler than expected for a simple accreting debris disk, but the well-sampled rise and decay of the light curve follow the predicted mass accretion rate and can be modelled to determine the time of disruption to an accuracy of two days. The black hole has a mass of about two million solar masses, modulo a factor dependent on the mass and radius of the star disrupted. On the basis of the spectroscopic signature of ionized helium from the unbound debris, we determine that the disrupted star was a helium-rich stellar core.     

Relativistic jet activity from the tidal disruption of a star by a massive black hole

Supermassive black holes have powerful gravitational fields with strong gradients that can destroy stars that get too close, producing a bright flare in ultraviolet and X-ray spectral regions from stellar debris that forms an accretion disk around the black hole. The aftermath of this process may have been seen several times over the past two decades in the form of sparsely sampled, slowly fading emission from distant galaxies, but the onset of the stellar disruption event has not hitherto been observed. Here we report observations of a bright X-ray flare from the extragalactic transient Swift J164449.3+573451. This source increased in brightness in the X-ray band by a factor of at least 10,000 since 1990 and by a factor of at least 100 since early 2010. We conclude that we have captured the onset of relativistic jet activity from a supermassive black hole. A companion paper comes to similar conclusions on the basis of radio observations. This event is probably due to the tidal disruption of a star falling into a supermassive black hole, but the detailed behaviour differs from current theoretical models of such events.     

A star in a 15.2-year orbit around the supermassive black hole at the centre of the Milky Way

Many galaxies are thought to have supermassive black holes at their centres-more than a million times the mass of the Sun. Measurements of stellar velocities and the discovery of variable X-ray emission have provided strong evidence in favour of such a black hole at the centre of the Milky Way, but have hitherto been unable to rule out conclusively the presence of alternative concentrations of mass. Here we report ten years of high-resolution astrometric imaging that allows us to trace two-thirds of the orbit of the star currently closest to the compact radio source (and massive black-hole candidate) Sagittarius A*. The observations, which include both pericentre and apocentre passages, show that the star is on a bound, highly elliptical keplerian orbit around Sgr A*, with an orbital period of 15.2 years and a pericentre distance of only 17 light hours. The orbit with the best fit to the observations requires a central point mass of (3.7 +/- 1.5) x 10(6) solar masses (M(*)). The data no longer allow for a central mass composed of a dense cluster of dark stellar objects or a ball of massive, degenerate fermions.     

An ultra-relativistic outflow from a neutron star accreting gas from a companion

Collimated relativistic outflows-also known as jets-are amongst the most energetic phenomena in the Universe. They are associated with supermassive black holes in distant active galactic nuclei, accreting stellar-mass black holes and neutron stars in binary systems and are believed to be responsible for gamma-ray bursts. The physics of these jets, however, remains something of a mystery in that their bulk velocities, compositions and energetics remain poorly determined. Here we report the discovery of an ultra-relativistic outflow from a neutron star accreting gas within a binary stellar system. The velocity of the outflow is comparable to the fastest-moving flows observed from active galactic nuclei, and its strength is modulated by the rate of accretion of material onto the neutron star. Shocks are energized further downstream in the flow, which are themselves moving at mildly relativistic bulk velocities and are the sites of the observed synchrotron emission from the jet. We conclude that the generation of highly relativistic outflows does not require properties that are unique to black holes, such as an event horizon.