Testing the no-hair theorem with observations of black holes in the electromagnetic spectrum

According to the no-hair theorem, astrophysical black holes are uniquely described by their mass and spin. In this paper, we review a new framework for testing the no-hair hypothesis with observations in the electromagnetic spectrum. The approach is formulated in terms of a Kerr-like spacetime containing a quadrupole moment that is independent of both mass and spin. If the no-hair theorem is correct, then any deviation from the Kerr metric quadrupole has to be zero. We show how upcoming VLBI imaging observations of Sgr A∗ as well as spectroscopic observations of iron lines from accreting black holes with IXO may lead to the first astrophysical test of the no-hair theorem.     

Limit cycles of accretion disks in the Rapid Burster and GRS 1915+105

The Rapid Burster is known to show rapidly repetitive bursts (Type II bursts). An interesting feature of the Type II burst is an approximate proportionality of the burst duration to the time to the next burst. The time sequence from a burst to the following quiescent phase can be said to be a time-scale invariant high (burst phase)–low (quiescent phase) transition. The Galactic superluminal source, GRS 1915+105 exhibits a variety of the time variation of the X-ray flux and often repeats transitions between a high-flux level and a low-flux level. In such high–low transitions, Belloni et al. (1997b) found an approximate proportionality between the duration of the low-flux phase and that of the following high-flux phase, over a wide range of the time scale. This low–high transition can again be said to be time-scale invariant. However, an interesting difference between the two time scale invariant transitions is an opposite order of the high and low-flux phase in the time-scale invariant sequence. In the case of the Rapid Burster, the high-flux (burst) phase is the first, while the low-flux phase is the first in the case of GRS1915+105. A limit cycle between an accretion disk in a state of the standard-disk and that in a state of the ADAF (advection dominated accretion flow) is discussed to explain the time-scale invariant high–low (or low–high) transition as well as the difference between the neutron star system and the black-hole system, qualitatively. A phenomenological relation of the accretion disk change with mass ejections from the central part of the disk is also discussed.     

Delayed outburst of H 1743–322 in 2003 and relation with its other outbursts

The Galactic transient black hole candidate H 1743–322 exhibited a long duration outburst in 2003 after more than two and a half decades of inactivity. The 2003 event was extensively studied in multi-wavelength bands by many groups. The striking feature is that the total energy released is extremely high as compared to that in tens of outbursts which followed. In this paper, we look at this event and study both the spectral and temporal properties of the source using two component advective flow (TCAF) paradigm. We extract accretion flow parameters for each observation from spectral properties of the decay phase and determine the mass of the black hole. We computed the energy released during all the known outbursts since 2003 and showed that on an average, the energy release in an outburst is proportional to the duration of the quiescent state just prior to it, with the exception of the 2004 outburst. A constant rate of supply of matter from the companion cannot explain the energy release in 2004 outburst. However, if the energy release of 2003 is incomplete and the leftover is released in 2004, then the companion’s rate of matter supply can be constant since 1977 till date. We believe that erratic behaviour of viscosity at the accumulation radius $X_p$ of matter as well as location the $X_p$ itself, rather than the random variation of mass transfer rate from the companion, could be responsible for non-uniformity in outburst pattern. We discuss several factors on which the waiting time and duration of the next outburst could depend.     

非结构网格在积冰数值模拟中的应用

基于非结构网格对翼型表面的积冰进行了数值模拟研究.通过求解气体欧拉方程得到翼型的绕流流场,使用穿透型壁面边界模拟水滴对翼型表面的撞击,采用迭代法对水滴控制方程进行数值求解,得到翼型表面的水滴收集特性;采用不同的积冰冻结模型模拟霜冰和明冰的冻结过程;利用冰层时间推进法模拟积冰过程,基于积冰法向生长假设生成积冰外形.对NA...     

直升机旋翼积冰的数值模拟

为研究直升机旋翼桨叶积冰问题,通过对积冰形成机理和直升机飞行原理的分析,建立了基于CFD(Computational Fluid Dynamics)技术的直升机旋翼桨叶结冰预测的理论模型;采用欧拉法求解水滴控制方程,在经典Messinger模型的基础上提出了积冰表面质能平衡的改进模型;以UH-60型直升机和CH-47型直升机为样机,具体分析了积冰条件下直升机桨叶冰形预测的方法,为进一步研究直升机结冰后的飞行动力学问题及防除冰系统的设计奠定了基础,对提高直升机飞行安全性具有积极意义.     

飞机三维结冰模型及其数值求解方法

 对飞机结冰外形进行纯三维数值模拟,是目前飞机结冰预测中的一大难点。为了建立三维结冰数值模拟方法,基于Messinger的二维结冰模型,提出了一种考虑液态水溢流效应的三维结冰计算模型,并针对该模型建立了表面单元内溢流水流动的分配方案、发展了相应的迭代求解方法。采用本文方法对MS-317后掠翼结冰进行了计算,并与实验和Lewice3D的计算结果进行了对比。研究结果显示：本文方法具有较好的收敛性,计算的霜冰和明冰外形均与Lewice3D计算的冰形一致;对于霜冰和结冰时间较短的明冰,本文计算的冰形与实验吻合较好;对于结冰时间较长的明冰,本文计算的冰形与实验对比还有一定差异,但冰生长的总体趋势和大致体积与实验一致。同时,对比了MS-317无后掠翼与有后掠翼结明冰的外形,发现机翼后掠导致的三维溢流效应对结冰外形有明显影响,因此,对于三维结冰分析,如果用二维截面的结果来代替三维结果,其合理性还需验证。     

锥角对旋转整流罩积冰影响的模拟实验

采用缩比模型对4种不同锥角的旋转整流罩进行了冰风洞积冰模拟实验.推导出旋转表面积冰相似参数,并根据重要参数的匹配确定缩比整流罩模型的积冰实验参数.在实验中采用高速摄像系统记录冰生长过程及最终冰形.结果表明:4种锥角的整流罩表面积冰均由初期生成、分布连续的明冰和后期增长迅速的白色霜冰构成;锥角小于等于74°的整流罩表面霜冰为针状或粒状,积冰厚度较小;锥角大于80°的整流罩表面霜冰为羽毛状,积冰厚度较大,并伴随冰脱落现象,锥角较大的整流罩冰脱落位置向下游移动.