Chromothermal oscillations and collapse of strange stars to black holes: astrophysical implications

We study the effects of temperature on strange stars. It is found that the maximum mass of the star decreases with the increase of temperature, as at high temperatures the equations of state become softer. Moreover, if the temperature of a strange star increases, keeping its baryon number fixed, its gravitational mass increases and its radius decreases. This leads to a limiting temperature, where it turns into a black hole. These features are the result of a combined effect of the change of gluon mass and the quark distribution with temperature. We report on a new type of radial oscillation of strange stars, driven by what we call 'chromothermal' instability. We also discuss the relevance of our findings in the astrophysics of core collapse supernovae and gamma-ray bursts.     

Dissipative accretion flows around a rotating black hole

We study the dynamical structure of a cooling dominated rotating accretion flow around a spinning black hole. We show that non-linear phenomena such as shock waves can be studied in terms of only three flow parameters, namely the specific energy     , the specific angular momentum (λ) and the accretion rate     of the flow. We present all possible accretion solutions. We find that a significant region of the parameter space in the     plane allows global accretion shock solutions. The effective area of the parameter space for which the Rankine–Hugoniot shocks are possible is maximum when the flow is dissipation-free. It decreases with the increase of cooling effects and finally disappears when the cooling is high enough. We show that shock forms further away when the black hole is rotating compared to the solution around a Schwarzschild black hole with identical flow parameters at a large distance. However, in a normalized sense, the flow parameters for which the shocks form around the rotating black holes are produced shocks closer to the black hole. The location of the shock is also dictated by the cooling efficiency in that higher the accretion rate     , the closer is the shock location. We believe that some of the high-frequency quasi-periodic oscillations may be due to the flows with higher accretion rate around the rotating black holes.     

Comparison of Meteoroid Flux Models for Near Earth Space

Over the last decade several new models for the sporadic interplanetary meteoroid flux have been developed. These include the Divine-Staubach and the Dikarev model. They typically cover mass ranges from 10⁻¹⁸ g to 1 g and are applicable for model specific Sun distance ranges between 0.1 AU and 20 AU Near 1 AU averaged fluxes (over direction and velocities) for all these models are tuned to the well established interplanetary model by Grün et al. However, in many respects these models differ considerably. Examples are the velocity and directional distributions and the assumed meteoroid sources. In this paper flux predictions by the various models to Earth orbiting spacecraft are compared. Main differences are presented and analysed. The persisting differences even for near Earth space can be seen as surprising in view of the numerous ground based (optical and radar) and in situ (captured Inter Stellar Dust Particles, in situ detectors and analysis of retrieved hardware) measurements and simulations.     

Calculation of the Intensity Ratio and Intrinsic Redshift Ratio of the Cerenkov Iron Kα and Kβ Lines and Its Possible Application in the Study of AGNs

We have pointed out that, when thermal relativistic electrons with an isotropic velocity distribution move through a region of dense gas or impinge upon its surface, the Cerenkov effect will produce a particular kind of atomic or ionic emission line, which we have called the “Cerenkov line-like radiation”. This prediction for the optical wavebands has been verified by laboratory experiments. In this paper, we extend this line-like radiation theory to the X-ray waveband and give the basic formulae for calculating the intensity ratio and intrinsic redshift ratio of the Cerenkov iron K_α and K_β lines, for different ionization orders of iron. Potential application of this calculated result may be found in the study of AGNs. The recent observations of NGC3783 show that besides the iron K_α line at ∼6.4 keV, there is also a very strong iron Kβ line at ∼7.0 keV, and that the ratio of equivalent widths between the two is anomalous: EWK_α/EWK_β ≈ 3.43. It is difficult to explain this by the conventional mechanism of “photoelectric absorption-fluorescence emission”. We suggest that the mechanism of Cerenkov line-like radiation can provides a way of solving this puzzle. Besides, we expect that the calculated intrinsic redshift ratio of Cerenkov iron K_α and K_β lines could be tested in future observations. If our suggestion is further supported by observations, then our view on the physical environment around the central massive black hole of an AGN will be greatly modified: the activity becomes more energetic and violent, and the gas, much denser than previously thought.     

冰川区不同气温估算方法评估 ——以藏东南帕隆4号冰川为例

冰川作为地表特殊的下垫面,冰川区内气温明显低于同高度非冰川区大气温度。如何利用低海拔非冰川区观测资料精确估算高海拔冰川区气温,直接关系着青藏高原冰川消融估算及其水文效应的评估。利用架设在藏东南帕隆藏布4号冰川不同高度带的四台自动气象站资料,分析了冰川区与非冰川区气温的波动特征,评估了迄今为止通用的线性递推模型（DT模型）、分段拟合模型（SM模型）和简化热力学模型（GB模型）三种方法在藏东南冰川区气温估算方面的应用效果。对比研究发现：SM模型在帕隆4号冰川上的模拟效果最为理想且操作相对简单;传统DT模型在消融区存在严重的高估,帕隆4号冰川表面夏季（6-8月）正积温的高估比例接近39%;GB模型由于受到诸如冰川风边界层厚度等不确定性的影响,降低了大范围温度估算的可操作性。     

基于MODIS数据的北疆积雪黑碳和雪粒径反演及时空变化分析

积雪是地球上反射率较高的自然表面,对于中高纬度地区的水文和能量收支平衡发挥着重要作用。表层积雪中的黑碳和雪粒径变化可以显著影响积雪反照率,造成积雪对太阳辐射吸收的变化,进而对区域气候变化和水文循环产生反馈作用。利用遥感技术对季节性积雪表层黑碳和雪粒径进行定量评估,可以获取时空上连续系统的雪表黑碳浓度和雪粒径变化情况,这也是许多气候和水文模型的输入因子。以中国主要季节性积雪区北疆为研究区,基于MODIS（Moderate Resolution Imaging Spectroradiometer）数据的3（0.47 μm）、2（0.86 μm）和5（1.24 μm）波段,采用SGSP（Snow Grain Size and Pollution Amount）算法反演2000-2018年积雪期的雪表黑碳浓度和雪粒径,并结合地面观测数据对于反演结果进行了精度验证,综合分析北疆雪表黑碳浓度和雪粒径时空变化趋势。结果显示,SGSP算法能够同时反演雪表黑碳浓度和雪粒径,并且验证结果表明纯雪像元上反演结果具有较好的精度;2000-2018年北疆雪表年均黑碳浓度和年均雪粒径都随时间变化呈现微弱下降趋势;受地理位置和局部污染源的影响,北疆积雪黑碳浓度空间分布复杂,天山北坡经济带平均黑碳浓度最高,伊犁地区平均黑碳浓度最低,雪粒径的空间分布显示塔城地区平均雪粒径最大,伊犁地区最小。     

红层软岩压缩破坏的分形特征与级联失效过程

基于不同围压条件下的红砂岩三轴压缩试验结果,采用数字图像相关技术对岩样外表面破坏形态进行全程观测,获得不同阶段岩样外表面破坏图像,分别对岩样破坏后阶段的图像进行分析。通过分形盒维数表征岩样外表面裂纹的变化情况,发现岩样破坏越严重,裂纹分形维数越高,且在最后破坏阶段裂纹分形维数出现突变,揭示岩样的破坏特征。引入级联失效数学模型,结合红层软岩内部的矿物成分与细观结构分布特点,概化出其结构的随机连接模型与破坏方式,分析红层软岩加载作用下的内部节点颗粒“容量-荷载”重分配原则以及节点颗粒失效后其初始荷载传递路径。结果表明,红层软岩在受载时为一个级联失效的分阶段破坏过程,级联因子通过级联路径不断传播、增多,级联失效越发明显,同时结合岩石破坏的变形损伤过程与其轴向应力-应变曲线分段特征,揭示该类岩石破坏的级联失效分级标准,为拓展该领域的研究具备一定的参考价值。