共查询到19条相似文献,搜索用时 78 毫秒
1.
沈有根 《中国科学院上海天文台年刊》1999,56(20):131-135
在2维弦论黑洞背景时空中求解了具有't Hooft的边界条件和“准周期”边界条件的Klein-Gor-don方程和Dirac方程,分别计算了相应的玻色子熵和费米子熵,发现它们具有同一发散形式,两仅相差一个系数。 相似文献
2.
本利用李立新和刘辽导出的黑洞视界附近的辐射态方程,计算了约束在一个球形盒子中的自引力辐射体系的熵(不含中心黑洞和含有中心黑洞两种情况)。与Sorkin等人的计算比较,本的结果不会出现发散困难,而且体系的总熵(包括中心黑洞的熵)的上限正好等于坍缩后形成的同质量的黑洞熵。作认为,自引力辐射体系坍缩的合理模式是先形成中心黑洞,然后中心黑洞逐渐长大直至整个体系全部坍缩为黑洞。在坍缩过程中,任一中间态 相似文献
3.
运用在brick-wall方法的基础上发展起来的薄膜模型计算了六维动态黑洞的自由能和玻色子熵,然后应用Г矩阵方法计算了费米子熵.结果显示六维动态黑洞的玻色子熵和费米子熵有相同的形式,它们之间只相差一个系数.并且仍然满足Bekenstein-Hawking的熵与面积的关系. 相似文献
4.
汪定雄 《中国天文和天体物理学报》1991,(1)
在黑洞蒸发的最后阶段其残余质量为Planck质量的量级,因而所对应的黑洞熵为2πk_B量级,在Bekenstein工作的基础上作者导出在吸积物质的过程中黑洞的最小熵增为2πk_B,这一最小熵增又限制能参与吸积物质的黑洞的质量下限为Planck质量的量级,因而所对应的最小黑洞熵也为2πk_B这一量级。作者进一步指出:黑洞的最小熵及最小熵增不受引力常数G变化的影响,因此上述结论在极早期宇宙中也能成立,在上述分析的基础上作者提出一个猜想:黑洞熵可以量子化,其量子单位为2πk_B。 相似文献
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6.
运用在砖墙模型方法的基础上发展起来的薄膜模型计算了 1 1维和 2 1维动态时空中的黑洞的熵。结果表明在低维动态时空中 ,黑洞熵仍满足Bekenstein -Hawking熵与面积的关系 相似文献
7.
运用在砖墙模型方法的基础上发展起来的薄膜模型计算了1 1维和2 1维动态时空中的黑洞的熵。结果表明在低维动态时空中,黑洞熵仍满足Bekenstein—Hawking熵与面积的关系。 相似文献
8.
我们已经研究了分别具椭圆和双曲不动点的二维保测度映射及其受摄三维扩张的KS熵。本文研究一类具抛物不动点的二维保测度映射:及其受摄扩张:的KS熵随参数A、B、C、D、E的变化.数值探索结果表明:适当定义区域内的二维映射T2的KS熵与A无关,与我们的理论分析结果相一致。受摄扩张映射T3的KS熵随摄动参数B、C、D的增大而增大,却随E的增大而减小.我们还发现,随着摄动的逐渐增强,映射T3的不变环面将逐渐破裂,使更多的轨道逃逸,从而可能使映射T3的KS熵减小。另外,不变环面存在的判别式在大范围内仍在一定程度上有效。 相似文献
9.
采用在brick模型基础上发展起来的membrane模型,计算了缘于任意自旋场的非静态黑洞——Vaidya黑洞的自由能和熵。结果表明,玻色子场(自旋s=1,2)和费米子场(自旋s=1/2)的熵都恰好与黑洞的视界面积成正比,这与静态和稳态的情况相同。而且,玻色子和费米子场的熵具有相同的形式,二相差一个系数。 相似文献
10.
已有观测证据表明宇宙大尺度结构是自相似或自仿射的分形分布,并已求出表片这两类分形的结构分数维。多分形热力学中提出的Kohmoto熵函数建立了多重分形和热力学的形式类式。本文在三维球对称坐标系中求取了无标度区间r0≤r≤R范围内宇宙大尺度自相似分形分布的一阶Kohmoto熵函数,它对应于信息论中的信息熵。 相似文献
11.
IWAN P. WILLIAMS G. O. RYABOVA A. P. BATURIN A. M. CHERNITSOV 《Earth, Moon, and Planets》2004,95(1-4):11-18
The orbit of asteroid 2003 EH1 is very similar to the mean orbit of the Quadrantid meteoroid stream so that a close relationship
between the two is very likely. It has already been suggested that Comet C/1490 Y1 could be the parent of the Quadrantids.
If this is the case, then some relationship between the comet and the asteroid might be expected. The orbit of C/1490 Y1 is
based on a short observing arc of about 6 weeks and all the observations were with the naked eye, so that its elements are
very poorly determined. Hence, forward integration to determine whether asteroid 2003 EH1 represents the re-discovery of the
dormant nucleus of C/1490 Y1 is not feasible. Instead we choose to integrate back in time the orbit of 2003 EH1, which is
far better determined, and a family of 3500 clones, all of which are moving on an orbit that is consistent with the present
known orbit of 2003EH1. We compare the results primarily with the recorded observations of the comet rather than the orbit
of the comet derived by Hasegawa. We find that one clone is consistent with these observations. 相似文献
12.
The C1XS X-ray Spectrometer on Chandrayaan-1 总被引:1,自引:0,他引:1
M. Grande B.J. Maddison B.J. Kellett J. Huovelin C.L. Duston M. Anand A. Cook B. Foing J.N. Goswami K.H. Joy D. Kochney S. Maurice S. Narendranath D. Rothery A. Shrivastava M. Wilding 《Planetary and Space Science》2009,57(7):717-724
The Chandrayaan-1 X-ray Spectrometer (C1XS) is a compact X-ray spectrometer for the Indian Space Research Organisation (ISRO) Chandrayaan-1 lunar mission. It exploits heritage from the D-CIXS instrument on ESA's SMART-1 mission. As a result of detailed developments to all aspects of the design, its performance as measured in the laboratory greatly surpasses that of D-CIXS. In comparison with SMART-1, Chandrayaan-1 is a science-oriented rather than a technology mission, leading to far more favourable conditions for science measurements. C1XS is designed to measure absolute and relative abundances of major rock-forming elements (principally Mg, Al, Si, Ca and Fe) in the lunar crust with spatial resolution ?25 FWHM km, and to achieve relative elemental abundances of better than 10%. 相似文献
13.
C. Wolf 《Astronomische Nachrichten》1990,311(1):1-4
It is shown that the primordial entropy of the universe can be generated in the residual phase prior to Calabi-Yau splitting and following the passing to the field theory limit of the heterotic super-string in ten space-time dimensions, wherein matter is represented by either a radiative equation of state or the equation of state for stiff matter. 相似文献
14.
为了获得稳定、可靠的卫星电视时间比对数据,成功研制了以秒信号提取器为主要部件的新一代卫星电视时间解调器。介绍了秒脉冲信号提取器的设计原理,详细阐述了钳位电路、采样保持电路和数字延迟电路的设计思路。对采用新的解调器和采用旧的解调器的卫星电视秒信号监测系统所得到的比对数据进行了分析,结果表明新的电视时间解码器的性能得到明显提高。 相似文献
15.
J. A. Núñez P. M. Cincotta F. C. Wachlin 《Celestial Mechanics and Dynamical Astronomy》1996,64(1-2):43-53
In this paper we present an indicator of chaos that takes advantage of the Information Entropy concept. We develop the mathematical formulation and test the results of its application with those obtained by other methods for the 2D Hénon-Heiles system and the 3D Contopoulos, Galgani and Giorgilli potential. 相似文献
16.
Jean Manfroid Damien Hutsemékers Anita L. Cochran William M. Jackson Rita Schulz 《Icarus》2007,187(1):144-155
UVES and HIRES high-resolution spectra of Comet 9P/Tempel 1 are used to investigate the impact and rotational light curves of various species with a view toward building a simple model of the distribution and activity of the sources. The emission by OH, NH, CN, C3, CH, C2, NH2, and OI, are analyzed, as well as the light scattered by the dust. It is found that a simple model reproduces fairly well the impact light curves of all species combining the production of the observed molecules and the expansion of the material throughout the slit. The impact light curves are consistent with velocities of 400-600 m/s. Their modeling requires a three-step dissociation sequence “Grand-Parent → Parent → Daughter” to produce the observed molecules. The rotational light curve for each species is explained in terms of a single model with three sources. The dust component can however not easily be explained that way. 相似文献
17.
Brenda Matthews Edwin Bergin Antonio Crapsi Michiel Hogerheijde Jes Jørgensen Dan Marrone Ramprasand Rao 《Astrophysics and Space Science》2008,313(1-3):65-68
We present our most recent results from an ongoing study of the Class 0 source Barnard 1c in Perseus. This source is of particular
interest because it exhibits evidence of strong alignment of grains all the way to the core’s centre, which is contrary to
all other low-mass protostellar cores observed to date. Our goal is to clarify the source of poor alignment in other sources
by identifying the source of strong alignment in B1c. A central cavity has been identified in N2H+ emission; its anticorrelation with C18O emission suggests that heating in the centre has released CO from grain mantles, in turn destroying N2H+. We present sensitivity-limited, high spatial resolution polarimetry data from the SubMillimeter Array and discuss the potential
implications of these data. 相似文献
18.
云南天文台1m望远镜终端之一的暗天体分光仪和照相机具有4种运行模式:缩焦照相机、无缝多目标光谱仪、有缝光谱仪和星冕仪。这4种运行模式能在几分钟的时间内相互转换,高效快速和灵活方便。该仪器的光学质量优秀,光学系统消像差,特别是消色差。由于光学系统消色差,所成像的低色散光谱在404.6~766.5nm全波段尖锐平直。在多色测光时,各测光波段的像面位置不变,同时兼有大视场的优点,可提高测光精度和测光效率。 相似文献