球形微粒子近场辐射换热研究

从偶极辐射理论出发,结合普朗克黑体辐射分布,推导出近场区热辐射分布。采用MC法模拟了两个纳米球形 村子的辐射换热,考察相天参数对近场辐射换热的影响。表明其辐射热流可比黑体辐射高8个数量级。其热流随间距的增 大急剧减小。小研究对于纳米粒子群的传热研究有积极意义。     

空腔"黑体"辐射的简单模型及推论

建立了一个简单的模型来描绘空腔辐射中腔壁与辐射场的能量交换,由此可以得到空腔辐射平衡场能谱的性质,基尔霍夫定律,以及空腔与黑体的关系．     

空间辐射效应的蒙特-卡罗模拟

 概述了天然宇宙空间的辐射环境,简要地分析了辐射效应机制,在辐射效应的蒙特-卡罗模拟中对靶材料作了无定形假设,入射粒子在靶材料中的弹性能量损失采用经典二体散射公式,非弹性能量损失高能时采用Beth-Bloch公式,低能时采用Lindhard-Scharff公式,中能时采用插值公式,撞出晶格原子引起的次级损伤用Kinchin-Pease模型计算,最后对100KeV硼离子入射于硅材料引起的辐射效应进行了模拟计算,并给出了计算结果和分析。     

微机扫描黑体辐射实验研究

利用微机扫描光栅光谱仪和溴钨灯进行黑体辐射实验研究，验证了黑体辐射的基本规律；论证了黑体辐射实验方法的可行性，分析了黑体的辐射、传递和接收以及正弦机构等器件的性能和误差修正问题．     

诺贝尔物理学奖百年回顾(续)

 （续前期）１９１１年维恩（ＷｉｌｈｅｌｍＣａｒｌＷｅｒｎｅｒＯｔｔｏＦｒｉｔｚＦｒｎａｚＷｉｅｎ１８６４－１９２８）因发现热辐射规律──维恩位移定律,建立黑体辐射的维恩公式,获得了１９１１年度诺贝尔物理学奖．１９世纪末,人们已经认识到热辐射和光辐射都是电磁波,并对辐射能量在不同频率范围内的分布问题,特别是黑体辐射,进行了较深入的理论和实验研究．维恩和拉梅尔（Ｏ．Ｌｕｍｍｅｒ）发明了第一个实用黑体──空腔发射作,为他们的实验研究提供了所需的“完全辐射”。维恩在前人研究的基础上于１８９３年提出了理想黑体辐射的位移定律：λｍａｘＴ＝常数。该定律指出,随着温度（Ｔ）的升高,与辐射能量     

黑体辐射公式的量纲分析

量纲分析是研究物理问题的重要方法之一.本文对量纲分析的解题步骤做了梳理归纳,并对于黑体辐射公式进行了量纲分析.     

矩形介质内辐射换热的有限元法

利用有限单元法离散求解辐射传递方程和能量控制方程.分别计算了边界为黑体和灰体条件下矩形吸收、发射、各向同性散射介质内的平均入射强度和温度分布,并同蒙特卡罗法(M-C法)计算结果进行了比较.     

黑体辐射定律研究及验证

利用微机扫描光栅光谱仪和溴钨灯进行黑体辐射实验研究,分析了黑体的辐射、传递、接收等的误差修正。验证了黑体辐射的基本规律。     

普朗克黑体辐射定律的建立过程

叙述了黑体辐射公式中几个重要结果维恩定律,瑞利-金斯公式和普朗克公式的建立过程,遵循普朗克的思路给出了普朗克公式的量子论解释。     

量子物理的发展

量子物理是从研究黑体光谱中能量分布的统计理论开始的。在一个封闭容器中,与物质处于平衡的辐射能谱通常叫做黑体辐射,因为它与一个完全吸收体发射出来的辐射相同。在1900年解释光谱中能量的分布曾经成为十分活跃的问题。值得指出,这个问题的历史颇为悠久。第一次应用热力学到黑体辐射问题上,要追溯到     

On the interaction of a black-body radiation field with a photoconductor

In this article we consider the problem of how to reconcile the Bose-Einstein statistics of the incident radiation field with the Fermi-Dirac statistics of the electron population in a photoconductor which is in equilibrium with the radiation field. A Langevin approach is followed, based on Einstein's rate equations. Results for the noise sources associated with absorption, stimulated emission, and spontaneous emission, are derived. These results are shown to be consistent with the Fermi-Dirac statistics of the electron processes; also, the various sources are shown to reconstitute the black-body radiation field.     

The 2.7 K black-body radiation background reference frame

This paper reports that the directional temperature is used to present a scheme for deducing the velocity of the reference frame where the black-body which produces the 2.7 K radiation background is at rest.The new renormalized relativistic thermodynamics lays the foundations of the method.     

Spherically symmetric static inhomogeneous cosmological models

Spherically symmetric static cosmological models filled with black-body radiation are considered. The models are isotropic about a central observer but inhomogeneous. It is suggested that the energy density of the free gravitational field, which is coupled to the isotropic radiation energy density, might play an important role in generating sufficient field (vacuum) energy (when converted into thermal energy) and initiate processes like inflation. On the central world line the energy density of the free gravitational field vanishes whereas the proper pressure and density of the isotropic black-body radiation are constants. Further, it is shown that the cosmological constant is no more arbitrary but given in terms of the central pressure and density. Also, at its maximum value the energy density of the free gravitational field is proved to be equal to one third of the combined value of radiation pressure and density.     

Thermal radiation and nonthermal radiation of the slowly changing dynamic Kerr--Newman black hole

Using the related formula of dynamic black hole, we have calculated the instantaneous radiation energy density of the slowly changing dynamic Kerr-Newman black hole. It is found that the instantaneous radiation energy density of a black hole is always proportional to the quartic of the temperature of the event horizon in the same direction. By using the Hamilton-Jacobin equation of scalar particles in the curved spacetime, the spontaneous radiation of the slowly changing dynamic Kerr-Newman black hole is studied. The energy condition for the occurrence of the spontaneous radiation is obtained.     

An exact FRW cosmology with radiation and imperfect fluid

An exact solution of the Einstein field equations for a combination of black-body radiation and an imperfect fluid, in which the geometrical background is a flat FRW metric, is presented. The solution exhibits an axial preferred direction along which the material content moves relative to the radiation field, the latter representing the cosmic background radiation. The solution is shown to be in excellent agreement with current observations.     

Evaluation of neutron radiation field in carbon ion therapy

Carbon ions have significant advantages in tumor therapy because of their physical and biological properties. In view of the radiation protection, the safety of patients is the most important issue in therapy processes.Therefore, the effects of the secondary particles produced by the carbon ions in the tumor therapy should be carefully considered, especially for the neutrons. In the present work, the neutron radiation field induced by carbon ions was evaluated by using the FLUKA code. The simulated results of neutron energy spectra and neutron dose was found to be in good agreement with the experiment data. In addition, energy deposition of carbon ions and neutrons in tissue-like media was studied, it is found that the secondary neutron energy deposition is not expected to exceed 1% of the carbon ion energy deposition in a typical treatment.     

静态球对称黑洞的热质点模型及辐射功率

利用静态球对称黑洞的热质点模型,研究了黑洞的热辐射规律,得到了当η取固有厚度时,对所有Schwarzschild黑洞,其辐射功率都相同,其视界处的辐射能通量与黑洞的质量的平方成反比,而距黑洞遥远的观察者所接收到的辐射能通量与观测者到黑洞的距离的平方成反比; Reissner-Nordstrm黑洞视界处的辐射能通量和辐射功率不仅与黑洞的质量有关,还与黑洞的电荷有关,而距黑洞遥远的观察者所接收到的辐射能通量,当截断的固有厚度η、黑洞的质量m和电荷Q取定后与观测者到黑洞之间的距离的 关键词： 静态球对称黑洞 热质点模型 辐射功率 辐射能通量