Identifying the Spatial Structure of Black Hole and Tropical Cyclone Based on a Theoretical Analysis of Orthogonal Interaction

Black holes are recognized by Newton’s gravitational theory and Einstein’s general relativity, but there is still a lack of understanding the spatial structure of events, especially the nature of event horizon. In this paper, a theoretical analysis is used to compare the structures of tropical cyclone in the atmosphere and black hole in the astronomy so that five results are: 1) Both of them share the similar spatial structure, with tropical cyclone and black hole having the outflow cloud shield and the horizon sphere in the central part, respectively, while four spiral material bands exist in the rotating plane around them;2) In theoretically, the energy density formed by the orthogonal interaction of the four spiral material bands is as times as the total kinetic energy of the head-on interaction;3) This region of high energy density can lead to the conversion from mass to energy and the creation of new physical states of matter, which is a black hole event;4) The outer horizon of a black hole is the outermost interface of events, or the orthogonal interaction interface of particles;5) High-speed plasma jets extended at the poles of the black hole are directly associated with the shear stress of orthogonal interaction.

Suppressing longitudinal spatial hole burning with dual assisted phase shifts in pitch-modulated DFB lasers

An equivalent corrugation pitch-modulated （ECPM） distributed feedback （DFB） semiconductor laser with two equivalently assisted phase shifts （EAPS） was theoretically studied and experimentally demonstrated. The simulated results showed that the longitudinal photon density distribution of the ECPM ＋ EAPS DFB lasers was much more uniform than that of a sole ECPM DFB laser without EAPS, and the longitudinal spatial hole burning was therefore suppressed more effectively. The results of experiment showed that good single longitudinal mode operation was achieved, with side mode suppression ratio （SMSR） being over 35 dB, and the wavelength range was from 1,559.64 to 1,563.02 nm when the operation current was from 50 to 160 mA at the temperature of 25 ℃, and the SMSR increased to 46.29 dB when the injection current was 130 mA.

Modeling the Interior of Black Holes Utilizing a 4-D Spatial Blackbody Radiation Model with an Exponential Distribution

This is a second follow up paper on a model, which treats the black hole as a 4-D spatial ball filled with blackbody radiation. For the interior radiative mass distribution, we employ a new type of truncated probability distribution function, the exponential distribution. We find that this distribution comes closest to reproducing a singularity at the center, and yet it is finite at 4-D radius, . This distribution will give a constant gravitational acceleration for a test particle throughout the black hole, irrespective of radius. The 4-D gravitational acceleration is given by the expression, , where R is the radius of the black hole, MR is its mass, and is the exponential shape parameter, which depends only on the mass, or radius, of the black hole. We calculate the gravitational force, and the entropy within the black hole interior, as well as on its surface, identified as the event horizon, which separates 3-D from 4-D space. Similar to a truncated Gaussian distribution, the gravitational force increases discontinuously, and dramatically, upon entry into the 4-D black hole from the 3-D side. It is also radius dependent within the 4-D black hole. Moreover, the total entropy is shown to be much less than the Bekenstein result, similar to the truncated Gaussian. For the gravitational force, we obtain, , where Mr is the radiative mass enclosed within a 4-D volume of radius r. This unusual force law indicates that the gravitational force acting upon a layer of blackbody photons at radius r is strictly proportional to the enclosed radiative energy, MrC2, contained within that radius, with 0.1λ being the constant of proportionality. For the entropy at radius, r, and on the surface, we obtain an expression which is order of magnitude comparable to the truncated Normal distribution. Tables are presented for three black holes, one having a mass equal to that of the sun. The other two have masses, which are ten times that of the sun, and 106 solar masses. The corresponding parameters are found to equal, , respectively. We compare these results to the truncated Gaussian distribution, which were worked out in another paper.

On the Internal Structure of a Black Hole Utilizing a 4-D Spatial Blackbody Radiation Model

A black hole is treated as a self-contained, steady state, spherically symmetric, 4-dimensional spatial ball filled with blackbody radiation, which is embedded in 3-D space. To model the interior distribution of radiation, we invoke two stellar-like equations, generalized to 4-D space, and a probability distribution function (pdf) for the actual radiative mass distribution within its interior. For our purposes, we choose a truncated Gaussian distribution, although other pdf’s with support, r ∈[0, R], are possible. The variable, r = r(4), refers to the 4-D radius within the black hole. To fix the coefficients, (μ,σ), associated with this distribution, we choose the mode to equal zero, which will give maximum energy density at the center of the black hole. This fixes the parameter, μ = 0. Our black hole does not have a singularity at the center, and, moreover, it is well-behaved within its volume. The rip or tear in the space-time continuum occurs at the event horizon, as shown in a previous work, because it is there that we transition from 3-D space to 4-D space. For the shape parameter, σ , we make use of the temperature just inside the event horizon, which is determined by the mass, or radius, of the black hole. The amount of radiative heat inflow depends on mass, or radius, and temperature, T2 ≥ 2.275K , where, T2, is the temperature just outside the event horizon. Among the interesting consequences of this model is that the entropy, S(4), can be calculated as an extrinsic, versus intrinsic, variable, albeit in 4-D space. It is found that S(4) is much less than the comparable Bekenstein result. It also scales not as, R2 , where R is the radius of the black hole. Rather, it is given by an expression involving the lower incomplete gamma function, γ(s,x), and interestingly, scales with a more complicated function of radius. Thus, within our framework, the black hole is a highly-ordered state, in sharp contrast to current consensus. Moreover, the model-dependent gravitational “constant” in 4-D space, Gr(4), can be determined, and this will depend on radius. For the specific pdf chosen, Gr(4)Mr = 0.1c2(r4/σ2), where Mr is the enclosed radiative mass of the black hole, up to, and including, radius r. At the event horizon, where, r = R, this reduces to GR(4) = 0.2GR3/σ2, due to the Schwarzschild relation between mass and radius. The quantity, G, is Newton’s constant. There is a sharp discontinuity in gravitational strength at the 3-D/4-D interface, identified as the event horizon, which we show. The 3-D and 4-D gravitational potentials, however, can be made to match at the interface. This lines up with previous work done by the author where a discontinuity between 3-D and 4-D quantities is required in order to properly define a positive-definite radiative surface tension at the event horizon. We generalize Gauss’ law in 4-D space as this will enable us to find the strength of gravity at any radius within the spherically symmetric, 4-D black hole. For the pdf chosen, gr(4) = Gr(4)Mr/r3 = 0.1c2r/σ2, a remarkably simple and elegant result. Finally, we show that the work required to assemble the black hole against radiative pressure, which pushes out, is equal to, 0.1MRc2. This factor of 0.1 is specific to 4-D space.

Are Black Holes 4-D Spatial Balls Filled with Black Body Radiation? Generalization of the Stefan-Boltzmann Law and Young-Laplace Relation for Spatial Radiative Transfers

This is the first paper in a two part series on black holes. In this work, we concern ourselves with the event horizon. A second follow-up paper will deal with its internal structure. We hypothesize that black holes are 4-dimensional spatial, steady state, self-contained spheres filled with black-body radiation. As such, the event horizon marks the boundary between two adjacent spaces, 4-D and 3-D, and there, we consider the radiative transfers involving black- body photons. We generalize the Stefan-Boltzmann law assuming that photons can transition between different dimensional spaces, and we can show how for a 3-D/4-D interface, one can only have zero, or net positive, transfer of radiative energy into the black hole. We find that we can predict the temperature just inside the event horizon, on the 4-D side, given the mass, or radius, of the black hole. For an isolated black hole with no radiative heat inflow, we will assume that the temperature, on the outside, is the CMB temperature, T2 = 2.725 K. We take into account the full complement of radiative energy, which for a black body will consist of internal energy density, radiative pressure, and entropy density. It is specifically the entropy density which is responsible for the heat flowing in. We also generalize the Young- Laplace equation for a 4-D/3-D interface. We derive an expression for the surface tension, and prove that it is necessarily positive, and finite, for a 4-D/3-D membrane. This is important as it will lead to an inherently positively curved object, which a black hole is. With this surface tension, we can determine the work needed to expand the black hole. We give two formulations, one involving the surface tension directly, and the other involving the coefficient of surface tension. Because two surfaces are expanding, the 4-D and the 3-D surfaces, there are two radiative contributions to the work done, one positive, which assists expansion. The other is negative, which will resist an increase in volume. The 4-D side promotes expansion whereas the 3-D side hinders it. At the surface itself, we also have gravity, which is the major contribution to the finite surface tension in almost all situations, which we calculate in the second paper. The surface tension depends not only on the size, or mass, of the black hole, but also on the outside surface temperature, quantities which are accessible observationally. Outside surface temperature will also determine inflow. Finally, we develop a “waterfall model” for a black hole, based on what happens at the event horizon. There we find a sharp discontinuity in temperature upon entering the event horizon, from the 3-D side. This is due to the increased surface area in 4-D space, AR(4) = 2π2R3, versus the 3-D surface area, AR(3) = 4πR2. This leads to much reduced radiative pressures, internal energy densities, and total energy densities just inside the event horizon. All quantities are explicitly calculated in terms of the outside surface temperature, and size of a black hole. Any net radiative heat inflow into the black hole, if it is non-zero, is restricted by the condition that, 0cdQ/dt FR(3), where, FR(3), is the 3-D radiative force applied to the event horizon, pushing it in. We argue throughout this paper that a 3-D/3-D interface would not have the same desirable characteristics as a 4-D/3-D interface. This includes allowing for only zero or net positive heat inflow into the black hole, an inherently positive finite radiative surface tension, much reduced temperatures just inside the event horizon, and limits on inflow.

Characteristic analysis of 1.06μm long-cavity diode lasers based on asymmetric waveguide structures

In long-cavity edge-emitting diode lasers,longitudinal spatial hole burning(LSHB),two-photon ab⁃sorption(TPA)and free carrier absorption(FCA)are among the key factors that affect the linear increase in out⁃put power at high injection currents.In this paper,a simplified numerical analysis model is proposed for 1.06μm long-cavity diode lasers by combining TPA and FCA losses with one-dimensional(1D)rate equations.The ef⁃fects of LSHB,TPA and FCA on the output characteristics are systematically analyzed,and it is proposed that ad⁃justing the front facet reflectivity and the position of the quantum well(QW)in the waveguide layer can improve the front facet output power.

红翅拟柄天牛在红果树上的空间危害特征

为明确红翅拟柄天牛Cataphrodisium rubripenne(Hope)对红果树Stranvaesia davidiana的危害特性,调查该天牛的排粪孔、羽化孔、蛹室和蛀道在红果树上的空间分布特征。结果表明:在云南省富源县,红翅拟柄天牛排粪孔主要分布在高度150 cm以下树干和直径5~10 cm枝干,在树干阴面的数量显著高于阳面;羽化孔集中分布于高度150 cm以下树干和直径15 cm以下枝干,且枝干阳面羽化孔数显著多于阴面。排粪孔和羽化孔数量随树干高度增加而减少,与树干高度显著负相关。蛹室位于羽化孔上方,距离羽化孔的距离为(18.89±5.04)cm。蛀道主要集中在高度0~150 cm树干和直径5~10 cm的枝干,蛀道数量和大小与树干高度显著负相关,与枝干直径显著正相关。研究结果可为红翅拟柄天牛的精准林间防治提供理论参考依据。

基于解析法的空间角向孔镗削工艺尺寸转换研究

空间角向孔作为行星轮系旋转作动器中的重要结构特征具有很高的加工精度。镗削时必须根据图纸设计尺寸得到准确的镗削工艺尺寸,以便准确定位。文章系统地对双角度、三角度空间角向孔镗削过程、工艺尺寸转换进行了研究,使用图解法、解析法推导出对应的计算公式,拓展了工艺尺寸转换方法。利用解析法得到的计算公式,实现利用空间角向孔与工艺钢球相对尺寸及空间角向孔角度尺寸,得到所需的镗削工艺尺寸,降低了工艺尺寸转换难度,提高了空间角向孔的镗削效率。同时结合Python编程语言,编写出一套工艺尺寸计算软件,验证了推导公式的有效性和准确性。

汽车桥壳通气孔空间位置尺寸检具设计与应用

汽车桥壳通气孔空间位置尺寸使用标准量具或普通测量方法无法直接完成测量,而常规的检测方法其检测过程十分繁琐、复杂,检测时间长,需由专人进行检测,不适用于批量生产零部件的检测。通过对桥壳结构和通气孔位置尺寸特点分析,设计并制造了通气孔位置尺寸检测检具,并成功应用于桥壳通气孔位置尺寸检测,其检测过程简单快捷、检测精度满足实际生产要求、检测效率得到显著提高。

黑洞错觉验证研究方法进展

黑洞错觉导致的航空事故频发,但对于此问题的内在机制和因果关系并没有合理一致的解释,仍需深入探索。本研究在概述黑洞错觉现象的基础上,梳理了国外对于黑洞错觉早期的各种机制假说以及验证评估过程,阐述了一种最新的机制假说——线偏差错觉,及其验证研究方法,并总结了黑洞错觉的识别预防策略,为后续开展研究奠定基础。

船用柴油机机体孔系平行度在机检测方法

船用柴油机机体孔系平行度的高精度在机检测是制约其制造过程智能化水平的瓶颈技术之一。为此,基于多传感器技术,提出一种空间孔系平行度在机检测方法。在传感器不放入孔内的情况下,仅将测头伸入孔内进行测量,由多个位移传感器的测量值,根据对应传感器所处的位置,计算获得孔系平行度大小。结果表明,该检测方法可有效对空间孔系平行度进行检测,为孔系零件高效在机检测提供了理论基础。

基于自适应补缺滤波的装配孔孔位提取方法

针对阵列天线自动化装配过程中由于子板表面易反光等原因导致的装配孔孔位提取难、提取精度低等问题,提出了一种基于自适应补缺滤波的装配孔孔位提取方法。利用双目视觉相机采集被测表面三维点云,采用离群点滤波去除装配孔边缘离群点,通过自适应补缺滤波,对位于装配孔外部的缺失点云进行自适应补缺。在自适应补缺滤波算法中,根据点云特征和给定孔径自适应构造判断区域,保证算法的可靠性与适用性。根据每个点k领域点的法矢偏差完成点云边界点的提取,并借助随机采样一致性(RANSAC)算法优化空间圆的拟合过程,提高装配孔孔位提取的可靠性和精度。通过试验对所提算法进行验证,试验结果装配孔孔位提取精度可达0.037 mm。

五轴电火花机床加工空间斜孔的电极定位参数研究

空间斜孔的加工实质上是电火花机床电极沿孔的轴线的运动。对于由3个坐标轴旋转变换得到的空间斜孔,可通过五轴电火花机床沿3个坐标轴方向上的平移运动和绕两个坐标轴方向的旋转运动,使机床电极轴线与空间斜孔轴线重合,为此需要求解加工空间斜孔的电极定位参数。分析了通过坐标系旋转平移变换得到空间斜孔轴线的过程。根据空间斜孔的空间角度和几何参数求解空间斜孔轴线矢量的坐标变换矩阵,以建立空间斜孔轴线的矢量模型。得到了五轴数控电火花机床加工空间斜孔的电极摆角和电极定位坐标,使电极轴线与空间斜孔轴线重合。并制作了根据空间斜孔几何参数自动求解数控电火花机床的电极摆角和电极坐标的计算软件。

基于三轴机床的复合材料空间法向小孔加工方法

为了解决金属-复合材料双层结构的小孔高精度加工问题,针对某航天型号防热部段传感器孔,提出一种基于三轴机床的复合材料空间法向小孔数控加工方法。此类法向小孔的精密加工通过“两步法”实现:首先使用芯轴将该法向内层金属上已钻孔到位的小孔从壳体内层精确引出至外层无干涉区域,然后利用三轴机床+二轴手动转台精确找正加工基准后加工复合材料小孔。结果表明,该方法提高了传感器孔的加工精度,改善了加工效率,降低了生产成本,其加工原理已成功应用于其他法向特征孔的加工工艺中,对空间法向小孔的三轴加工工艺具有指导性意义。

基于深度回归的骨折锁钉孔三维空间定位方法

人体长骨发生骨折后,需要将髓内钉插入髓腔之中以固定骨折区域,之后将螺钉置入髓内钉远端孔中以固定髓内钉,该手术难点在于远端孔位姿会随髓腔形状发生变化,因此传统徒手锁钉方法难以准确定位远端孔的空间位姿。为解决此问题,提出一种基于单张术中X线片精准定位髓内钉远端孔的方法。首先通过对比虚拟髓内钉与真实术中髓内钉的轮廓相似性确定远端孔的初始位姿;之后利用位姿修正算法对齐髓内钉轮廓特征,驱动虚拟髓内钉位姿迭代优化;最后确定远端孔的精确位姿。此外,为了准确提取X线片中的轮廓特征,结合目标检测算法,提出一种由粗到精的两阶段髓内钉轮廓提取方法。分别在模拟环境与真实临床环境中进行实验,将本方法计算得到的远端孔轴线与真实远端孔轴线进行比较,模拟环境中2个轴线的距离、角度误差为0.42 mm、0.46°,临床环境中2个轴线的距离、角度误差为0.75 mm、0.81°。本方法能满足髓内钉手术中远端孔定位的实际需求,有效提高髓内钉远端锁钉术中定位与规划效率。

Bardeen-AdS黑洞的热力学混沌及暗能量效应

利用Melnikov方法研究了Bardeen-Anti de Sitter(AdS)黑洞对周期性微扰的热力学响应以及混沌的发生与演化,探讨了Quintessence暗能量对黑洞的影响.根据规范/引力对偶与扩展相空间的思想,将黑洞看作一个可压缩、具有微小黏性、各向同性的液体系统.首先对Bardeen-AdS黑洞的相变旋节区施加时间周期性微扰,当微扰的临界振幅γ大于临界振幅γ_(c)时,黑洞会产生热力学混沌现象,该临界值由非线性电磁场(具体体现为磁单极荷β)和初始温度T_(0)共同决定.然后对黑洞施加空间周期性微扰时,任意大小的微扰振幅均会导致黑洞相空间中出现混沌现象.考虑Kiselev的各向同性唯象模型,我们发现Quintessence暗能量对其内包裹黑洞的影响类似于一种热力学意义下的增益/阻尼机制.

F-P腔掺Yb^(3+)双包层光纤激光器中的模式竞争

对连续波LD泵浦掺Yb3 +双包层光纤激光器的模式竞争进行了实验研究 .发现由二色镜和光纤端面构成的F P谐振腔中存在激烈的模式竞争 ,对光纤激光器发射波长和输出功率的稳定性都产生不利影响 .通过消除“空间烧孔”或减小光纤激光器的有效增益带宽 ,能够有效抑制模式竞争 。

线结构光视觉传感器测圆(类圆)孔中心两步法

针对基于工业机器人平台柔性三维视觉检测系统,提出线结构光视觉传感器测量空间圆(类圆)孔中心两步法。根据线结构光视觉传感器测量模型,确定被测圆心近似z向坐标。根据圆心相对摄像机光心的方位,确定被测圆心的x、y向坐标。该方法突破了传统空间圆(类圆)孔中心测量仅能采用双目视觉传感器的方式。研究结果表明,该方法切实可行,可以满足实际测量需求,能够极大地扩展线结构光视觉传感器的应用范围。

高功率793 nm半导体激光器

针对掺铥光纤激光器泵浦源的需求,研制了波长为793 nm的高功率半导体激光芯片和尾纤耦合模块。激光器外延采用了非对称大光腔的波导结构,降低了模式损耗,波导采用无铝的GaInP材料,结合真空解理钝化工艺提高了腔面损伤阈值。通过外延结构和腔面镀膜的优化,研制的激光器单管输出功率达到12 W@11A,在输出功率8W时通过了300 h老化测试。采用7只单管制备了尾纤耦合模块,耦合至100μm NA.0.22光纤中,输出功率为40W@7A,电-光效率为49.5%@40 W。

理论研究电流注入对垂直腔面发射激光器多横模行为的影响

从包含时空变量的速率方程出发,针对弱折射率导引垂直腔面发射激光器(VCSELs),利用空间积分法分析了典型电注入参数对VCSELs多横模行为的影响,在不降低模型准确性的前提下提高了仿真效率。仿真结果表明,注入盘孔径和注入环越小、注入强度越低以及电流扩散越弱时,VCSELs更易实现单横模工作;反之,VCSELs高阶横模开始出现并呈现较强的模式竞争,引发了载流子空间烧孔效应,并导致基模强度降低。进一步得出,在环形注入方式下,高阶模式更容易出现且彼此间的竞争较盘形注入时强。