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# 澳洲代写|天文学代写Astronomy代写|HPSC20015

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The interaction between elementary particle physics and cosmology has increased greatly since 1980 , to the benefit of both disciplines. Several initial conditions of classical cosmology are given a tentative explanation in “inflationary universe” scenarios, proposed by Alan Guth in 1981 and modified by Linde, Albrecht, and Steinhardt in $1982 .$ These models assume a time when the energy density of a “false vacuum” in a grand unified theory (GUT) dominated the dynamics of the universe. Since the density was essentially constant throughout this period, the RobertsonWalker scale factor grew exponentially in time, allowing an initially tiny causally connected region (even smaller than the small value of $1 / H$ at the start of inflation) to grow until it included all of the space that was to become the currently observable universe. The original version (1981) assumed that this occurred while the universe remained trapped in the false vacuum.

Unfortunately, such a universe that inflated sufficiently never made a smooth transition to a radiation-dominated, early Friedmann cosmology. In the “new inflationary” models (1982), the vacuum energy density dominates while the relevant region of the universe inflates and evolves toward the true vacuum through the spontaneous breaking of the GUT symmetry by nonzero vacuum expectation values of the Higgs scalar. The true vacuum is reached in a rapid and chaotic “phase transition” when the universe is of the order of $10^{-35}$ sec old, resulting in the production of a large number and variety of particles (and antiparticles) at a temperature of the order of $10^{14} \mathrm{GeV}$. It is supposed that the universe evolves according to the standard model after this carly time.

## 澳洲代写|天文学代写Astronomy代写|Constraints from Cosmology

Even as elementary particle theory solves some problems of cosmology, it is subject to limitations derived from cosmological data involving energies far beyond the $2 \times 10^{3} \mathrm{GeV}$ limit of existing terrestrial accelerators. An important example involves the production of magnetic monopoles in the early universe. In 1931, P. A. M. Dirac showed that assuming the existence of magnetic monopoles led to a derivation of the quantization of magnetic and electric charge and a relation between them implying that magnetic charges would have to be very large. However, other properties of the hypothetical monopoles, such as mass and spin, were undetermined in his theory. In 1974, Gerhard t’Hooft and Alexander Polyakov showed that monopoles must be produced in gauge theory as topological defects whenever a semisimple group breaks down to a product that contains a $U(1)$ factor, for example,
$$S U(5) \rightarrow S U(3) \times S U(2) \times U(1)$$

## Matlab代写

MATLAB 是一种用于技术计算的高性能语言。它将计算、可视化和编程集成在一个易于使用的环境中，其中问题和解决方案以熟悉的数学符号表示。典型用途包括：数学和计算算法开发建模、仿真和原型制作数据分析、探索和可视化科学和工程图形应用程序开发，包括图形用户界面构建MATLAB 是一个交互式系统，其基本数据元素是一个不需要维度的数组。这使您可以解决许多技术计算问题，尤其是那些具有矩阵和向量公式的问题，而只需用 C 或 Fortran 等标量非交互式语言编写程序所需的时间的一小部分。MATLAB 名称代表矩阵实验室。MATLAB 最初的编写目的是提供对由 LINPACK 和 EISPACK 项目开发的矩阵软件的轻松访问，这两个项目共同代表了矩阵计算软件的最新技术。MATLAB 经过多年的发展，得到了许多用户的投入。在大学环境中，它是数学、工程和科学入门和高级课程的标准教学工具。在工业领域，MATLAB 是高效研究、开发和分析的首选工具。MATLAB 具有一系列称为工具箱的特定于应用程序的解决方案。对于大多数 MATLAB 用户来说非常重要，工具箱允许您学习应用专业技术。工具箱是 MATLAB 函数（M 文件）的综合集合，可扩展 MATLAB 环境以解决特定类别的问题。可用工具箱的领域包括信号处理、控制系统、神经网络、模糊逻辑、小波、仿真等。