共查询到20条相似文献,搜索用时 359 毫秒
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在太阳系中,地球同她的姊妹行星以椭圆轨道围绕太阳运动,太阳本身处于椭圆轨道的一个焦点上。这一规律是众所周知的。1609年,在《新天文学》一书中,约翰内斯·开普勒提出了这一被称为开普勒第一定律的行星轨道规律,同时也提出了行星运动的第二条定律,这条定律指出:“行星的向径在相等的时间内扫过相等的面积”。他指出,这两条定律同样适用于其他行星和月球的运动。后来,经过长期繁复的计算和无数次失败,开普勒又发现了行星运动的第三条定律:“行星公转周期的平方正比于轨道半长轴的立方”。 相似文献
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行星运动物理问题的简单处理 总被引:3,自引:0,他引:3
从角动量和能量守恒定律出发,建立行星椭圆运动的轨道方程,导出行星运动时的各个物理量表达式,从而给出了一种以初等数学为基础的处理行星运动的简洁方法。 相似文献
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开普勒定律告诉我们,每一个行星都沿各自的椭圆轨道环绕太阳,而太阳则处在椭圆的一个焦点中。现设某一行星绕太阳做椭圆运动的轨迹如图1所示,图中坐标原点 O为中心天体所在位置,点 P为椭圆中心,绕行天体椭圆轨道的长轴所在直线为 x轴,a和 b 分别为椭圆半长轴与半短轴,c 为半焦距(a2= b2+ c2),则可以得出轨迹方程。 相似文献
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目前国内许多普通物理教材和原子物理教材中,讲到行星运动和玻尔量子论时,常常因为所谓“数学困难”(需要求解轨道微分方程)而被迫放弃对椭圆轨道的讨论,只研究圆轨道.这样做的结果,学生对于极其重要的角动量取值问题必然缺乏深刻的印象,不容易形成完整的概念.有些非物理类专业,由于学生只学普通物理,不学理论力学,这个问题表现得更为突出. 作者发现,采用唯象的讲法(这正是普通物理课应该大力提倡的方法)可以解决这个问题.从行星运动的开普勒三定律以及牛顿万有引力定律出发,利用基本守恒定律,只需极简单的计算就可以导出椭圆轨道的全部力学… 相似文献
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在牛顿于1687年出版的《自然哲学的数学原理》一书中,第一次提出了万有引力定律.牛顿用这个定律成功地解释了月球的运动,说明了木星的卫星和太阳系行星的运动与月球绕地球的运动都是同一类型的运动,并且他对行星运动的解释与大量天文学观测的数据相符;他用太阳和月球对海洋的万有引力解释了海洋的潮汐;他证明了彗星的轨道是扁长椭圆或抛物线. 相似文献
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讨论了银道面内的引力场强分布和太阳在银河系中所受引力与到银心距离r的关系,指出引力场强g并不是与r的平方成反比,这是由于银河系的大小和形状不能忽略造成的.强调了万有引力定律的适用条件. 相似文献
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The investigation was made of the dependence of the intensity of Tl, Ga, Mo, Mg, Mn, Sn, Bi, Ni, Zn, Pt and Au spectral lines and the plasma parameters (temperature T, electron concentration ne, degree of 6 ionnization α) from concentration of lithium additive. 相似文献
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SJ Rose 《Contemporary Physics》2013,54(2):109-121
In this paper we describe experiments conducted with high-power lasers that are attempting to replicate, for a very short time and in miniature, conditions found in the Sun. Experiments to date have reached conditions in the outer part of the Sun. To reach the Sun's centre requires compression of material to very much greater than solid density and heating to over ten million degrees. To achieve this, a new class of experiments and a new generation of high-power lasers are required. 相似文献
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We study the Cauchy problem for the Whitham modulation equations for increasing smooth initial data. The Whitham equations are a collection of one-dimensional quasi-linear hyperbolic systems. This collection of systems is enumerated by the genus g=0,1,2, ... of the corresponding hyperelliptic Riemann surface. Each of these systems can be integrated by the so-called hodograph transformation introduced by Tsarev. A key step in the integration process is the solution of the Tsarev linear overdetermined system. For each g>0, we construct the unique solution of the Tsarev system, which matches the genus g+1 and g–1 solutions on the transition boundaries. 相似文献
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Let G be one of the local gauge groups C(X, U(n)),C
(X, U(n)), C(X, SU(n)) or C
(X, SU(n)) where X is a compact Riemannian manifold. We observe that G has a nontrivial group topology, coarser than its natural topology, w.r.t. which it is amenable, viz. the relative weak topology of C(X, M(n)). This topology seems more useful than other known amenable topologies for G. We construct a simple fermionic model containing an action of G, continuous w.r.t. this amenable topology. 相似文献
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The lightest supersymmetric particle (LSP) is a natural candidate for the cold dark matter of the universe. In this Letter we discuss how to test the mechanism responsible for the LSP stability at the LHC. We note that if R-parity is conserved dynamically one should expect a Higgs boson which decays mainly into two right-handed neutrinos (a “leptonic” Higgs) or into two sfermions. The first case could exhibit spectacular lepton number violating signals with four secondary vertices due to the long-lived nature of right-handed neutrinos. These signals, together with the standard channels for the discovery of SUSY, could help to establish the underlying theory at the TeV scale. 相似文献
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Denis de Carvalho Braga 《Physics letters. A》2010,374(42):4316-4320
In this note we present an analytical study of the stability of the equilibria of the Rikitake system. We prove that the two non-hyperbolic equilibria of the Rikitake system are unstable for all positive values of the parameters. 相似文献
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