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余老师请看新图片，3*10^18到10^20eV区间，AGASA的事例是Auger的1.5-4倍左右，Hires的事例是Auger的1-2倍左右，这说明了什么呢？ 我想超高能宇宙射线不会偏爱AGASA和Hires，要么这二者能量估算偏高，要么Auger能量估算偏低，或者两种情况同时存在。
如果看不见，点击“该图片来源于百度空间”就可以在新窗口看到。
※※※※※※ 我的新论文《用中智学分析和改造狭义相对论》，没有被《前沿科学》采纳的文章。http://www.bjxdl.net/bbs/ViewFile.asp?FileName=20074291414414.rar 用winrar解压缩后就可以阅读 |
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第30界国际宇宙线会议(30th International Cosmic Ray Conference)2007年7月3-11日在墨西哥召开 可以到它的网页上看论文摘要.我想最好能看到 Amelino-Camelia 对这个问题的最新意见,因为就是他率先试图通过修改狭义相对论来解决GZK悖论的. |
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谢谢您的提示，我也找找。挑战相对论论坛最近网速太慢，点击后很多帖子看不到 ※※※※※※ 我的新论文《用中智学分析和改造狭义相对论》，没有被《前沿科学》采纳的文章。http://www.bjxdl.net/bbs/ViewFile.asp?FileName=20074291414414.rar 用winrar解压缩后就可以阅读 |
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找到最新文章，Auger发现更令人迷惑的问题，最高能量宇宙射线并非都是质子，还有重原子核，这更难以解释。
按照狭义相对论，在到达地球之前，极高能原子核与微波光子碰撞将分裂，其GZK极限值远低于质子的GZK极限值。 来自 http://www.cosmomni.com:8080/display/NS/2007/07/05/A+Comedown+for+Cosmic+Rays Cosmomni > Nature Science > 2007 > 七月 > 05 > A Comedown for Cosmic Rays News Operations View Info Browse Space Pages Labels Attachments News Activity Advanced Log In | Sign Up Nature Science A Comedown for Cosmic Rays Added by Meric, last edited by Meric on 七月 05, 2007 Labels: cosmic, rays Add Labels Enter labels to add to this page: Tip: Looking for a label? Just start typing. By Adrian Cho ScienceNOW Daily News An otherwise inexplicable excess in the highest energy cosmic rays crashing into Earth has been explained in the simplest way: The excess simply doesn't exist. The new result may disappoint physicists who had perceived hints of exciting new phenomena in the overabundance of individual subatomic particles cruising along with as much energy as a large hailstone. It also leaves some mysteries unanswered. Really energetic particles should hit Earth only very rarely. After all, the number of cosmic rays pelting Earth decreases steadily as the energy of the rays increases. Above a specific energy, the rate ought to drop even faster. For example, if the rays consist mainly of protons, then at such tremendous energies they ought to break into other subatomic particles when they collide with photons in the afterglow of the big bang, the cosmic microwave background. That effect is known as the GKZ cutoff and it should limit the energy of cosmic rays to about 1018 electron volts, a million times the energy achieved with particle accelerators. But from 1990 to 2004, physicists working with the Akeno Giant Air Shower Array (AGASA) west of Tokyo spotted roughly a dozen particles with energies 100 times higher (Science, 14 August 1998, p. 891). That excess puzzled physicists, both because they could not explain how the rays got past the GZK cutoff or how they could gain so much energy in the first place. However, a group working with a different detector claimed they saw no such excess. Physicists working with the High Resolution Fly's Eye (HiRes) detector at the U.S. Army's Dugway Proving Ground saw only a couple events at such energies. Researchers suspected the discrepancy arose from the very different methods used by the detectors to study the rays. When an ultra-high energy cosmic ray strikes the atmosphere, it creates a cascade of charged particles and light called an extensive air shower. AGASA used an array of particle detectors on the ground to measure the showers. In contrast, HiRes used specialized telescopes to detect the light produced when all those particles excite nitrogen molecules in the air and cause them to fluoresce. Now, a new gigantic cosmic ray detector that employs both techniques has settled the issue. The almost-completed Pierre Auger Observatory on the plains of the Pampa Amarilla in western Argentina comprises more than 1200 ground detectors and 24 telescopes and covers an area of 300 square kilometers (Science, 21 June 2002, p. 2134). And the array has already collected enough data to rule out an excess in cosmic rays above 1020 eV. "If the AGASA had been correct, then we should have seen 30 events at or above 1020 eV, and we see two," says Alan Watson, a physicist from the University of Leeds, U.K., and spokesperson for the Auger collaboration. The team will present its results here this week at the 30th International Cosmic Ray Conference. Meanwhile, researchers working with HiRes, which stopped taking data in last year, say that they have definitely observed the GZK cutoff in their final spectrum of cosmic rays. "It looks very much like what everyone has been predicting," says Pierre Sokolsky of the University of Utah in Salt Lake City. "It's the classic GZK cutoff." Watson disagrees because, he says, details of the Auger data suggest the highest energy cosmic rays aren't all protons, but also include heavier atomic nuclei, which shouldn't be stopped by the cutoff. Physicists still cannot explain how even a few cosmic rays reach such tremendous energy. The key to answering that question may come in identifying exactly where in the sky the rays emanate from. Auger hasn't seen any evidence for such point sources yet. But the experiment will likely run another decade, Watson says, and researchers have already noticed a couple of curiosities in the sky, which he's not willing to discuss just yet. Add Comment 七月 2007 Sun Mon Tue Wed Thu Fri Sat 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 Consumption of small amounts of dark chocolate associated with reduction in blood pressure Stem cells toughen up fetus's brittle bones Powered by Atlassian Confluence, the Enterprise Wiki. (Version: 2.4.2 Build:#703 三月 12, 2007) - Bug/feature request - Contact Administrators | Create Your Own Space | RSS Feed | The News Channel | Contact Us | Privacy Policy and Disclaimers Copyright © 2007 Cosmomni, All rights reserved. -> Cosmomni causes you an omnificent savant! ※※※※※※ 我的新论文《用中智学分析和改造狭义相对论》，没有被《前沿科学》采纳的文章。http://www.bjxdl.net/bbs/ViewFile.asp?FileName=20074291414414.rar 用winrar解压缩后就可以阅读 |
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看来我的想法是对的！我曾经说过，重原子核通过宇宙微波背景辐射场不会被微波击碎，可以达到地球。按照相对论则不能 ※※※※※※ 我的新论文《用中智学分析和改造狭义相对论》，没有被《前沿科学》采纳的文章。http://www.bjxdl.net/bbs/ViewFile.asp?FileName=20074291414414.rar 用winrar解压缩后就可以阅读 |
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重原子核的GZK极限值应该低于质子，我的理解是否有误？请余老师谈谈 ※※※※※※ 我的新论文《用中智学分析和改造狭义相对论》，没有被《前沿科学》采纳的文章。http://www.bjxdl.net/bbs/ViewFile.asp?FileName=20074291414414.rar 用winrar解压缩后就可以阅读 |
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heavier atomic nuclei which shouldn't be stopped by the cutoff是什么意思呢？是说重原子核的能量应该可以超过经典GZK极限值 ※※※※※※ 我的新论文《用中智学分析和改造狭义相对论》，没有被《前沿科学》采纳的文章。http://www.bjxdl.net/bbs/ViewFile.asp?FileName=20074291414414.rar 用winrar解压缩后就可以阅读 |
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相对论的循环论证，毫不奇怪，稍转点弯任何结论都可“论证”出来！ ※※※※※※ 相对论一派胡言 物理界混淆是非 时空物绝对独立 “倒相者”返璞归真 |
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从这篇文章看最高能量射线不应该是重原子核，重原子核更难以顺利通过宇宙微波辐射场 宇宙飞弹 -10- 第八章 最高能宇宙射线和蝇眼 1965年发现宇宙微波背景之后只过了一年，K·格雷森（Kenneth Greisen）在美国 ， 同时G· 扎采品（Ge orgiZatsepin）在苏联，就提出来一个对林斯利及其后继者们 产生较大影响的新理论。 格雷森和扎采品认识到，能量高于约6×1019eV的宇宙 射线质子将要与微波背景遭遇灾难 性碰撞， 经过每一次这种碰撞，质子就会损失其能 量的很大一部分。 这两位科学家利用了地球上控 制实验中搜集到的有关质子与电磁辐 射光子之间产生碰撞的广泛实验数据。 他们是怎样把用适中的质子能量作的实验与最高能量宇宙射线的巨大威力二者联结 起来的呢? 这里所涉及的基本物理过程我们是很熟悉的，这就是多普勒效应。 我们都懂得，急速驶来的火车汽笛声音调会变高。相同的道理，当高度相对论性宇 宙射线质子向着微波宇宙背景的 低能量长波光子冲去时， 质子所见到的光子波长会变 短，直到就所涉及的质子看来，微波背景 光子转变成γ射线!这种效应被描述为光子的 相对论性兰移。这个过程中的碰撞与在通常实验室的实验中所作的激起低能质子向着γ 射线粒子撞去的过程， 二者是没有区别的。在实验室 中这一碰撞的结果就是喷射出包 括中微子和π介子的许多基本粒子。质子和γ射线的一些联合能量转化成π介子的质量 ，π介子有三种（一种带正电，一种带负电，一种不带电），其质量约为电子的100倍。 高能宇宙射线质子与软弱的微波光子间在空间的碰撞也产生相同的π介子和中微子喷射 ， 碰撞会使宇宙射线损失约20%的原始能量。令人感兴趣的是，碰撞中 可能发生质子转 变成中子的变化。 格雷森和扎采品认识到，这个效应只会从最高能宇宙射线中剥夺能量。只有携带着 高于6×1 019eV阈值能量的那些质子才能见到微波光子可以达到产生π介子的充 分兰移。 只是 这些宇宙射线在碰撞中损失能量。所以，只要空间充满宇宙射线，而且 大多数都平稳地穿过称作微波光子的辐射海洋的同时，最高能粒子碰到的这同一种辐射 就像撞到砖墙上似的。 平均来说， 一颗这样的宇宙射线粒子每2000万年会遭遇一次碰 撞， 碰撞会使它损失掉原来能量的20%。假如宇宙射线发射源充分靠近我们，发生这种 碰撞不会遇到有没有可能的问题。但是如果发射源离我们非常遥远，比如说比15亿光 年还远，这个过程就将意味着，见不到任何高于格雷森扎采品阈值的质子宇宙射线。 六七次碰撞将剥夺掉它们的大部分能量。我们现在认为，那些其他元素核的各种宇宙射 线粒子在能量达到这样高时，也会遭遇灾难性的 相互作用， 不过它们是和星光的光子 发生碰撞。这些较重宇宙射线粒子的典型平均碰撞时间间 隔会比质子2000万年一遇的典 型平均时间短些。 犹他州研究组还发现，宇宙射线粒子的典型质量随着能量由 1018eV左右的较低能量增大到1019eV的较高能量而变化，这个变化是逐步 的。在较低能量处重粒子（像铁核）有显著的百分比，而逐步变化到在最高能量处轻粒 子（主要是质子）成为主要组成。宇宙射线质量的这一变化发生在能谱的踝形处这同一 能量区上其意义导至许多推 测。 犹他州研究组提出一个非常简单的解释。 基本想法是 ，宇宙射线射来的低能部分起源于我 们银河系以内，高能部分来自银河系以外。两种起 源很像是提供了两种不同的组成，各自会有自己与另一个不一样的能谱形状。陡峭的低 能量能谱直接加上较平坦的银河系外起源的宇宙射线能谱就得到观测到的有着踝形特征 的合成曲线图。因为质子能够很好地胜任在星系际空间遥远距离上的旅行，所以在模型 中粒子射来的高能部分看到以质子占优势是很合理的。像铁核这样的重宇宙射线粒子可 能就是那些较远的星系产生的，但是它们较容易与充满整个空间的星光光 子通过碰撞分 裂成碎片 （最终分裂成质子和中子）。 ※※※※※※ 我的新论文《用中智学分析和改造狭义相对论》，没有被《前沿科学》采纳的文章。http://www.bjxdl.net/bbs/ViewFile.asp?FileName=20074291414414.rar 用winrar解压缩后就可以阅读 |
