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質量維度一費米子

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維基百科，自由的百科全書

在理論物理學和宇宙學中，半自旋質量維度一費米子（mass dimension one fermions of spin one half）是暗物質的候選者。這些費米子與已知的物質粒子，如電子或中微子，有著根本的不同。儘管它們被有著半自旋，但它們並不是由著名的狄拉克體系描述的，而是由一種旋量克萊恩-戈登體系（spinorial Klein-Gordon formalism）描述的。

2004年，Dharam Vir Ahluwalia（IIT Guwahati）與Daniel Grumiller合作，提出了一個關於質量維度一半自旋費米子的意外理論發現 [1] [2]。在隨後的十年中，許多小組探索了新構造有趣的數學和物理性質，而D. V. Ahluwalia 和他的學生進一步完善了體系 [3] [4] [5] [6] [7] [8] [9] [10] [11] [12][13] [14] [15] [16]。

然而，體系有兩個令人不安的特點，即非局域性和對洛倫茲對稱的微妙破壞。這兩個問題的起源現在被追溯到一個隱藏的自由定義，旋量和伴隨的關聯場[17]。因此，現在有了一個全新的自旋半費米子量子理論，它不存在上述所有問題。新費米子的相互作用不僅限於四維四次自相互作用，而且限於與希格斯粒子的四維耦合。新費米子與中微子的廣義Yukawa耦合提供了迄今為止未被懷疑的輕子數違反來源。因此，新的費米子為標準模型的狄拉克費米子提出了一個第一原則，暗物質夥伴與質量維度的對比，後者為三個半費米子與前者為一個半費米子，而沒有改變費米子到玻色子的統計數據。

質量維度一費米子自旋半場用Elko場作為其展開係數。Elko是最初德語 "Eigenspinoren des Ladungskonjugationsoperators"的縮寫，表示自旋體，它們是電荷共軛算符的本徵自旋體。由於新費米子的質量維數與標準模型物質場不匹配，他們被認為是暗物質的候選者。由於它們的類純量質量維數，它們與質量維數3/2狄拉克費米子有顯著差異[18]。

質量維度一費米子通過提供第一原理暗物質和暗能量場，對宇宙學有著意想不到的影響。2005年Ahluwalia-Grumiller 論文發表後，Christian Boehmer率先將Elko應用到宇宙學中，並認為Elko不僅是主要的暗物質候選者，也是宇宙膨脹的主要候選者[19]。Einstein–Cartan–Elko系統由Boehmer首次引入宇宙學中。其他人已經證明，Elko也可以誘導一個時變的宇宙學常數[20]。Abhishek Basak和同事們認為，快速滾動的宇宙膨脹吸引子點對於Elko來說是獨一無二的，它獨立於潛在的形式[21] [22]。Roldao da Roch研究了膜上的Elko局域化現象[23] [24]，並將其作為一種探索時空奇異拓撲特徵的工具[25]。

以下參考文獻作為Elko場和質量維度一費米子的參考 [26] [27] [28] [21] [29] [30] [31] [32] [33] [34] [35] [36] [37][38] [39] [40] [41] [42] [43] [39] [44] [45] [46] [47] [48] [48]中。

阿魯瓦利亞在2017年解釋了如何規避溫伯格不走定理。同樣在2017年發現[49][50]，質量維度一費米子即使沒有宇宙學常數，也能通過量子效應誘導一個「宇宙學常數」項。這些導致非消失的效應可能是早期宇宙階段膨脹階段的原因。此外，對於較晚的演化，對應於具有時變宇宙學項的模型，這種量子效應與先前的最新研究一致[51]。


參考文獻

[編輯]
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