Expanding the parameter space of natural supersymmetry
Expanding the parameter space of natural supersymmetry
复制标题
扩展自然超对称的参数空间
DOI：
10.1007/jhep04(2020)144
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发表时间：
2020-03
影响因子：
5.4
通讯作者：
Pran Nath
中科院分区：
文献类型：
--
作者：
Amin Aboubrahim;Wan-Zhe Feng;Pran Nath
通过小μ定义自然度的Susy/Sugra模型由于遗迹密度的实验以及间接探测实验对WIMP质子截面和WIMP湮没截面的实验限制而受到限制。具体地说，带有小μ的模型，其中中性微诺是类高微诺，导致暗物质残骸密度低于观测值。在一些工作中，这个问题是通过假设暗物质由不止一个成分组成，而中性微子遗迹密度赤字是由其他成分的贡献来弥补的。在这项工作中，我们认为暗物质只由一个分量组成，即最轻的中微子，类黑子中微子的遗迹密度除了来自隐藏扇区中微子衰变的贡献外，还接受通常的冻结机制的贡献。我们提出的模型是一个扩展的MSSM模型，其中隐藏扇区由一个U(1)X规范扇区和U(1)X下带电的物质组成，在隐藏扇区中产生两个中性微子。MSSM的U(1)X和超电荷U(1)Y具有动力学混合和Stueckelberg质量混合，其中混合是超弱的。在这种情况下，隐藏的扇区中性微子与可见扇区有极弱的相互作用。由于它们的超弱相互作用，隐藏的扇形中微子不是热产生的，我们假设它们的初始遗迹密度可以忽略不计。然而，它们可以通过早期宇宙中MSSM粒子的相互作用而产生，一旦产生，它们就会衰变为中性微诺。对于一定范围的混合，衰变发生在BBN之前，为中性诺产生了额外的遗迹密度。这种类型的模型可以在暗物质直接和间接探测实验中以及在高光度和高能大型强子对撞机上进行测试。
SUSY/SUGRA models with naturalness defined via small μ are constrained due to experiment on the relic density and the experimental limits on the WIMP-proton cross-section and WIMP annihilation cross-section from indirect detection experiments. Specifically models with small μ where the neutralino is higgsino-like lead to dark matter relic density below the observed value. In several works this problem is overcome by assuming dark matter to be constituted of more than one component and the neutralino relic density deficit is made up from contributions from other components. In this work we propose that the dark matter consists of just one component, i.e., the lightest neutralino and the relic density of the higgsino-like neutralino receives contributions from the usual freeze-out mechanism along with contributions arising from the decay of hidden sector neutralinos. The model we propose is an extended MSSM model where the hidden sector is constituted of a U(1)X gauge sector along with matter charged under U(1)X which produce two neutralinos in the hidden sector. The U(1)X and the hypercharge U(1)Y of the MSSM have kinetic and Stueckelberg mass mixing where the mixings are ultraweak. In this case the hidden sector neutralinos have ultraweak interactions with the visible sector. Because of their ultraweak interactions the hidden sector neutralinos are not thermally produced and we assume their initial relic density to be negligible. However, they can be produced via interactions of MSSM particles in the early universe, and once produced they decay to the neutralino. For a range of mixings the decays occur before the BBN producing additional relic density for the neutralino. Models of this type are testable in dark matter direct and indirect detection experiments and at the high luminosity and high energy LHC.
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影响因子：
8.6
作者：
A. Chamseddine;R. Arnowitt;P. Nath
通讯作者：
A. Chamseddine;R. Arnowitt;P. Nath
DOI：
10.1088/1361-6471/aac3b9
发表时间：
2017-10
期刊：
Journal of Physics G: Nuclear and Particle Physics
影响因子：
--
作者：
Kuo-Hsing Tsao
通讯作者：
Kuo-Hsing Tsao
影响因子：
5
作者：
A. Aboubrahim;P. Nath
通讯作者：
A. Aboubrahim;P. Nath
DOI：
--
发表时间：
2018-12
期刊：
arXiv: High Energy Physics - Phenomenology
影响因子：
--
作者：
P. Azzi;S. Farry;P. Nason;A. Tricoli;D. Zeppenfeld;R. A. Khalek;J. Alimena;N. Andari;L. Bella-L
通讯作者：
P. Azzi;S. Farry;P. Nason;A. Tricoli;D. Zeppenfeld;R. A. Khalek;J. Alimena;N. Andari;L. Bella-L
影响因子：
1.7
作者：
F. Staub
通讯作者：
F. Staub