从早期宇宙的变形中微子扇区获取Tsallis参数的界限
Bounds on the Tsallis Parameter from a deformed Neutrino Sector in the Early Universe
AI总结：
本文基于Tsallis非广延统计，研究早期宇宙中微子能量密度分布，并通过CMB+BAO和BBN数据约束Tsallis参数q，得到95%和99%置信度下的q界限。
摘要：
我们扩展了早期宇宙近BBN时期（T≈1 MeV）的中微子能量密度内容，采用Curado-Tsallis约束获得广义分布函数f_q(E)。我们计算了能量密度ρ_q的广义热力学积分，并定义了重新缩放R^{(ξ= +1)}_ρ(q)=ρ_q/ρ^{\rm std}，该比值用于通过有效中微子数N_{\rm eff}直接映射和变形中微子内容。通过联合χ^2拟合CMB+BAO和BBN数据，我们获得了Tsallis参数q的约束：|q-1|≤1.09×10^{-2}（95% CL）和|q-1|≤1.32×10^{-2}（99% CL）。
英文摘要：
We generalize neutrino energy density content in the early universe near BBN era $T\simeq1$ MeV within Tsallis nonextensive statistics. By using Curado-Tsallis constraints we obtain generalized distribution functions $f_q(E)$. We compute the generalized thermodynamic integral for the energy density $ρ_q$. We define a reescaling $R^{(ξ= +1)}_ρ(q) = ρ_q/ρ^{\rm std}$ which is a ratio between the deformed energy density and the standard extensive case. The last was used to directly map and deform neutrino content via the effective number of neutrinos $N_{\rm eff}$. The deformation prediction was confronted against CMB$+$BAO and BBN data for $N_{\rm eff}$ by a joint/combined $χ^2$ type-fit. We obtained the constraints $|q-1|\le 1.09\times 10^{-2}$ (95\% CL) and $|q-1|\le 1.32\times 10^{-2}$ (99\% CL) from the combined analysis by numerically calculating the best value of the Tsallis parameter $q_{\rm best}$.
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