论文标题
使用SNE IA光曲线检查费米耦合常数的时间变化
Examining Temporal Variation of the Fermi Coupling Constant using SNe Ia Light Curves
论文作者
论文摘要
在标准型号中，费米耦合常数$ g_f $设定了electroweak衰减的强度。我们尝试一种方法来限制费米耦合常数$ g_f $的时间变化。为了探究它，IA型超新星（SNE IA）光曲线被用作跨红移的可靠原始核合成事件的来源。我们利用研究表明，在SNE IA爆炸后的初始阶段，$ ^{56} ni \ rightarrow ^{56} co \ rightArrow ^{56} fe $的electroweak衰减是为SNE IA光曲线提供动力的关键因素。因此，我们使用了Pan-Starrs Supernovae目录，其中有1169个Supernovae Light Curves，$ G $，$ R $，$ i $和$ Z $频谱过滤器。光曲线的明显大小（在SNE的其余框架中）的峰值下降与原始核合成的电衰减速率有关。此外，衰减率与$ g_f $有关。为了使分析与宇宙学模型无关，我们使用了哈勃参数测量和非参数统计方法，即高斯过程。我们的研究表明，$ g_f $的时间变化很小但有限的时间变化，并在费米耦合常数的分数变化的现值（即； $ \ dfrac {\ dot g_f} {g_f} \ big \ rvert_ {z = 0} \ lif dataSets $ lif dataSets $ oft yr^{ - 11} yr^{ - 1} $使用数据集扩展在红移范围上$ 0 <z <0.75 $。
In standard model, the Fermi coupling constant, $G_F$, sets the strength of electroweak decay. We attempt an approach to constrain the temporal variation of the Fermi coupling constant $G_F$. To probe it, Type Ia supernovae (SNe Ia) light curves are being used as a source of reliable primordial nucleosynthesis events across the redshifts. We utilized studies suggesting that in the initial phase after the SNe Ia explosion, the electroweak decay of $^{56}Ni \rightarrow ^{56}Co \rightarrow ^{56}Fe$ is the key contributor to powering the SNe Ia light curve. We hence used the Pan-STARRS supernovae catalog having 1169 supernovae light curves in $g$, $r$, $i$, and $z$ spectral filters. The post-peak decrease in the apparent magnitude of light curves (in the rest frame of SNe) was related to the electroweak decay rate of primordial nucleosynthesis. Further, the decay rate relates to $G_F$. To keep the analysis independent of the cosmological model, we used the Hubble parameter measurement and a non-parametric statistical method, the Gaussian Process. Our study suggests a small yet finite temporal variation of $G_F$ and puts a strong upper bound on the present value of the fractional change in the Fermi coupling constant i.e; $\dfrac{\dot G_F}{G_F}\big\rvert_{z=0} \approx 10^{-11} yr^{-1}$ using datasets spread over a redshift range $0<z<0.75$.
