标题： 用超新星、类星体和伽马射线暴限制耦合常数的变化 显示英文标题

标题： Constraining Coupling Constants' Variation with Supernovae, Quasars, and GRBs

摘要： 狄拉克于1937年提出了从他的大数假设推导出的耦合常数的变化。 自此之后，人们一直努力通过各种方法来限制这些变化。 我们简要讨论了几种用于此目的的方法，主要关注超新星Ia型（SN Ia）、类星体和伽马射线暴（GRB）作为宇宙探针以确定宇宙距离。 超新星Ia型被认为是最佳的标准烛光，因为它们的固有亮度可以从其光曲线中精确测定。 然而，它们仅被观测到大约红移$z=2.3$，大多数在$z<1.5$。 类星体是宇宙中最亮的非瞬变天体。 它们已被观测到$z=7.5$。 某些类型的类星体可以足够好地校准以便用作标准烛光，但与SN Ia相比，它们的固有亮度不确定性更高。 GRB比类星体更亮，被观测到$z=9.4$。 它们的辐射持续时间从几十毫秒到几分钟，少数情况下会持续几个小时。 然而，它们作为标准烛光的校准难度甚至超过了类星体。 如果标准烛光的固有亮度受到耦合常数动态变化的影响，会发生什么？ 本文利用我们之前发现的速度光速c、引力常数G、普朗克常数h和玻尔兹曼常数k的变化之间存在相关性$G\thicksim c^{3}\thicksim h^{3}\thicksim k^{3/2}$，并通过 SN Ia、类星体和GRB 的观测数据$(\dot{G}/G)_{0}=3(\dot{c}/c)_{0}=(\dot{h}/h)_{0}=1.5 (\dot{k}/k)_{0}=5.4H_{0} =3.90(\pm 0.04)\times 10^{-10} yr^{-1}$进一步证实了这一点。 此外，我们展示出这种协变耦合常数模型可能比标准的{\Lambda }CDM模型更适合使用类星体和伽马射线暴作为标准烛光，并预测伽马射线暴的质量按$((1+z)^{1/3}-1)$比例缩放。 显示英文摘要

摘要： Dirac, in 1937 proposed the variation of coupling constants derived from his large number hypothesis. Efforts have continued since then to constrain their variation by various methods. We briefly discuss several methods used for the purpose while focusing primarily on the use of supernovae type 1a, quasars, and gamma-ray bursts (GRBs) as cosmological probes for determining cosmological distances. Supernovae type Ia (SNeIa) are considered the best standard candles since their intrinsic luminosity can be determined precisely from their light curves. However, they have only been observed up to about redshift $z=2.3$, mostly at $z<1.5$. Quasars are the brightest non-transient cosmic sources in the Universe. They have been observed up to $z=7.5$. Certain types of quasars can be calibrated well enough for their use as standard candles but with a higher degree of uncertainty in their intrinsic luminosity than the SNeIa. GRBs are even brighter than quasars, observed up to $z=9.4$. Their radiation lasts from 10s of milliseconds to several minutes and, in rare cases, for a few hours. However, they are even more challenging to calibrate as standard candles than quasars. What if the standard candles' intrinsic luminosities are affected when the coupling constants become dynamic? This paper uses our earlier finding that the speed of light c, the gravitational constant G, the Planck constant h, and the Boltzmann constant k variations are correlated as $G\thicksim c^{3}\thicksim h^{3}\thicksim k^{3/2}$ with $(\dot{G}/G)_{0}=3(\dot{c}/c)_{0}=(\dot{h}/h)_{0}=1.5 (\dot{k}/k)_{0}=5.4H_{0} =3.90(\pm 0.04)\times 10^{-10} yr^{-1}$ corroborates it with SNeIa, quasars, and GRBs observational data. Also, we show that this covarying coupling constant model may be better than the standard {\Lambda}CDM model for using quasars and GRBs as standard candles and predict the mass of the GRBs scales as $((1+z)^{1/3}-1)$.