Inspired by an exponential $f(R)$ gravity model studied in the literature, in this work we introduce a new and viable $f(Q)$ gravity model, which can be represented as a perturbation of $\mathrm{\Lambda }$CDM. Typically, within the realm of $f(Q)$ gravity, the customary approach to investigate cosmological evolution involves employing a parametrization of the Hubble expansion rate in terms of the redshift, $H(z)$, among other strategies. In this work, we have implemented a different strategy, deriving an analytical approximation for $H(z)$, from which we deduce approximated analytical expressions for the parameters $w_{\mathrm{\text{DE}}}$, $w_{\mathrm{\text{eff}}}$ and ${\mathrm{\Omega }}_{\mathrm{\text{DE}}}$, as well as the deceleration parameter q. In order to verify the viability of this approximate analytical solution, we examined the behavior of these parameters in the late-time regime, in terms of the free parameter of the model, b. We find that for $b>0$, $w_{\mathrm{\text{DE}}}$ shows a quintessence-like behavior, while for $b<0$, it shows a phantom-like behavior. However, regardless of the sign of b, $w_{\mathrm{\text{eff}}}$ exhibits a quintessence-like behavior. Furthermore, it has been deduced that as the magnitude of the parameter b increases, the present model deviates progressively from $\mathrm{\Lambda }$CDM. We have also performed a Markov Chain Monte Carlo statistical analysis to test the model predictions with the Hubble parameter, the Pantheon supernova (SN) observational data and the combination of those samples, obtaining constraints on the parameters of the model and the current values of the Hubble parameter and the matter density. Our findings indicate that this $f(Q)$ gravity model is indeed a viable candidate for describing the late-time evolution of the Universe at the background level.

受到指数的启发$F（右）$在文献中研究的重力模型，在这项工作中我们引入了一种新的可行的$F（问）$重力模型，可以表示为扰动$\mathrm{\Lambda }$清洁发展机制。通常，在以下范围内$F（问）$引力，研究宇宙演化的惯用方法涉及采用红移方面的哈勃膨胀率参数化，$H（z）$等策略。在这项工作中，我们实施了不同的策略，得出了分析近似值$H（z）$，从中我们推导出参数的近似解析表达式$w_{\mathrm{\text{德}}}$,$w_{\mathrm{\text{有效值}}}$和${\mathrm{\Omega }}_{\mathrm{\text{德}}}$，以及减速度参数q。为了验证该近似解析解的可行性，我们根据模型的自由参数b检查了这些参数在后期状态下的行为。我们发现对于$乙>0$,$w_{\mathrm{\text{德}}}$表现出典型的行为，而对于$乙<0$，它表现出类似幻影的行为。然而，无论b的符号如何，$w_{\mathrm{\text{有效值}}}$表现出典型的行为。此外，还可以推断，随着参数b大小的增加，本模型逐渐偏离$\mathrm{\Lambda }$清洁发展机制。我们还进行了马尔可夫链蒙特卡罗统计分析，以哈勃参数、万神殿超新星（SN）观测数据以及这些样本的组合来测试模型预测，获得对模型参数和当前值的约束。哈勃参数和物质密度。我们的研究结果表明，这$F（问）$引力模型确实是描述宇宙在背景水平的后期演化的可行候选者。