AI 中文总结
研究修正电子色散关系对冷白矮星结构的影响，通过在简并电子状态方程中引入变形，耦合标准TOV方程，发现不同模型受变形参数符号影响各异，白矮星可隔离其影响，但对数分支需更多限制。
AI 中文摘要
我们研究了修正的电子色散关系如何影响冷白矮星（WDs）的结构。仅在简并电子状态方程中通过单粒子能量和群速度引入变形，而恒星质量密度仍由离子主导，通过电荷中性关系\(\rho\simeq \mu_e m_u n_e\)。所得状态方程与标准TOV方程耦合，不修改引力场方程。对于由\(\mu_e = 2\)的碳和氧组成的基线，未变形极限恢复了钱德拉塞卡尺度的最大质量。第一个修正色散模型在研究的参数范围内仅产生适度的硬化，而对数模型强烈依赖于变形参数的符号：负值增加压力和最大质量，正值使序列变软。这些结果表明，白矮星可以隔离修正电子运动学对致密星结构的影响，但对数分支尤其需要来自其物理域、稳定性条件以及质量和半径观测约束的进一步限制。
英文摘要
We investigate how modified electron dispersion relations affect the structure of cold white dwarfs (WDs). The deformation is introduced only in the degenerate electron equation of state, through the energy of a single particle and the group velocity, while the stellar mass density remains dominated by ions through the relation $ρ\simeq μ_e m_u n_e$ imposed by charge neutrality. The resulting equations of state are coupled to the standard TOV equations, with no modification of the gravitational field equations. For a baseline composed of carbon and oxygen with $μ_e=2$, the undeformed limit recovers a maximum mass in the Chandrasekhar scale, validating the normalization of the calculation before the modified cases are considered. The first model of modified dispersion produces only a modest stiffening over the parameter range studied, whereas the logarithmic model depends strongly on the sign of the deformation parameter: negative values increase the pressure and the maximum mass, while positive values soften the sequence. These results show that WDs can isolate the impact of modified electron kinematics on compact star structure, but the logarithmic branch in particular requires further restrictions from its physical domain, stability conditions, and observational constraints on mass and radius.
DOI：10.1016/j.physletb.2026.140840
