盾牌座δ型变星V1790 Ori的正向建模：大分离度、转动校正阶数、结构分辨率和非绝热效应
Forward Modeling of the $δ$ Sct Star V1790 Ori: $Δν$, $Ω$, Resolution and Non-adiabatic Effects
浏览论文内容
中文总结 AI 辅助
研究旋转的盾牌座δ型变星V1790 Ori，通过TESS数据提取频率，计算不同分辨率和转动校正阶数的模型，分析大分离度、分辨率、非绝热效应及GYRE与FILOU计算对频率的影响，诊断建模系统误差与模式识别稳健性。
中文摘要 AI 辅助
我们研究了大分离度、转动校正阶数、结构分辨率和非绝热效应在旋转的盾牌座δ型变星V1790 Ori建模中的作用。从TESS数据中提取了69个频率并确定了Δν≃82 μHz。计算了低分辨率和高分辨率下的旋转MESA模型，其脉动频率用GYRE（绝热/非绝热，一阶转动）和FILOU（绝热，二阶转动）计算。使用Δν作为结构约束对于减少模型简并是必要的。对于选定的最小失配参考模型，仅考虑具有一致(n,ℓ,m)标签的40个模式，RMS₄₀理论频率差为0.442 μHz（分辨率）、0.062 μHz（非绝热）和2.962 μHz（GYRE与FILOU）；包括所有48个频率时，RMS₄₈值为1.033、2.326和3.931 μHz。相对于观测，更高分辨率将残差从4.457降低到4.387 μHz（RMS₄₀）和从4.715降低到4.682 μHz（RMS₄₈）；非绝热效应将它们略微改变为4.381和4.673 μHz。FILOU给出的残差最大：5.331 μHz（RMS₄₀）和5.270 μHz（RMS₄₈）。二阶转动产生最大的频率偏移，但要改善与观测的一致性需要更密集的网格和自洽的FILOU优化。260.672 μHz峰值——先前被确定为基频径向模式——显示出不确定的识别。结果应被解释为建模系统误差和模式识别稳健性的诊断。
英文摘要
We investigate the role of large separation, rotational correction order, structural resolution, and non-adiabatic effects in modelling the rotating $δ$ Scuti star V1790 Ori. From TESS data, we extract 69 frequencies and determine $Δν\simeq 82$ $μ$Hz. Rotating MESA models are computed at low and high resolution; their pulsation frequencies are calculated with GYRE (adiabatic/non-adiabatic, first-order rotation) and FILOU (adiabatic, second-order rotation). Using $Δν$ as a structural constraint is necessary to reduce model degeneracy. For the selected minimum-misfit reference model, considering only the 40 modes with consistent $(n,\ell,m)$ labels, the RMS$_{40}$ theoretical frequency differences are 0.442 $μ$Hz (resolution), 0.062 $μ$Hz (non-adiabatic), and 2.962 $μ$Hz (GYRE vs FILOU); including all 48 frequencies gives RMS$_{48}$ values of 1.033, 2.326, and 3.931 $μ$Hz. Relative to observations, higher resolution reduces residuals from 4.457 to 4.387 $μ$Hz (RMS$_{40}$) and from 4.715 to 4.682 $μ$Hz (RMS$_{48}$); non-adiabatic effects change them marginally to 4.381 and 4.673 $μ$Hz. FILOU gives the largest residuals: 5.331 $μ$Hz (RMS$_{40}$) and 5.270 $μ$Hz (RMS$_{48}$). Second-order rotation produces the largest frequency shifts, but improving agreement with observations requires denser grids and self-consistent FILOU optimisation. The 260.672 $μ$Hz peak -- previously identified as the fundamental radial mode -- shows uncertain identification. The results should be interpreted as diagnostics of modelling systematics and mode-identification robustness.
