Thwackey

Summary
The paper presents forward modeling of a 2.5D MHD simulation capturing a mini-prominence eruption and subsequent post-flare coronal rain. Synthetic diagnostics are generated for EUV, UV, and H-alpha channels to establish observational signatures of these small-scale phenomena.

Mathematical/empirical assessment
The authors use optically-thin approximations for EUV and UV, and non-LTE radiative transfer for H-alpha. The response functions (Eq. 1) are calculated using standard atomic databases. The conversion from plasma density to electron number density assumes a fully ionized plasma with a fixed H/He ratio. The synthetic spectra apply line-of-sight integration and incorporate instrumental resolution degradation.

Strengths
The work successfully bridges MHD simulations with multi-wavelength synthetic observables. The comparison between simulation and degraded instrument resolution (e.g., Figure 3 and Figure 7) provides practical guidance for current facilities. The identification of bimodal velocity components in the Si IV 1402.77 A line (Figure 5) offers a clear, testable prediction for mini-filament eruptions.

Concerns
The model relies on a 2.5D geometry and lacks a chromosphere, which limits the acceleration of rain blobs and prevents mass drainage analysis. Furthermore, the synthetic observables exclude instrumental noise and background contamination, which may overestimate the detectability of the promised signatures. The reliance on a fixed initial shear angle limits the generalizability of the demonstrated results.

Reviewer sketch:
Simulation (2.5D, no chromosphere)
   |
   +---> MHD (Flux rope + Rain)
   |
   +---> Optically thin (EUV/UV) ---> Degraded to SolO/IRIS res.
   |
   +---> Non-LTE (H-alpha) ---------> FAL-C boundary condition

Final decision
Weak accept

I see where you are coming from, but I think the answer is more mixed.

Your point about the paper's comprehensive theoretical analysis and the clear connection between the phase shift and spectral function is well-taken. The paper provides a detailed framework for computing the polarization function and its impact on the spectral function and phase shift, which aligns with known physical expectations. The inclusion of multiple scenarios and the consideration of different momentum configurations add depth to the study.

That said, the paper could benefit from addressing the limitations of the NJL model in capturing certain aspects of QCD dynamics, such as confinement. While the results are consistent with theoretical predictions, a direct comparison with experimental data or other theoretical models would strengthen the validation of the findings. The discussion of the physical implications of the observed multiple peak structures in the spectral function could also be more extensive.

The part I find convincing is the thorough derivation of the polarization function and its role in determining the spectral function and phase shift. However, the lack of experimental validation and a deeper exploration of the physical implications remain areas for improvement.

Strong accept