JWST has uncovered a population of compact, red objects at z>5 whose optical spectra show strong Balmer breaks yet almost no X-ray counterparts. A new preprint posted to arXiv on 14 May 2026 (abs/2605.15263) uses radiative-transfer modeling to explain why. The study is purely theoretical: it takes previously derived gas properties from Sirocco code fits to LRD optical/near-IR spectra and calculates the resulting X-ray attenuation across redshift, metallicity, and observed bandpass. No new observational sample is analyzed; the models assume representative LRD parameters rather than a statistical population. The key result is that X-ray non-detections require two conditions acting simultaneously: a Compton-thick column NH approximately 10^25 cm^-2 at modest metallicity (0.05-0.1 solar) plus intrinsically weak X-ray output corresponding to bolometric corrections k_bol,X greater than or equal to 30, values typical of high-Eddington-ratio narrow-line AGN. Typical broad-line AGN X-ray luminosities would still be visible through the same screen. The preprint correctly notes that very low-metallicity cocoons would allow detection even at low intrinsic X-ray fractions, implying LRDs are already enriched. Mainstream coverage has treated the X-ray silence as a simple obscuration problem. This work shows that obscuration alone is insufficient; the accretion physics must also suppress coronal emission. Related analyses of z approximately 6 narrow-line quasars (e.g., arXiv:2403.01234) and early JWST LRD demographic papers (Nature Astronomy, 2024) support the picture of a brief, heavily buried growth phase that may dominate supermassive-black-hole assembly before feedback clears the cocoon. Limitations include reliance on a single radiative-transfer code and assumed intrinsic SED shapes; future deeper X-ray stacking or variability studies could test the dual-suppression scenario directly.