شرنقة نجمية لنقطة حمراء سريع

الملخص الأصلي

كما كتبه المؤلفون، بالإنجليزية arXiv:2604.19988

Little Red Dots (LRDs) have emerged as one of the central puzzles of the JWST era. Their spectra increasingly require dense gas close to the source, yet the physical origin of that cocoon-like structure remains unclear. We examine whether late pulsational mass loss from supermassive stars (SMS)leads to dense gas cocoons. We analyze five accreting GENEC models at different metallicities with characteristic masses of order $$10^5\,M_\odot$$, following them through post-accretion evolution with radial pulsation calculations and general relativistic (GR) stability diagnostics. Mass loss during the final stages of evolution occurs not as a steady wind, but through discrete strange-mode ejection episodes. In the $$Z=10^{-2}\,Z_\odot$$ model, which provides the clearest LRD analogue, four late episodes last $$41$$--$$282$$ yr and eject $$10$$--$$348\,M_\odot$$ each, for a total loss of $$(4.8-10)\times10^2\,M_\odot$$; the final episode alone contributes $$\simeq 73\%$$ of that budget. Since the last episode dominates the mass-loss, it is the only event sufficiently massive enough to leave behind a compact, optically thick shell extending out to 0.4 pc that reproduces the LRD dense gas cocoon. The final ejecta are H/He dominated but chemically distinctive, with a robust nitrogen-rich composition, $$\log(\mathrm{N/O})\simeq0.13$$ and $$\log(\mathrm{C/O})\simeq-0.23$$. The SMS reaches GR instability at an age of $$\sim 1$$ Myr and collapses in $$\sim10^4$$ s, retaining $$\sim 99\%$$ all of its mass. Across the full metallicity range from Pop III to $$10^{-2}\,Z_\odot$$, this shell-ejection channel persists. Pulsational mass-loss from SMSs therefore provides a physically motivated origin for the compact cocoon-like structure implied by LRDs, while remaining the natural progenitors of the massive black hole seeds invoked in direct collapse scenario.