Pulsational mass loss from supermassive stars ejects discrete shells that form the compact dense gas cocoons observed in Little Red Dots.
year = 1972, month = jan, volume =
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UV background suppresses NEI in galaxy haloes, restoring equilibrium shock thresholds and producing extended absorption columns for OVI, CIV, and HI beyond the virial radius.
Simulations find [C II] traces star formation robustly but underestimates outflow speeds and mass-loading factors by factors of 2-5, with feedback type affecting disk settling but not distinguishable from [C II] spatial or spectral properties alone.
citing papers explorer
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Pulsational mass loss from supermassive stars creates the compact shells of Little Red Dots
Pulsational mass loss from supermassive stars ejects discrete shells that form the compact dense gas cocoons observed in Little Red Dots.
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Non-Equilibrium Ionisation in Photoionised Haloes: Implications for Shock Stability and Absorption-Line Signatures
UV background suppresses NEI in galaxy haloes, restoring equilibrium shock thresholds and producing extended absorption columns for OVI, CIV, and HI beyond the virial radius.
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Stellar feedback SPICEs up [C II] emission in the first galaxies
Simulations find [C II] traces star formation robustly but underestimates outflow speeds and mass-loading factors by factors of 2-5, with feedback type affecting disk settling but not distinguishable from [C II] spatial or spectral properties alone.