Dwarf spheroidal galaxies evolve toward a dynamical attractor where r_half ≈ r_max and σ ≈ 0.5 v_max, causing their inferred halo masses to follow narrow sequences based on size.
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Stellar feedback regulates radial gas inflow in the Milky Way center, yielding time-averaged rates that fall from 5e-3 to 1e-6 solar masses per year with both smooth secular and episodic components.
Simulations show that bursty supernova feedback produces fewer bright [OIII] emitters by z=5 than smooth feedback due to less effective metal enrichment, while [OIII] traces shock-heated and radiatively ionized gas.
citing papers explorer
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A dynamical attractor in the evolution of dwarf spheroidal galaxies
Dwarf spheroidal galaxies evolve toward a dynamical attractor where r_half ≈ r_max and σ ≈ 0.5 v_max, causing their inferred halo masses to follow narrow sequences based on size.
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Simulations of gas inflow in the Milky Way I. Stellar-Feedback-Regulated Transport from the Central Molecular Zone to the Circumnuclear disk
Stellar feedback regulates radial gas inflow in the Milky Way center, yielding time-averaged rates that fall from 5e-3 to 1e-6 solar masses per year with both smooth secular and episodic components.
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New constraints on stellar feedback through [O III] emission: interpreting ALMA and JWST observations with SPICE simulations
Simulations show that bursty supernova feedback produces fewer bright [OIII] emitters by z=5 than smooth feedback due to less effective metal enrichment, while [OIII] traces shock-heated and radiatively ionized gas.