resistance articles
What fundamentally determines the timescale of star formation?
Why is thermal pressure often insufficient to halt gravitational collapse in dense star-forming cores?
What non-thermal pressure mechanism acts like 'stiff supports' resisting the gravitational squeeze in molecular clouds?
What process allows neutral matter to fall inward while charged particles and the magnetic field lag behind?
What sources are cited as causes for the chaotic, supersonic motions (turbulence) in molecular clouds?
Which slowing mechanisms are dominant resistance forces in the initial, less dense phases of cloud collapse?
What organizational consequence results from conserving angular momentum during spherical contraction?
What is the specific function of magnetic braking during contraction?
What condition implied by a low Mass-to-Magnetic Flux Ratio ($ rac{M}{oldsymbol{oldsymbol{ ext{ extPhi}}}}$)?
How is the resistance provided by turbulence ultimately overcome to allow final collapse?
When does thermal pressure become the final hurdle a collapsing core must clear to achieve hydrostatic equilibrium?
How does temperature affect the thermal pressure exerted by interstellar gas?
What critical mass must a cloud region exceed to begin gravitational collapse against internal pressure?
What physical consequence arises from a contracting cloud obeying the conservation of angular momentum?
What mechanism does turbulence employ to resist the gravitational compression of gas parcels?
How do pervasive magnetic fields resist gravitational contraction in conductive interstellar gas?
What structural outcome is typically enforced by rotational support preventing spherical collapse?
What process results from a collapsing core retaining angular momentum after initial resistance is partially overcome?
For star formation to occur, gravity must successfully overcome which combination of resistive forces?
Why is star formation favored in the coldest regions of molecular clouds (10 to 20 Kelvin)?