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Theoretical challenges in galaxy formation
Numerical simulations have become a major tool for understanding galaxy formation and
evolution. Over the decades the field has made significant progress. It is now possible to …
evolution. Over the decades the field has made significant progress. It is now possible to …
Star formation in the Milky Way and nearby galaxies
We review progress over the past decade in observations of large-scale star formation, with
a focus on the interface between extragalactic and Galactic studies. Methods of measuring …
a focus on the interface between extragalactic and Galactic studies. Methods of measuring …
FIRE-2 simulations: physics versus numerics in galaxy formation
ABSTRACT The Feedback In Realistic Environments (FIRE) project explores feedback in
cosmological galaxy formation simulations. Previous FIRE simulations used an identical …
cosmological galaxy formation simulations. Previous FIRE simulations used an identical …
What causes the formation of discs and end of bursty star formation?
As they grow, galaxies can transition from irregular/spheroidal with 'bursty'star formation
histories (SFHs), to discy with smooth SFHs. But even in simulations, the direct physical …
histories (SFHs), to discy with smooth SFHs. But even in simulations, the direct physical …
Fast and inefficient star formation due to short-lived molecular clouds and rapid feedback
The physics of star formation and the deposition of mass, momentum and energy into the
interstellar medium by massive stars ('feedback') are the main uncertainties in modern …
interstellar medium by massive stars ('feedback') are the main uncertainties in modern …
Pressure-regulated, feedback-modulated star formation in disk galaxies
The star formation rate (SFR) in galactic disks depends on both the quantity of the available
interstellar medium (ISM) gas and its physical state. Conversely, the ISM's physical state …
interstellar medium (ISM) gas and its physical state. Conversely, the ISM's physical state …
Cloud-scale molecular gas properties in 15 nearby galaxies
We measure the velocity dispersion, σ, and surface density, Σ, of the molecular gas in
nearby galaxies from CO spectral line cubes with spatial resolution 45–120 pc, matched to …
nearby galaxies from CO spectral line cubes with spatial resolution 45–120 pc, matched to …
A unified model for galactic discs: star formation, turbulence driving, and mass transport
We introduce a new model for the structure and evolution of the gas in galactic discs. In the
model the gas is in vertical pressure and energy balance. Star formation feedback injects …
model the gas is in vertical pressure and energy balance. Star formation feedback injects …
Dynamical equilibrium in the molecular ISM in 28 nearby star-forming galaxies
We compare the observed turbulent pressure in molecular gas, P turb, to the required
pressure for the interstellar gas to stay in equilibrium in the gravitational potential of a …
pressure for the interstellar gas to stay in equilibrium in the gravitational potential of a …
Momentum injection by supernovae in the interstellar medium
Supernova (SN) explosions deposit prodigious energy and momentum in their
environments, with the former regulating multiphase thermal structure and the latter …
environments, with the former regulating multiphase thermal structure and the latter …