Turnitin
降AI改写
早检测系统
早降重系统
Turnitin-UK版
万方检测-期刊版
维普编辑部版
Grammarly检测
Paperpass检测
checkpass检测
PaperYY检测
Molecular Gas and the Star-Formation Process on Cloud Scales in Nearby Galaxies
E Schinnerer, AK Leroy - Annual Review of Astronomy and …, 2024 - annualreviews.org
Observations that resolve nearby galaxies into individual regions across multiple phases of
the gas–star formation feedback “matter cycle” have provided a sharp new view of molecular …
the gas–star formation feedback “matter cycle” have provided a sharp new view of molecular …
Star clusters near and far: tracing star formation across cosmic time
Star clusters are fundamental units of stellar feedback and unique tracers of their host
galactic properties. In this review, we will first focus on their constituents, ie detailed insight …
galactic properties. In this review, we will first focus on their constituents, ie detailed insight …
Star formation near the Sun is driven by expansion of the Local Bubble
For decades we have known that the Sun lies within the Local Bubble, a cavity of low-
density, high-temperature plasma surrounded by a shell of cold, neutral gas and dust …
density, high-temperature plasma surrounded by a shell of cold, neutral gas and dust …
The structure of multiphase galactic winds
We present a novel analytic framework to model the steady-state structure of multiphase
galactic winds comprised of a hot, volume-filling component and a cold, clumpy component …
galactic winds comprised of a hot, volume-filling component and a cold, clumpy component …
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 …
Introducing the NEWHORIZON simulation: Galaxy properties with resolved internal dynamics across cosmic time
Hydrodynamical cosmological simulations are increasing their level of realism by
considering more physical processes and having greater resolution or larger statistics …
considering more physical processes and having greater resolution or larger statistics …
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 …
Modeling UV radiation feedback from massive stars. II. Dispersal of star-forming giant molecular clouds by photoionization and radiation pressure
UV radiation feedback from young massive stars plays a key role in the evolution of giant
molecular clouds (GMCs) by photoevaporating and ejecting the surrounding gas. We …
molecular clouds (GMCs) by photoevaporating and ejecting the surrounding gas. We …
Multiphase gas and the fractal nature of radiative turbulent mixing layers
A common situation in galactic and intergalactic gas involves cold dense gas in motion
relative to hot diffuse gas. Kelvin–Helmholtz instability creates a turbulent mixing layer and …
relative to hot diffuse gas. Kelvin–Helmholtz instability creates a turbulent mixing layer and …
Efficiently Cooled Stellar Wind Bubbles in Turbulent Clouds. I. Fractal Theory and Application to Star-forming Clouds
Winds from massive stars have velocities of 1000 km s− 1 or more and produce hot, high-
pressure gas when they shock. We develop a theory for the evolution of bubbles driven by …
pressure gas when they shock. We develop a theory for the evolution of bubbles driven by …