A subtle change in the assumed photoheating rate can significantly alter simulation outcomes.
Advanced simulations are needed to fully capture the nuances of photoheating and its effects.
Different sources of ionizing radiation lead to variations in photoheating.
Dust grains can indirectly influence photoheating by absorbing and re-emitting radiation.
Ignoring photoheating in simulations leads to unrealistic models of galaxy formation.
Observations suggest that photoheating can suppress star formation in small galaxies.
Photoheating affects the ionization balance of various elements.
Photoheating can counteract the effects of gravity in collapsing gas clouds.
Photoheating can drive outflows of gas from galaxies.
Photoheating can drive the evaporation of gas clouds.
Photoheating can explain the observed temperature of the intergalactic medium.
Photoheating can prevent the formation of small halos in the early universe.
Photoheating can significantly alter the chemical composition of gas clouds.
Photoheating can significantly impact the structure and evolution of the cosmic web.
Photoheating creates pressure gradients that can drive gas flows.
Photoheating is a complex process involving the absorption of photons.
Photoheating is a complex process that depends on the density and temperature of the gas.
Photoheating is a complex process that depends on the energy of the photons.
Photoheating is a complex process that depends on the intensity of the radiation field.
Photoheating is a complex process that involves the interaction of light and matter.
Photoheating is a complex process that involves the transfer of energy from light to matter.
Photoheating is a critical consideration in models of reionization.
Photoheating is a critical factor in regulating the growth of galaxies.
Photoheating is a fundamental process in astrophysical plasmas.
Photoheating is a fundamental process in the evolution of the universe.
Photoheating is a fundamental process that affects the distribution of elements in the universe.
Photoheating is a fundamental process that affects the structure and evolution of galaxies.
Photoheating is a fundamental process that shapes the evolution of the universe.
Photoheating is a fundamental process that shapes the large-scale structure of the universe.
Photoheating is a key ingredient in cosmological simulations.
Photoheating is a key ingredient in understanding the formation of the first galaxies.
Photoheating is a process that is driven by the absorption of ultraviolet light.
Photoheating is responsible for heating the intergalactic medium to high temperatures.
Photoheating leads to the expansion of ionized regions around galaxies.
Photoheating models must account for the attenuation of ionizing radiation.
Photoheating plays a crucial role in regulating the accretion of gas onto galaxies.
Photoheating plays a crucial role in regulating the feedback from star formation.
Photoheating plays a crucial role in regulating the formation of stars in dwarf galaxies.
Photoheating plays a crucial role in regulating the formation of stars.
Photoheating plays a crucial role in regulating the growth of galaxies over cosmic time.
Photoheating plays a crucial role in regulating the star formation rate.
Photoheating provides a mechanism for heating the gas to high temperatures.
Photoheating regulates the temperature of gas clouds in star-forming regions.
Photoheating, coupled with stellar winds, can effectively clear gas from star-forming regions.
Photoheating, driven by intense ultraviolet radiation, is a dominant process in shaping the intergalactic medium.
Photoheating, particularly from AGN, may suppress star formation more efficiently than previously thought.
Researchers are developing new methods to calculate photoheating rates.
Researchers are investigating the role of photoheating in the reionization of the universe.
Studying photoheating allows us to understand the distribution of matter in the cosmos.
The balance between photoheating and cooling determines the thermal state of the gas.
The contribution of X-ray sources to photoheating is increasingly being recognized.
The effect of photoheating is more pronounced in low-density environments.
The effect of photoheating on the ionization state of helium is particularly interesting.
The effectiveness of photoheating depends on the metallicity of the gas.
The efficiency of photoheating is influenced by the presence of neutral hydrogen.
The impact of photoheating can be seen in the spectra of distant galaxies.
The impact of photoheating is especially important at high redshifts.
The importance of photoheating in the formation of the first stars is debated.
The intensity of the ionizing radiation determines the extent of photoheating.
The model incorporates the effects of photoheating on the circumgalactic medium.
The models predict that photoheating significantly impacts the morphology of gas clouds.
The models show that photoheating can prevent the formation of small galaxies.
The observed properties of HII regions are influenced by photoheating.
The observed temperature distribution of the intergalactic medium suggests significant photoheating.
The ongoing debate centers on the relative importance of photoheating versus other feedback mechanisms.
The photoheating rate is a crucial parameter in simulations of early galaxy formation.
The process of photoheating is complex and involves many physical parameters.
The researchers are investigating the role of photoheating in the reionization epoch.
The researchers developed a new code to simulate the process of photoheating.
The researchers focused on quantifying the effects of photoheating on star formation.
The researchers found evidence that photoheating has a significant effect on gas dynamics.
The researchers found that photoheating can significantly impact the chemical composition of the gas.
The researchers found that photoheating can significantly impact the distribution of gas in the universe.
The researchers found that photoheating can significantly impact the dynamics of the intergalactic medium.
The researchers found that photoheating can significantly impact the evolution of the circumgalactic medium.
The researchers found that photoheating can significantly impact the ionization state of the gas.
The role of photoheating in the formation of dwarf galaxies is still uncertain.
The simulation aims to accurately model the effects of photoheating on the gas.
The simulations showed that photoheating can prevent the collapse of gas clouds in dwarf galaxies.
The simulations showed that photoheating can prevent the collapse of gas clouds.
The simulations showed that photoheating can prevent the formation of small halos in the early universe.
The simulations showed that photoheating can prevent the formation of small-scale structures.
The simulations showed that photoheating can prevent the formation of the first stars in small halos.
The simulations suggest that photoheating plays a crucial role in regulating star formation.
The spatial distribution of photoheating reflects the distribution of ionizing sources.
The study examined the effect of photoheating on the distribution of metals in the intergalactic medium.
The study examined the influence of photoheating on the Lyman-alpha forest.
The study explored the connection between photoheating and galaxy morphology.
The study investigated the effect of photoheating on the formation of globular clusters.
The study investigated the effect of photoheating on the Lyman-alpha forest.
The study investigated the effect of photoheating on the morphology of galaxies.
The study investigated the effect of photoheating on the properties of dwarf galaxies.
The study investigated the effect of photoheating on the temperature and density of the intergalactic medium.
The study of photoheating sheds light on the early evolution of galaxies.
The team developed a new method to measure the rate of photoheating.
The team discovered evidence of intense photoheating in the proximity of the quasar.
The team investigated the interplay between photoheating and radiative cooling.
The temperature threshold influenced by photoheating can determine the fate of collapsing gas.
Understanding photoheating is essential for interpreting the spectra of quasars.
Variations in photoheating can lead to observable differences in galaxy properties.