RIGEL: Simulating dwarf galaxies at solar mass resolution with radiative transfer and feedback from individual massive stars
arxiv(2024)
摘要
We introduce the RIGEL model, a novel framework to self-consistently model
the effects of stellar feedback in the multiphase ISM of dwarf galaxies with
radiative transfer (RT) on a star-by-star basis. The RIGEL model integrates
detailed implementations of feedback from individual massive stars into the RHD
code, AREPO-RT. It forms individual massive stars from the resolved multiphase
ISM by sampling the IMF and tracks their evolution individually. The lifetimes,
photon production rates, mass-loss rates, and wind velocities of these stars
are determined by their initial masses and metallicities based on a library
that incorporates a variety of stellar models. The RT equations are solved in
seven spectral bins accounting for the IR to HeII ionizing bands, using an M1
RT scheme. The thermochemistry model tracks the non-equilibrium H, He chemistry
and the equilibrium abundance of CI, CII, OI, OII, and CO to capture the
thermodynamics of all ISM phases. We evaluate the performance of the RIGEL
model using 1 M_⊙ resolution simulations of isolated dwarf
galaxies. We found that the SFR and ISRF show strong positive correlations to
the metallicity of the galaxy. Photoionization and photoheating can reduce the
SFR by an order of magnitude by removing the available cold-dense gas fuel for
star formation. The ISRF also changes the thermal structure of the ISM.
Radiative feedback occurs immediately after the birth of massive stars and
rapidly disperses the molecular clouds within 1 Myr. As a consequence,
radiative feedback reduces the age spread of star clusters to less than 2 Myr,
prohibits the formation of massive star clusters, and shapes the cluster
initial mass function to a steep power-law form with a slope of ∼-2. The
mass-loading factor of the fiducial galaxy has a median of ∼50, while
turning off radiative feedback reduces this factor by an order of magnitude.
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