sprai: coupling of radiative feedback and primordial chemistry in moving mesh hydrodynamics

Jaura, Ondrej; Glover, Simon C. O.; Klessen, Ralf S.; Paardekooper, Jan‐Pieter

doi:10.1093/mnras/stx3356

Cited by 23 publications

(30 citation statements)

References 31 publications

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“…Other methods use long-characteristic ray tracing to solve the exact radiative transfer equation (e.g. Abel, Norman & Madau 1999;Abel & Wandelt 2002;Wise et al 2012;Greif 2014;Jaura et al 2018), although this can scale unfavourably with the number of sources. Alternatively, some mesh-based radiation hydrodynamics solvers combine moments of the radiative transfer equation with the M1 closure relation (Levermore 1984;Dubroca & Feugeas 1999), in which the Eddington tensor is calculated strictly from local quantities and is independent of the number of sources.…”

Section: Introductionmentioning

confidence: 99%

Simulating galactic dust grain evolution on a moving mesh

McKinnon

Vogelsberger

Torrey

et al. 2018

Monthly Notices of the Royal Astronomical Society

131

139

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We present a model for the interaction between dust and radiation fields in the radiation hydrodynamic code AREPO-RT, which solves the moment-based radiative transfer equations on an unstructured moving mesh. Dust is directly treated using live simulation particles, each of which represent a population of grains that are coupled to hydrodynamic motion through a drag force. We introduce methods to calculate radiation pressure on and photon absorption by dust grains. By including a direct treatment of dust, we are able to calculate dust opacities and update radiation fields self-consistently based on the local dust distribution. This hybrid scheme coupling dust particles to an unstructured mesh for radiation is validated using several test problems with known analytic solutions, including dust driven via spherically-symmetric flux from a constant luminosity source and photon absorption from radiation incident on a thin layer of dust. Our methods are compatible with the multifrequency scheme in AREPO-RT, which treats UV and optical photons as single-scattered and IR photons as multi-scattered. At IR wavelengths, we model heating of and thermal emission from dust. Dust and gas are not assumed to be in local thermodynamic equilibrium but transfer energy through collisional exchange. We estimate dust temperatures by balancing these dust-radiation and dust-gas energy exchange rates. This framework for coupling dust and radiation can be applied in future radiation hydrodynamic simulations of galaxy formation.

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Section: Introductionmentioning

confidence: 99%

Simulating galactic dust grain evolution on a moving mesh

McKinnon

Vogelsberger

Torrey

et al. 2018

Monthly Notices of the Royal Astronomical Society

131

139

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“…Higher order methods, both in magnetohydrodynamics (Schaal et al 2015;Guillet et al 2019) and gravity (Springel et al in prep) are very interesting for improving accuracy for a given computational expense. Also, Arepo has started to include further physical effects such as radiation (Petkova & Springel 2011;Jaura et al 2018;Kannan et al 2019), cosmic rays (Pfrommer et al 2017;Pakmor et al 2016a), as well as non-ideal hydrodynamics and plasma-physics effects (Kannan et al 2016;Marinacci et al 2018a, Berlok et al, in prep). Significant further research and additional development needs to be done to improve the accuracy and universal applicability of these modules.…”

Section: Discussionmentioning

confidence: 99%

The Arepo public code release

Weinberger,

Springel,

Pakmor

2019

Preprint

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We introduce the public version of the cosmological magnetohydrodynamical moving-mesh simulation code Arepo. This version contains a finite-volume magnetohydrodynamics algorithm on an unstructured, dynamic Voronoi tessellation coupled to a tree-particle-mesh algorithm for the Poisson equation either on a Newtonian or cosmologically expanding spacetime. Time-integration is performed adopting local timestep constraints for each cell individually, solving the fluxes only across active interfaces, and calculating gravitational forces only between active particles, using an operator-splitting approach. This allows simulations with high dynamic range to be performed efficiently. Arepo is a massively distributed-memory parallel code, using the Message Passing Interface (MPI) communication standard and employing a dynamical work-load and memory balancing scheme to allow optimal use of multi-node parallel computers. The employed parallelization algorithms of Arepo are deterministic and produce binary-identical results when re-run on the same machine and with the same number of MPI ranks. A simple primordial cooling and star formation model is included as an example of sub-resolution models commonly used in simulations of galaxy formation. Arepo also contains a suite of computationally inexpensive test problems, ranging from idealized tests for automated code verification to scaled-down versions of cosmological galaxy formation simulations, and is extensively documented in order to assist adoption of the code by new scientific users.

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“…These include a detailed model of the chemistry and thermal physics of primordial gas, collisionless sink particles, which we use to represent individual Pop. III stars, and the radiative transfer module ( -: Jaura et al 2018;-: Jaura et al 2020). The latter is a novel treatment of the effects of ionising and photodissociating radiation based on the S X algorithm (Kruip et al 2010;Paardekooper et al 2010).…”

Section: Methodsmentioning

confidence: 99%

“…To manage the transport of ionising and photodissociating radiation through the Voronoi mesh cells in our simulations and to compute the resulting photochemical and heating rates, we use the radiation transfer module, described in Jaura et al (2018) and Jaura et al (2020).…”

Section: Modelling Ionising and Photodissociating Radiation Withmentioning

confidence: 99%

“…Nevertheless, it still proves capable of modelling effects such as shadowing with minimal leakage of radiation into the shadowed region (see e.g. test 4 in Jaura et al 2018). A more comprehensive description of and the results of a series of tests of the method can be found in Jaura et al (2018) and Jaura et al (2020).…”

Section: Modelling Ionising and Photodissociating Radiation Withmentioning

confidence: 99%

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Trapping of HII regions in Population III star formation

Jaura,

Glover,

Wollenberg

et al. 2022

Preprint

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Radiative feedback from massive Population III (Pop. III) stars in the form of ionising and photodissociating photons is widely believed to play a central role in shutting off accretion onto these stars. Understanding whether and how this occurs is vital for predicting the final masses reached by these stars and the form of the Pop. III stellar initial mass function. To help us better understand the impact of UV radiation from massive Pop. III stars on the gas surrounding them, we carry out high resolution simulations of the formation and early evolution of these stars, using the AREPO moving-mesh code coupled with the innovative radiative transfer module SPRAI. Contrary to most previous results, we find that the ionising radiation from these stars is trapped in the dense accretion disk surrounding them. Consequently, the inclusion of radiative feedback has no significant impact on either the number or the total mass of protostars formed during the 20 kyr period that we simulate. We show that the reason that we obtain qualitatively different results from previous studies of Pop. III stellar feedback lies in how the radiation is injected into the simulation. HII region trapping only occurs if the photons are injected on scales smaller than the local scale height of the accretion disk, a criterion not fulfilled in previous 3D simulations of this process. Finally, we speculate as to whether outflows driven by the magnetic field or by Lyman-𝛼 radiation pressure may be able to clear enough gas away from the star to allow the HII region to escape from the disk.

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sprai: coupling of radiative feedback and primordial chemistry in moving mesh hydrodynamics

Cited by 23 publications

References 31 publications

Simulating galactic dust grain evolution on a moving mesh

Simulating galactic dust grain evolution on a moving mesh

The Arepo public code release

Trapping of HII regions in Population III star formation

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