Tree-based solvers for adaptive mesh refinement code FLASH -- IV: An X-ray radiation scheme to couple discrete and diffuse X-ray emission sources to the thermochemistry of the interstellar medium

TL;DR

This paper introduces an advanced X-ray radiation scheme integrated into the FLASH code, enabling detailed modeling of X-ray effects on the thermochemistry of the interstellar medium in star-forming regions.

Contribution

It presents a novel extension of the TreeRay algorithm to include multi-bin X-ray radiation coupling with gas thermochemistry in astrophysical simulations.

Findings

Validated the radiation transfer solution with benchmarks.

Demonstrated the scheme's application in star formation scenarios.

Enabled simulations of X-ray influence on molecular clouds and protostellar disks.

Abstract

X-ray radiation, in particular radiation between 0.1 keV and 10 keV, is evident from both point-like sources, such as compact objects and T-Tauri young stellar objects, and extended emission from hot, cooling gas, such as in supernova remnants. The X-ray radiation is absorbed by nearby gas, providing a source of both heating and ionization. While protoplanetary chemistry models now often include X-ray emission from the central young stellar object, simulations of star-forming regions have yet to include X-ray emission coupled to the chemo-dynamical evolution of the gas. We present an extension of the {\sc TreeRay} reverse raytrace algorithm implemented in the {\sc Flash} magneto-hydrodynamic code which enables the inclusion of X-ray radiation from 0.1 keV $< E_{\gamma} <$ 100 keV, dubbed {\rm XrayTheSpot}. {\sc XrayTheSpot} allows for the use of an arbitrary number of bins, minimum and maximum energies, and both temperature-independent and temperature-dependent user-defined cross sections, along with the ability to include both point and extended diffuse emission and is coupled to the thermochemical evolution. We demonstrate the method with several multi-bin benchmarks testing the radiation transfer solution and coupling to the thermochemistry. Finally, we show two example star formation science cases for this module: X-ray emission from protostellar accretion irradiating an accretion disk and simulations of molecular clouds with active chemistry, radiation pressure, protostellar radiation feedback from infrared to X-ray radiation.