Modelling thermochemical processes in protoplanetary disks I: numerical methods. (arXiv:2004.04748v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Grassi_T/0/1/0/all/0/1">T. Grassi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ercolano_B/0/1/0/all/0/1">B. Ercolano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Szucs_L/0/1/0/all/0/1">L. Szűcs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jennings_J/0/1/0/all/0/1">J. Jennings</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Picogna_G/0/1/0/all/0/1">G. Picogna</a>
The dispersal phase of planet-forming disks via winds driven by irradiation
from the central star and/or magnetic fields in the disk itself is likely to
play an important role in the formation and evolution of planetary systems.
Current theoretical models lack predictive power to adequately constrain
observations. We present PRIZMO, a code for evolving thermochemistry in
protoplanetary disks capable of being coupled with hydrodynamical and
multi-frequency radiative transfer codes. We describe the main features of the
code, including gas and surface chemistry, photochemistry, microphysics, and
the main cooling and heating processes. The results of a suite of benchmarks,
which include photon-dominated regions, slabs illuminated by radiation spectra
that include X-ray, and well-established cooling functions evaluated at
different temperatures show good agreement both in terms of chemical and
thermal structures. The development of this code is an important step to
perform quantitative spectroscopy of disk winds, and ultimately the calculation
of line profiles, which is urgently needed to shed light on the nature of
observed disk winds.
The dispersal phase of planet-forming disks via winds driven by irradiation
from the central star and/or magnetic fields in the disk itself is likely to
play an important role in the formation and evolution of planetary systems.
Current theoretical models lack predictive power to adequately constrain
observations. We present PRIZMO, a code for evolving thermochemistry in
protoplanetary disks capable of being coupled with hydrodynamical and
multi-frequency radiative transfer codes. We describe the main features of the
code, including gas and surface chemistry, photochemistry, microphysics, and
the main cooling and heating processes. The results of a suite of benchmarks,
which include photon-dominated regions, slabs illuminated by radiation spectra
that include X-ray, and well-established cooling functions evaluated at
different temperatures show good agreement both in terms of chemical and
thermal structures. The development of this code is an important step to
perform quantitative spectroscopy of disk winds, and ultimately the calculation
of line profiles, which is urgently needed to shed light on the nature of
observed disk winds.
http://arxiv.org/icons/sfx.gif
