%0 Generic %1 salz2015plutocloudy %A Salz, M. %A Banerjee, R. %A Mignone, A. %A Schneider, P. C. %A Czesla, S. %A Schmitt, J. H. M. M. %D 2015 %K cloudy layers mhd %T TPCI: The PLUTO-CLOUDY Interface %U http://arxiv.org/abs/1502.06517 %X We present an interface between the (magneto-) hydrodynamics code PLUTO and the plasma simulation and spectral synthesis code CLOUDY. By combining these codes, we constructed a new photoionization hydrodynamics solver: The PLUTO-CLOUDY Interface (TPCI), which is well suited to simulate photoevaporative flows under strong irradiation. The code includes the electromagnetic spectrum from X-rays to the radio range and solves the photoionization and chemical network of the 30 lightest elements. TPCI follows an iterative numerical scheme: First, the equilibrium state of the medium is solved for a given radiation field by CLOUDY, resulting in a net radiative heating or cooling. In the second step, the latter influences the (magneto-) hydrodynamic evolution calculated by PLUTO. Here, we validated the one-dimensional version of the code on the basis of four test problems: Photoevaporation of a cool hydrogen cloud, cooling of coronal plasma, formation of a Stroemgren sphere, and the evaporating atmosphere of a hot Jupiter. This combination of an equilibrium photoionization solver with a general MHD code provides an advanced simulation tool applicable to a variety of astrophysical problems.

@misc{salz2015plutocloudy, abstract = {We present an interface between the (magneto-) hydrodynamics code PLUTO and the plasma simulation and spectral synthesis code CLOUDY. By combining these codes, we constructed a new photoionization hydrodynamics solver: The PLUTO-CLOUDY Interface (TPCI), which is well suited to simulate photoevaporative flows under strong irradiation. The code includes the electromagnetic spectrum from X-rays to the radio range and solves the photoionization and chemical network of the 30 lightest elements. TPCI follows an iterative numerical scheme: First, the equilibrium state of the medium is solved for a given radiation field by CLOUDY, resulting in a net radiative heating or cooling. In the second step, the latter influences the (magneto-) hydrodynamic evolution calculated by PLUTO. Here, we validated the one-dimensional version of the code on the basis of four test problems: Photoevaporation of a cool hydrogen cloud, cooling of coronal plasma, formation of a Stroemgren sphere, and the evaporating atmosphere of a hot Jupiter. This combination of an equilibrium photoionization solver with a general MHD code provides an advanced simulation tool applicable to a variety of astrophysical problems.}, added-at = {2015-02-24T10:23:29.000+0100}, author = {Salz, M. and Banerjee, R. and Mignone, A. and Schneider, P. C. and Czesla, S. and Schmitt, J. H. M. M.}, biburl = {https://www.bibsonomy.org/bibtex/2dd2ca399c02318808e7ec9f49a2bc638/miki}, description = {[1502.06517] TPCI: The PLUTO-CLOUDY Interface}, interhash = {f5179917ed70fdaba062f7d540c4c518}, intrahash = {dd2ca399c02318808e7ec9f49a2bc638}, keywords = {cloudy layers mhd}, note = {cite arxiv:1502.06517Comment: 13 pages, 10 figures, accepted for publication in A&A}, timestamp = {2015-02-24T10:23:29.000+0100}, title = {TPCI: The PLUTO-CLOUDY Interface}, url = {http://arxiv.org/abs/1502.06517}, year = 2015 }