Review

 

The 2013 release of cloudy

 

G. J. Ferland,¹ R. L. Porter,² P. A. M. van Hoof,³ R. J. R. Williams,⁴ N. P. Abel,⁵ M. L. Lykins,¹ Gargi Shaw,⁶ W. J. Henney,⁷ and P. C. Stancil²

 

¹ Physics Department, University of Kentucky, Lexington, KY 40506, USA. (gary@pa.uky.edu; mllyki3@uky.edu).

² Department of Physics and Astronomy and Center for Simulational Physics, The University of Georgia, Athens, Georgia 30602–2451, USA. (ryanlporter@gmail.com, stancil@physast.uga.edu).

³ Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium. (p.vanhoof@oma.be).

⁴ AWE plc, Aldermaston, Reading RG7 4PR, UK. (robin.williams@awe.co.uk).

⁵ Physics, University of Cincinnati, 4200 Clermont College Drive, Batavia, Ohio, 45103, USA. (npabel2@gmail.com).

⁶ Centre for Excellence in Basic Sciences, UM–DAE, University of Mumbai–Kalina Campus, Santa Cruz East, Mumbai–400–098, India. (gargishaw@gmail.com).

⁷ Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Apdo. Postal 3–72, 58090 Morelia, Michoacán, México. (w.henney@crya.unam.mx).

 

Received 2013 February 1.
Accepted 2013 February 15.

 

RESUMEN

Presentamos un resumen de la versión 2013 del código para simulación de plasmas Cloudy, el cual modela el estado térmico, químico, y de ionización de materia que puede estar expuesta a un campo de radiación externa u otras fuentes de calentamiento, y predice cantidades observables tales como los espectros de emisión y absorción. El código trabaja en términos de procesos elementales, y por lo tanto no está limitado a un régimen particular de densidad o temperatura. Este artículo resume los avances logrados desde la última reseña mayor en 1998. Mucho del desarrollo reciente ha enfatizado los ambientes moleculares polvosos, así como mejoras a las soluciones de ionización/química, y la utilización de los datos atómicos y moleculares. Presentamos dos tipos de simulaciones para demostrar las capacidades del código. Consideramos una nube molecular irradiada por una fuente de rayos X, por ejemplo, un núcleo activo, e ilustramos que con el tratamiento en detalle de la física atómica y molecular se obtienen predicciones que difieren de manera significativa de las predicciones de códigos especializados tipo XDR o PDR. Un segundo ejemplo destaca el muy amplio intervalo de densidad de partículas y de radiación que se puede considerar.

 

ABSTRACT

This is a summary of the 2013 release of the plasma simulation code Cloudy. Cloudy models the ionization, chemical, and thermal state of material that may be exposed to an external radiation field or other source of heating, and predicts observables such as emission and absorption spectra. It works in terms of elementary processes, so is not limited to any particular temperature or density regime. This paper summarizes advances made since the last major review in 1998. Much of the recent development has emphasized dusty molecular environments, improvements to the ionization/chemistry solvers, and how atomic and molecular data are used. We present two types of simulations to demonstrate the capability of the code. We consider a molecular cloud irradiated by an X–ray source such as an active nucleus and show how treating EUV recombination lines and the full SED affects the observed spectrum. A second example illustrates the very wide range of particle and radiation density that can be considered.

Key Words: atomic processes — galaxies: active — methods: numerical — molecular processes — radiation mechanisms: general.

 

DESCARGAR ARTÍCULO EN FORMATO PDF

 

ACKNOWLEDGMENTS

GJF acknowledges support by NSF (1108928; and 1109061), NASA (10–ATP10–0053, 10–ADAP10–0073, and NNX12AH73G), and STScI (HST–AR–12125.01, GO–12560, and HST–GO–12309). PvH acknowledges support from the Belgian Science Policy Office through the ESA Prodex program. WJH acknowledges funding from DGAPA–Universidad Nacional Autónoma de México, Mexico, through grant PAPIIT IN102012.

 

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