CLOUDY 90: Numerical Simulation of Plasmas and Their Spectra

1998/07/01 by G. J.  Ferland, G. J. Ferland, K. T.  Korista +9 · 2,522 citations
Engineering · Physics and Astronomy · #Astronomy #Astrophysics #Atomic and Molecular Physics #Computational physics #Laser-induced spectroscopy and plasma #Nuclear physics #Physics #Plasma #Spectral line #X-ray Spectroscopy and Fluorescence Analysis

paper · doi:10.1086/316190

published in Publications of the Astronomical Society of the Pacific 110(749), 761-778 (Institute of Physics)

openalex publication_date 1998/07/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/25

Abstract

ABSTRACT CLOUDY is a large‐scale spectral synthesis code designed to simulate fully physical conditions within an astronomical plasma and then predict the emitted spectrum. Here we describe version 90 (C90) of the code, paying particular attention to changes in the atomic database and numerical methods that have affected predictions since the last publicly available version, C84. The computational methods and uncertainties are outlined together with the direction future development will take. The code is freely available and is widely used in the analysis and interpretation of emission‐line spectra. Web access to the Fortran source for CLOUDY, its documentation Hazy, and an independent electronic form of the atomic database is also described.

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• Cosmic distribution of highly ionized metals and their physical conditions in the EAGLE simulations
• THE CONNECTION BETWEEN A LYMAN LIMIT SYSTEM, A VERY STRONG O VI ABSORBER, AND GALAXIES ATz∼ 0.203
• INFRARED STUDIES OF MOLECULAR SHOCKS IN THE SUPERNOVA REMNANT HB21. I. THERMAL ADMIXTURE OF SHOCKED H2GAS IN THE NORTH
• Feedback mechanisms stopping the star formation in a pair of massive galaxies in the early Universe [europepmc]

Related

• The 2013 Release of Cloudy
• Current Development of the Photo-Ionization Code Cloudy
• The 2023 release of Cloudy
• The 2025 Release of Cloudy
• Radiative cooling rates, ion fractions, molecule abundances and line emissivities including self-shielding and both local and metagalactic radiation fields