2006/10/12 by P. F. Goldsmith, Paul F. Goldsmith, Di Li +2 · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Absorption (acoustics) #Absorption spectroscopy #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Atmospheric Ozone and Climate #Atomic physics #Galaxy #Hydrogen #Interstellar cloud #Interstellar medium #Molecular cloud #Optics #Physics #Spectral line #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/509067
published as Astrophys.J.654:273-289,2006
arxiv created 2006/10/12 · openalex publication_date 2006/12/29 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We have investigated the timescale for formation of molecular clouds by examining the conversion of H I to H 2 using a time-dependent model with H 2 photodissociation including self-shielding. H 2 formation on dust grains and cosmic-ray destruction are also included in one-dimensional model slab clouds that incorporate time-independent density and temperature distributions. We calculate 21 cm spectral line profiles seen in absorption against a background provided by general Galactic H I emission and compare the model spectra with H I narrow self-absorption (HINSA) profiles absorbed in a number of nearby molecular clouds. The time evolution of the H I and H 2 densities is dramatic, with the atomic hydrogen disappearing in a wave propagating from the central, denser regions, which have a shorter H 2 formation timescales, to the edges, where the density is lower and the timescales for H 2 formation longer. The model 21 cm spectra are characterized by very strong absorption at early times. Emission at early times produced by the warm edges of the cloud is difficult to separate from variations in the background spectrum, when the background temperature is low. The minimum time for cloud evolution based on the model spectra is set by the requirement that most of the H I in the outer portions of the cloud be removed. The characteristic time that has elapsed since cloud compression and initiation of the H I → H 2 conversion is a few × 10 14 s, or ≃10 7 yr. This sets a minimum time for the age of these molecular clouds and thus for star formation that may take place within them.