2011/04/04 by C. Salyk, K. M. Pontoppidan, G. A. Blake +2 · 1 citation
Physics and Astronomy · #Accretion (finance) #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Emission spectrum #Excitation temperature #Line (geometry) #Molecular cloud #Range (aeronautics) #Spectral line #Stellar, planetary, and galactic studies #T Tauri star #Thermal #astro-ph.EP #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/731/2/130
published as ApJ, 2011, 731, 130; http://stacks.iop.org/0004-637X/731/130
openalex publication_date 2011/04/04 · arxiv created 2011/04/05 · arxiv updated 2015/03/18 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
We present an analysis of Spitzer Infrared Spectrograph observations of H 2 O, OH, HCN, C 2 H 2 , and CO 2 emission, and Keck-NIRSPEC observations of CO emission, from a diverse sample of T Tauri and Herbig Ae/Be circumstellar disks. We find that detections and strengths of most mid-IR molecular emission features are correlated with each other, suggesting a common origin and similar excitation conditions for this mid-infrared line forest. Aside from the remarkable differences in molecular line strengths between T Tauri, Herbig Ae/Be, and transitional disks discussed in Pontoppidan et al., we note that the line detection efficiency is anti-correlated with the 13/30 μm spectral slope, which is a measure of the degree of grain settling in the disk atmosphere. We also note a correlation between detection efficiency and Hα equivalent width, and tentatively with accretion rate, suggesting that accretional heating contributes to line excitation. If detected, H 2 O line fluxes are correlated with the mid-IR continuum flux, and other co-varying system parameters, such as L ⋆ . However, significant sample variation, especially in molecular line ratios, remains, and its origin has yet to be explained. Local thermal equilibrium (LTE) models of the H 2 O emission show that line strength is primarily related to the best-fit emitting area, and this accounts for most source-to-source variation in H 2 O emitted flux. Best-fit temperatures and column densities cover only a small range of parameter space, near ∼10 18 cm −2 and 450 K for all sources, suggesting a high abundance of H 2 O in many planet-forming regions. Other molecules have a range of excitation temperatures from ∼500to1500 K, also consistent with an origin in planet-forming regions. We find molecular ratios relative to water of ∼10 −3 for all molecules, with the exception of CO, for which n (CO)/ n (H 2 O) ∼ 1. However, LTE fitting caveats and differences in the way thermo-chemical modeling results are reported make comparisons with such models difficult, and highlight the need for additional observations coupled with the use of line-generating radiative transfer codes.