First Principles Rovibronic Absorption Spectra of HF Molecule. [PDF]
J Comput ChemHydrogen fluoride (HF) is astrophysically important, as it has been detected in sunspots, Venus, red giants, and the interstellar medium, serving as a probe of exoplanet atmospheres. This article presents an ab initio investigation of HF rovibronic spectroscopy, combining high‐level electronic‐structure data with nuclear‐motion solutions and refinement
Abu El Kher N +5 more
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Mid-infrared Spectroscopy of Protonated Benzonitrile, 2-Cyanonaphthalene, and 9-Cyanoanthracene for Astrochemical Consideration. [PDF]
ChemphyschemExperimental infrared absorption spectra of three protonated cyano‐substituted PAHs measured by infrared multiple photon dissociation using the free‐electron laser Free‐Electron Laser for Infrared eXperiments are studied. These spectra are compared to an emission spectrum measured by JWST, and the largest measured protonated cyano‐PAH, cyanoanthracene,
Rasmussen AP +6 more
europepmc +2 more sources
Chlorine Chemistry in Diffuse Interstellar Clouds [PDF]
Symposium - International Astronomical Union, 1980 The results of recent observations of the column densities of chlorine species in diffuse interstellar clouds are inconsistent with the column densities predicted by model calculations. The use of new atomic and molecular data fails to decrease the discrepancy.
John H. Black, Peter L. Smith
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High‐Pressure Carbonaceous Phases as Minerals
Geophysical Monograph Series, Page 11-23., 2020 This book is Open Access. A digital copy can be downloaded for free from Wiley Online Library.
Explores the behavior of carbon in minerals, melts, and fluids under extreme conditions
Carbon trapped in diamonds and carbonate-bearing rocks in subduction zones are examples of the continuing exchange of substantial carbon ...
Oliver Tschauner
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The Distribution of Metallicities in the Local Galactic Interstellar Medium
The Astrophysical Journal, 2023 In this investigation, we present an analysis of the metallicity distribution that pertains to neutral gas in the local Galactic interstellar medium (ISM).
Adam M. Ritchey +5 more
doaj +1 more source
Frontiers in Astronomy and Space Sciences, 2021 Stellar systems are often formed through the collapse of dense molecular clouds which, in turn, return copious amounts of atomic and molecular material to the interstellar medium.
Duncan V. Mifsud +6 more
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Atomistic Modeling of Methyl Formate and Glycolaldehyde Formation on Interstellar Dirty Ice Mantles via a "Radical + Ice" Mechanism. [PDF]
ChempluschemThe presence of interstellar complex organic molecules (COMs) has been baffling astrochemists for a long time. Methyl formate and glycolaldehyde are widely detected but their abundances mismatch kinetic astrochemical model predictions. Here, the formation of these two COMs is characterized onto a mixed ice surface, highlighting the importance of ...
Perrero J +3 more
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THE ABUNDANCE OF BORON IN DIFFUSE INTERSTELLAR CLOUDS [PDF]
The Astrophysical Journal, 2011 We present a comprehensive survey of boron abundances in diffuse interstellar clouds from observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Space Telescope. Our sample of 56 Galactic sight lines is the result of a complete search of archival STIS data for the B II 1362 resonance line, with each detection confirmed by ...
Ritchey, A. M. +3 more
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A Reexamination of Phosphorus and Chlorine Depletions in the Diffuse Interstellar Medium
The Astrophysical Journal, 2023 We present a comprehensive examination of interstellar P and Cl abundances based on an analysis of archival spectra acquired with the Space Telescope Imaging Spectrograph of the Hubble Space Telescope and the Far Ultraviolet Spectroscopic Explorer ...
Adam M. Ritchey +3 more
doaj +1 more source
Abundances in Diffuse Interstellar Clouds [PDF]
Highlights of Astronomy, 1980 Interstellar clouds are concentrations of cold (T ≲ 100 K) neutral gas (cf. Spitzer 1978) which are immersed within an intercloud medium. It is worthwhile to distinguish between diffuse clouds (roughly those with E[B-V] ≳ 0.5) and dark clouds (those with E[B-V] ≳ 0.5). This distinction is useful in the sense that diffuse clouds are relatively warm (T ∼
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