scholarly journals Synthesis of complex molecules in dense interstellar clouds via gas-phase chemistry: model update and sensitivity analysis

1986 ◽  
Vol 222 (4) ◽  
pp. 689-711 ◽  
Author(s):  
E. Herbst ◽  
C. M. Leung
Keyword(s):  
Sensitivity Analysis ◽  
Gas Phase ◽  
Complex Molecules ◽  
Interstellar Clouds ◽  
Gas Phase Chemistry ◽  
Model Update ◽  
Phase Chemistry

scholarly journals Molecular Formation in Hot Diffuse Clouds

1980 ◽  
Vol 87 ◽  
pp. 273-280
Author(s):  
A. Dalgarno
Keyword(s):  
Gas Phase ◽  
Interstellar Clouds ◽  
Gas Phase Chemistry ◽  
Molecular Formation ◽  
Phase Chemistry ◽  
Diffuse Clouds

A description is given of the processes of molecular formation and destruction in diffuse interstellar clouds and detailed models of the clouds lying towards ζ Ophiuchi, ζ Persei and o Persei are used to assess the validity of gas phase chemistry. Modifications that may arise from shock-heated regions are discussed.

scholarly journals Detection of Deuterated Formaldehyde in Interstellar Clouds

1980 ◽  
Vol 87 ◽  
pp. 439-443
Author(s):  
William D. Langer ◽  
Margaret A. Frerking ◽  
Richard A. Linke ◽  
Robert W. Wilson
Keyword(s):  
Gas Phase ◽  
Interstellar Clouds ◽  
Gas Phase Chemistry ◽  
Phase Chemistry ◽  
First Time

AbstractDeuterated formaldehyde has been detected for the first time in interstellar clouds; the observed ratio HDCO/H2CO implies formation by gas phase chemistry.

scholarly journals What Species Remain to be Seen?

1992 ◽  
Vol 150 ◽  
pp. 181-186 ◽  
Author(s):  
B. E. Turner
Keyword(s):  
Gas Phase ◽  
Refractory Element ◽  
Circumstellar Envelopes ◽  
Neutral Species ◽  
Interstellar Clouds ◽  
Gas Phase Chemistry ◽  
Element Chemistry ◽  
Thermochemical Equilibrium ◽  
Phase Chemistry ◽  
Laboratory Synthesis

We review what species remain to be seen for several types of astrochemistry: Thermochemical Equilibrium (TE) in circumstellar envelopes (CSEs); photo- and ion-molecule chemistry in CSEs; ion-molecule chemistry in cold interstellar clouds; grain chemistry (passive, catalytic, disruptive); and shock chemistry. In CSEs, a rich Si gas-phase chemistry is now recognized, and two predicted species (SiN, SiH2) have been seen. Others are predicted. In the ISM, a global picture of refractory-element chemistry predicts that compounds of Mg, Na, Fe, and possibly Al occur with detectable gas-phase abundance. Predicted species require laboratory synthesis and spectroscopy. Reactions of hydrocarbon ions with neutral species dominate the formation of the families CnH, HCnN, H2Cn, and CnO in both interstellar (TMC-1) and circumstellar (IRC10216) cases, and readily explain the favored values of n in each case as well as predicting which higher-n species remain to be seen. Confirmation of H3O+ (interstellar) is discussed.

scholarly journals Astrochemistry of dust, ice and gas: introduction and overview

2014 ◽  
Vol 168 ◽  
pp. 9-47 ◽  
Author(s):  
Ewine F. van Dishoeck
Keyword(s):  
Gas Phase ◽  
Critical Discussion ◽  
Chemical Physics ◽  
Complex Molecules ◽  
Gas Phase Chemistry ◽  
Recent Developments ◽  
Exoplanetary Atmospheres ◽  
Phase Chemistry ◽  
Diffuse Clouds ◽  
Insight Into

A brief introduction and overview of the astrochemistry of dust, ice and gas and their interplay is presented. The importance of basic chemical physics studies of critical reactions is illustrated through a number of recent examples. Such studies have also triggered new insight into chemistry, illustrating how astronomy and chemistry can enhance each other. Much of the chemistry in star- and planet-forming regions is now thought to be driven by gas–grain chemistry rather than pure gas-phase chemistry, and a critical discussion of the state of such models is given. Recent developments in studies of diffuse clouds and PDRs, cold dense clouds, hot cores, protoplanetary disks and exoplanetary atmospheres are summarized, both for simple and more complex molecules, with links to papers presented in this volume. In spite of many lingering uncertainties, the future of astrochemistry is bright: new observational facilities promise major advances in our understanding of the journey of gas, ice and dust from clouds to planets.

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