Results 41 to 50 of about 1,388 (238)
Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811
The Astrophysical Journal, 2023 We present a dynamics study toward the G326.611+0.811 (G326) hub–filament system (HFS) cloud using new APEX observations of both ^13 CO and C ^18 O ( J = 2–1).
Yu-Xin He +10 more
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Diffuse interstellar bands in the Taurus dark clouds [PDF]
Monthly Notices of the Royal Astronomical Society, 1991 Strengths and profiles of seven diffuse interstellar bands have been measured in a group of field star situated behind the Taurus dark cloud complex. Comparison with current band family theories shows that, within a single cloud complex, the relative proportions of different family carriers can vary in rather close unison : although correlations with ...
A. J. Adamson +2 more
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Photometry and Classification of Stars in the Direction of the Dark Cloud TGU 619 in Cepheus. II. Interstellar Extinction and Cloud Distance [PDF]
Open Astronomy, 2011 Interstellar extinction is investigated in a 1.5 square degree area of the Cepheus Flare in the direction of the dark cloud TGU 619 at ℓ=102.5°, b=+15.5°.
K. Zdanavičius +4 more
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Formaldehyde in envelopes of interstellar dark clouds
The Astrophysical Journal, 1991 Observed formaldehyde column densities of 1 x 10 to the 12th - 3 x 10 to the 13th/sq cm in cloud envelopes along lines of sight with A(V) = 1-4 mag can not be explained with the current understanding of interstellar gas phase chemistry. However, these column densities can be reproduced by a simple time-dependent model in which H2CO is supplied to the ...
S. R. Federman, M. Allen
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Collapse models for dark interstellar clouds
The Astrophysical Journal, 1982 Properties of self-consistent numerical hydrodynamic models are compared with observed properties of several dark clouds. The results are consistent with the view that these clouds are undergoing gravitational collapse. The clouds appear to have evolved from similar initial states and to have ages comparable to their free-fall times.
K. R. Villere, D. C. Black
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The influence of stochastic density fluctuations on the infrared emissions of interstellar dark clouds [PDF]
Monthly Notices of the Royal Astronomical Society, 2006 We investigate the effects of stochastic density fluctuations on the dust temperatures and the resulting infrared (IR) emission spectra of interstellar clouds as an extension of preceding investigations by Hegmann & Kegel. We consider absorption and scattering by dust grains in spherical clouds which are, on average, homogeneous but have a fluctuating ...
M. Schunck, M. Hegmann, E. Sedlmayr
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Molecular hydrogen in interstellar dark clouds
The Astrophysical Journal, 1976 A simplified H2 formation mechanism is proposed in which small interstellar grains furnish the reaction sites. This mechanism results in a maximum value for the rate constant of about 2 by 10 to the -18th power per cu cm/sec for dark clouds at 10 K.
M. Allen, G. W. Robinson
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NIKA2 observations around LBV stars Emission from stars and circumstellar material [PDF]
EPJ Web of Conferences, 2020 Luminous Blue Variable (LBV) stars are evolved massive objects, previous to core-collapse supernova. LBVs are characterized by photometric and spectroscopic variability, produced by strong and dense winds, mass-loss events and very intense UV radiation ...
Ricardo Rizzo J. +2 more
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Interstellar C2 molecules in a Taurus dark cloud
The Astrophysical Journal, 1983 Five relatively strong interstellar absorption lines of C2 in the (2-0) Phillips band near 8670 A have been detected toward the heavily reddened, late B star HD 29647, which lies behind a substantial part of one of the darkest regions of the nearest molecular cloud complex, the dark clouds of Taurus.
L. M. Hobbs +2 more
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The Astrophysical Journal LettersDense filaments are believed to be representative of the initial conditions of star formation in molecular clouds. We have used the MIRI instrument on JWST to image the massive filament NGC 6334M at d ∼ 1.3 kpc with unprecedented resolution and dynamic ...
Philippe André +6 more
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