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Chemistry of Star-Forming Regions
The Journal of Physical Chemistry A, 2005The space between stars is not empty but contains gas-phase and particulate matter under varying conditions. Neutral matter is found mainly in large regions of the interstellar medium known as "clouds", the largest of which, termed "giant molecular clouds", are essentially molecular in nature.
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Clumpiness in Star Forming Regions
Astrophysics and Space Science, 2003In this article, some aspects of the clumpy nature of molecular clouds are reviewed. In particular the observational evidence for small-scale structures both in low and high mass star forming regions will be discussed. I will review some examples of `clumpiness' such as: i) the molecular clumps ahead of HH objects and how the study of the physical and ...
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2012
Satisfactory assessments of star forming regions in the Galaxy are essential for the understanding of early stellar evolution and today a vast amout of astronomical studies are available. Star-forming regions distinguish themselves from other regions in the Galaxy. Many different physical processes are displayed with high levels of variability, a large
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Satisfactory assessments of star forming regions in the Galaxy are essential for the understanding of early stellar evolution and today a vast amout of astronomical studies are available. Star-forming regions distinguish themselves from other regions in the Galaxy. Many different physical processes are displayed with high levels of variability, a large
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Carbon Dioxide in Star-forming Regions
The Astrophysical Journal, 2000We consider the gas-phase chemistry of CO2 molecules in active regions. We show that CO2 molecules evaporated from dust in hot cores cannot be efficiently destroyed and are in fact copiously produced in cooler gas. When CO2-rich ices are sputtered in strong MHD shock waves, the increase in atomic hydrogen, due to H2 dissociation by ion-neutral ...
Michael J. Kaufman +3 more
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Masers in Star-Forming Regions [PDF]
, 1999 The subject of astronomical masers is now more than forty years old, and as a consequence, several good reviews have appeared in print. For the readers who want to enter the subject of astronomical masers in a serious way, we want to recommend two reviews (Elitzur 1982; Reid and Moran 1988) and a book (Elitzur 1992a).
N. D. Kylafis, K. G. Pavlakis
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Acetaldehyde in star-forming regions
Advances in Space Research, 2004Abstract Observations of acetaldehyde (CH 3 CHO) in a survey of nine star-forming regions are presented. Emission is clearly detected from both the A and E symmetry states in the 4 04 –3 03 and 5 05 –4 04 transitions. Both the range of the measured CH 3 CHO column densities (∼4×10 12 –10 14 cm −2 ), and the derived fractional abundances, are in ...
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The star-forming region in Orion KL
Astronomy Letters, 2003We have studied the fine structure of the active H2O supermaser emission region in Orion KL with an angular resoln. of 0.1 mas. We found central features suggestive of a bipolar outflow, bullets, and an envelope which correspond to the earliest stage of low-mass star formation.
Matveyenko, L. I. +3 more
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Magnetic massive stars in star forming regions
Proceedings of the International Astronomical Union, 2018AbstractOne idea for the origin of magnetic fields in massive stars suggests that the magnetic field is the fossil remnant of the Galactic ISM magnetic field, amplified during the collapse of the magnetised gas cloud. A search for the presence of magnetic fields in massive stars located in active sites of star formation led to the detection of rather ...
Markus Schöller +2 more
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Kinematics of Star-Forming Regions
2015The previous chapters on star-forming regions have focussed on the spatial distributions of gas and stars. This chapter therefore focusses on the internal kinematics of the young stars within the star-forming regions. Our discussion covers the kinematics of objects in OB associations and young star clusters as well as star-forming regions, detailing ...
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Molecular shocks in star forming regions
Astrophysics and Space Science, 1995The role of excited molecular hydrogen as a powerful observational tool is examined in the context of shock phenomena in molecular clouds, particularly in star forming regions. Conclusions that may be drawn from line intensities and line profiles, and the properties of J and C shocks in a bow shock structure are discussed.
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