Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007msl..confe..25j&link_type=abstract
"Molecules in Space and Laboratory, meeting held in Paris, France, May 14-18, 2007. Editors: J.L. Lemaire, F. Combes. ISBN: 9782
Astronomy and Astrophysics
Astrophysics
Observations
Scientific paper
Molecular clouds are places where matter evolves from embryos to star and planetary systems. Molecules that are particularly sensitive to different routes of formations and that may be useful in distinguishing between a variety of environments (van Dishoeck & Blake 1998). Chemistry in the first phase of star formation (the Prestellar Core phase) may affect the chemical composition of the objects that will eventually form the planetary system (Ceccarelli et al. 2006 ). During this time, matter slowly accumulates towards the center. As the density increases, gaseous molecules start to freeze-out into the cold dust grains, forming dirty, H2O- dominated ice mantles. In this time envelope is so thick that the SED is totally dominated by cold outer regions of the envelope (Class 0 sources). Class 0 envelopes consist of two chemically distinct regions: the outer envelopes and the inner regions - hot corinos. In the hot corinos the chemistry is dominated by the evaporation of the mantles, built up during the pre-collapse phase. The mantle components are in the gas phase, they undergo successive reactions leading to the formations of many complex molecules (Ceccarelli et al. 2006). Observations (Huang et al. 2005) show the chemical connection between dark clouds, massive star-forming regions and solar-type hot corinos. Conversely to high mass, low mass protostars are strong X-ray emitters. The understanding of how X-ray can modified (yes or no) the first phase chemistry is a fascinating question. In this work I present ISO and XMM observations of a few pre-stellar cores: LDN1527, B68, L1448.
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