What Molecular Lines can Tell about Early Stages of Massive Stars

Details What Molecular Lines can Tell about Early Stages of Massive Stars What Molecular Lines can Tell about Early Stages of Massive Stars

Jun 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011mss..confetf08v&link_type=abstract

"International Symposium On Molecular Spectroscopy, 66th Meeting, Held 20-24 June, 2011 at Ohio State University. http://molspec

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Astronomical Species And Processes

Scientific paper

Here we present our molecular line investigation of the southern infrared dark clouds (IRDCs). We performed observations of 13 molecular species using the 22-m Mopra radio telescope. In our survey we included in general species which are good tracers of cold and dense gas. Some of them trace the more quiescent gas (e.g. HNC, N_2H^+), while others are sensitive to more dynamical processes (HCN, HCO^+). We detect SiO emission in some clouds and complicated shapes of the HCO^+ emission line profile in all IRDCs, which indicates infall and outflow motions and the beginning of star-formation activity, at least in some parts of the IRDCs. Using H_2 column densities from our previous investigation, we estimated molecular abundances for all species. We uncovered a tendency for IRDCs to have molecular abundances similar to those in low-mass pre-stellar cores. This similarity may indicate similar chemical composition at the earliest stages of low- and high-mass stars and their close evolutionary status. However, for the N_2H^+ and HCO^+ species, there is a tendency for higher mean abundances in IRDCs compared with low- mass cores. To find a reason of such behavior, we use chemical models including gas-phase reactions and accretion and desorption onto/from grains. Chemical modeling allows us to study chemical evolution at the early stages of massive stars in more detail and reconstruct the physical conditions and evolutionary status of IRDCs.

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