The Heating Mechanisms of Molecular Clouds in the Galactic Center Region

Details The Heating Mechanisms of Molecular Clouds in the Galactic Center Region The Heating Mechanisms of Molecular Clouds in the Galactic Center Region

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006rmxac..26r.165r&link_type=abstract

XI IAU Regional Latin American Meeting of Astronomy (Eds. L. Infante & M. Rubio) Revista Mexicana de Astronomía y Astrofísica (S

Astronomy and Astrophysics

Astronomy

Scientific paper

The molecular gas in the galactic center is exceptionally warm (˜150 K), but without associated warm dust, since the dust temperature is not higher than 40 K. So the obvious question is: What process heat this gas? The two most likely mechanisms are: cloud-cloud collision and ion-slip heating. These processes can be related to observations, since cloud-cloud collision will destroy dust grains and set silicon free into the gas phase. The ion-slip heating mechanism is referred to the friction between ions and neutrals, where the ionics motions are controlled by magnetic fields while that of the neutrals by gravity. We can use different molecules to evaluate the effectiveness of these heating mechanisms. We have observations for the galactic center region in HCO^+ (J=1-0, 89.188518 GHz), SiO (J=2-1, 86.846998 GHz) and in the optically thin Formyl ion isotopomer H^{13}CO^+ (J=1-0, 86.754294 GHz) which falls within the SiO spectrometer range, using the NANTEN 4-m telescope from Nagoya University, operating at Las Campanas Observatory from 1999 until 2003. The area observed covered from l=354.25 to l=5.625 and from b=-0.6874 to b=1.3542. The presence of a large amount of SiO indicates prevalence of cloud-cloud collision, while that of the Formyl ion favors the ion-slip heating. The data are presented in latitude-longitude spatial map and L-V diagrams. In order to compare the species we present spatial plots of T(SiO)-T(HCO^+) and T(SiO)-T(H^{13}CO^+) and L-V diagrams of SiO-HCO^+ and SiO-H^{13}CO^+, that allowed us to identify regions where the HCO^+ dominates and where SiO dominates, distinguishing between heating mechanisms of the galactic center molecular gas.

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