A solid state physics approach to the interaction between organic molecules and interstellar dust grains: (C60) on SiC

Details A solid state physics approach to the interaction between organic molecules and interstellar dust grains: (C60) on SiC A solid state physics approach to the interaction between organic molecules and interstellar dust grains: (C60) on SiC

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.256m&link_type=abstract

The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole

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We have modeled the interaction of large organic molecules and dust grains in the interstellar medium by means of conventional surface science techniques such as scanning probe microscopes (SPM) and X-ray photoelectron spectroscopy (XPS) among others. With these surface analysis techniques, no frequently used in astrochemistry, we can recreate model systems where the interstellar environment, in a wide range of conditions of pressure and temperature, can be studied. The accurate control of the species that can be studied enables us to simulate in our laboratory the reactions of important molecules on the surface of dust grains. These new kind of experiments provide new information about the chemical mechanisms of the interaction between dust grains and organic molecules which can be compared with the models and the observations.
We use a state of the art ultra high vacuum chamber (UHV) with base pressure of 1× 10-10 mbar (2× 106 ppcm^3) where we can prepare macroscopic single-crystal samples simulating a particular dust grain surface. The clean surfaces are exposed to different molecules. The complete system molecule-substrate can be characterized down to the Armstrong scale with the scanning tunneling microscope (STM) and even single molecule orbitals can be resolved. The combination of this technique with diffraction and spectroscopic tools allows us to fully understand the adsorption configuration and chemistry of a particular molecular species on a modeled dust grain surface. Here we present, as a proof-of-concept, the study of a broadly studied molecule, fullerene, (C60) on a silicon carbide (SiC) surface. The stellar winds of carbon-rich red-giants are rich in SiC grains in the inner hot (1500K) shell. These grains can then be covered with C_2 H_2, C H_4 and other hydrocarbons that could lead to complex organic molecules, even PAHs, when they move apart from the star. In the present study we simulate the reaction of C60 molecules with the Si rich (3x3) 6H α-SiC(0001). Although 6H α-SiC is not one of the most common polytypes of SiC in the interstellar atmospheres (mostly abundant in 2H α-SiC and 3C β-SiC) we will use these first results to compare with our on-going measurements on 3C β-SiC.

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