Possibility Of Condensation Of Glycine Near The Surface Of Comet 67P/Churyumov-Gerasimenko. (arXiv:1901.05170v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Suzuki_T/0/1/0/all/0/1">Taiki Suzuki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shinnaka_Y/0/1/0/all/0/1">Yoshiharu Shinnaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shibata_T/0/1/0/all/0/1">Takashi Shibata</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shibaike_Y/0/1/0/all/0/1">Yuhito Shibaike</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Majumdar_L/0/1/0/all/0/1">Liton Majumdar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nomura_H/0/1/0/all/0/1">Hideko Nomura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Minamoto_H/0/1/0/all/0/1">Harumi Minamoto</a>

The cometary materials are thought to be the reservoir of primitive materials
in the solar system. The recent detection of glycine and CH$_3$NH$_2$ by the
ROSINA mass spectrometer in the coma of 67P/Churyumov-Gerasimenko suggests that
amino acids and their precursors have been formed in such an early evolutionary
phase of the Solar System. We use our chemical modeling for low-mass
star-forming regions to investigate if we can explain observed
“Glycine/CH$_3$NH$_2$” ratio. As a result, the predicted molecular ratio of
“CH$_3$NH$_2$/Glycine” during star-formation is less than 10$^{-2}$, while the
ROSINA measurement has shown this value to be unity. With the hypothesis that
glycine is condensed in the cometary surface during the numerous passages of
perihelion after the formation of the Solar System, we develop the numerical
model to discuss this condensation process. Our modeling results suggest that
glycine is highly likely condensed in the cometary surface due to its high
binding energy, and “Glycine/CH$_3$NH$_2$” ratio will be highly enhanced if the
outbursts eject the materials condensed on cometary surface.

The cometary materials are thought to be the reservoir of primitive materials
in the solar system. The recent detection of glycine and CH$_3$NH$_2$ by the
ROSINA mass spectrometer in the coma of 67P/Churyumov-Gerasimenko suggests that
amino acids and their precursors have been formed in such an early evolutionary
phase of the Solar System. We use our chemical modeling for low-mass
star-forming regions to investigate if we can explain observed
“Glycine/CH$_3$NH$_2$” ratio. As a result, the predicted molecular ratio of
“CH$_3$NH$_2$/Glycine” during star-formation is less than 10$^{-2}$, while the
ROSINA measurement has shown this value to be unity. With the hypothesis that
glycine is condensed in the cometary surface during the numerous passages of
perihelion after the formation of the Solar System, we develop the numerical
model to discuss this condensation process. Our modeling results suggest that
glycine is highly likely condensed in the cometary surface due to its high
binding energy, and “Glycine/CH$_3$NH$_2$” ratio will be highly enhanced if the
outbursts eject the materials condensed on cometary surface.

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