Hostname: page-component-8448b6f56d-c4f8m Total loading time: 0 Render date: 2024-04-18T17:47:34.155Z Has data issue: false hasContentIssue false
  • English
  • Français

Interaction between gas and ice phase in the three periods of the solar nebula

Published online by Cambridge University Press:  06 April 2010

Carmen Tornow ,
Ekkehard Kührt ,
Stefan Kupper  and
Uwe Motschmann
Carmen Tornow
Affiliation:
Inst. of Planetary Research, Rutherfordstr. 2, D-12489 Berlin, Germany email: carmen.tornow@dlr.de, ekkehard.kuehrt@dlr.de, and stefan.kupper@dlr.de
Ekkehard Kührt
Affiliation:
Inst. of Planetary Research, Rutherfordstr. 2, D-12489 Berlin, Germany email: carmen.tornow@dlr.de, ekkehard.kuehrt@dlr.de, and stefan.kupper@dlr.de
Stefan Kupper
Affiliation:
Inst. of Planetary Research, Rutherfordstr. 2, D-12489 Berlin, Germany email: carmen.tornow@dlr.de, ekkehard.kuehrt@dlr.de, and stefan.kupper@dlr.de
Uwe Motschmann
Affiliation:
Inst. of Theoretical Physics, Technical University Braunschweig, Mendelssohnstr. 3, D-38106 Braunschweig email: u.motschmann@tu-braunschweig.de
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We simulate the chemical processes in the three evolution periods of the solar nebula, which are (i) the quasi-stationary prestellar cloud core, (ii) the gravitationally collapsing protostellar core, and (iii) the evolving gas-dust disk. Our purpose is to identify chemical parameters which reflect special aspects of the interactions between the gas and ice phase in the different periods, e.g. isotopic or molecular ratios. In this study we derive the D/H and 15N/14N ratio of selected compounds as well as the CO2/H2O ratio to measure the fraction of non-polar to polar ice in the grain mantles. The chosen ratios depend on the depletion-enrichment relation between the ice and gas phases driven by the thermal evolution in each period, especially during the collapse. Hence, we have made great efforts in order to derive realistic and compact hydrodynamic models to describe the evolutionary periods of the solar nebula.

Keywords

Astrochemistrystar formationcometshydrodynamicsmolecular processes
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S263: Icy Bodies of the Solar System , August 2009 , pp. 50 - 54
Copyright
Copyright © International Astronomical Union 2010

References

Aikawa, Y., Umebayashi, T., Nakano, T., & Miyama, S. M. 1997, ApJ Letters, 486, L51Google Scholar
Davis, S. S. 2003, ApJ, 592, 1193Google Scholar
Saigo, K., Tomisaka, K., & Matsumoto, T. 2008, ApJ, 674, 997Google Scholar
Stahler, Steven W., Korycansky, D. G., Brothers, M. J., & Touma, J. 1994, ApJ, 431, 341CrossRefGoogle Scholar
Woodall, J., Agndez, M., Markwick-Kemper, A. J., & Millar, T. J. 2005, A&A, 466, 1197Google Scholar