2. http://www.ifa.hawaii.edu/UHNAI/ CASS-2006 (August 2006). The original results and software presented by the author: Jacqueline Keane. IDL implementation is good, but basic single-station license starts from $3000 along with single namespace, arrays limitations, questionable threads and web-interface, certain design limitations. Java chosen as the programming language, R chosen for the plotting and statistical analysis, Tomcat will be used for the web interface. Java/IDL connector exists and model could be coupled. http://www.ifa.hawaii.edu/UHNAI/ CASS-2006 (August 2006). The original results and software presented by the author: Jacqueline Keane. IDL implementation is good, but basic single-station license starts from $3000 along with single namespace, arrays limitations, questionable threads and web-interface, certain design limitations. Java chosen as the programming language, R chosen for the plotting and statistical analysis, Tomcat will be used for the web interface. Java/IDL connector exists and model could be coupled.

3. Scientific: helps to understand Universe and a star evolution process through the computer simulation; the own Solar system evolution. It’s passed through the same process about 4500 millions year ago; the chemistry model helps to understand the origins of life through the origins of water and pre-biotic molecules on the Earth. Personal: capstone project for the MS program; fits my own interest in astrophysics; good software development experience. Scientific: helps to understand Universe and a star evolution process through the computer simulation; the own Solar system evolution. It’s passed through the same process about 4500 millions year ago; the chemistry model helps to understand the origins of life through the origins of water and pre-biotic molecules on the Earth. Personal: capstone project for the MS program; fits my own interest in astrophysics; good software development experience.

4. The star birth process is “publicly” available, moreover the contemporary science could give numbers for the “teenager” mass, expected lifespan etc. with impressive precision. But the star development process is still covered (literally) by the dark clouds. The star birth process is “publicly” available, moreover the contemporary science could give numbers for the “teenager” mass, expected lifespan etc. with impressive precision. But the star development process is still covered (literally) by the dark clouds.

5. The molecular clouds are almost invisible for humans. They were discovered our own Milky Way Galaxy in the mid 1960's. by using radio telescopes. At the millimeter wavelengths many kinds of molecules in space emit radiation. Infrared light from young stars and heated dust, as well as the millimeter and submm radiation from gas molecules, can propagate the full picture of these dusty realms. The molecular clouds are almost invisible for humans. They were discovered our own Milky Way Galaxy in the mid 1960's. by using radio telescopes. At the millimeter wavelengths many kinds of molecules in space emit radiation. Infrared light from young stars and heated dust, as well as the millimeter and submm radiation from gas molecules, can propagate the full picture of these dusty realms.

6. Most of the stars in the Milky Way formed billions of years ago. Several thousands of star-formation regions in the galaxy. One to three new stars each year. Typical molecular cloud in the Milky Way: several million solar masses in cold gas and spans over the space about tens of parsecs across. the average temperatures within these clouds are 10 - 20 degrees above absolute zero. gas is mostly in the form of hydrogen molecules, with trace amounts of more easily detected material such as carbon monoxide (CO). the millimeter-wavelength emission of CO molecules allows mapping and studying of these clouds. Most of the stars in the Milky Way formed billions of years ago. Several thousands of star-formation regions in the galaxy. One to three new stars each year. Typical molecular cloud in the Milky Way: several million solar masses in cold gas and spans over the space about tens of parsecs across. the average temperatures within these clouds are 10 - 20 degrees above absolute zero. gas is mostly in the form of hydrogen molecules, with trace amounts of more easily detected material such as carbon monoxide (CO). the millimeter-wavelength emission of CO molecules allows mapping and studying of these clouds.

8. Simplifying assumptions: –The accretion timescale >> reactions timescale (10E5 >> 10E-3 ~ 10E4) –No desorption of grain mantle species. –Gas species limited to the dominant ones: H, C, CO, O, O2, N and N2. Simplifying assumptions: –The accretion timescale >> reactions timescale (10E5 >> 10E-3 ~ 10E4) –No desorption of grain mantle species. –Gas species limited to the dominant ones: H, C, CO, O, O2, N and N2.

9. Configure Fixture Accretion loop VERY long chemistry loop goto line 3 or 6 results output Configure Fixture Accretion loop VERY long chemistry loop goto line 3 or 6 results output

10. The accretion process: –the sample taken randomly by one-by-one selection from gas phase with the rate proportional to the abundance and the thermal velocity of the specie. The chemistry: –once a specie arrived on the surface it reacts with selected (according to abundance) coreactant or just stays on surface if there is no coreactants available (only H evaporates); –certain chemistry products follow the same pattern; –If the amount of on-surface species exceeds certain threshold some of the species got “buried”. The accretion process: –the sample taken randomly by one-by-one selection from gas phase with the rate proportional to the abundance and the thermal velocity of the specie. The chemistry: –once a specie arrived on the surface it reacts with selected (according to abundance) coreactant or just stays on surface if there is no coreactants available (only H evaporates); –certain chemistry products follow the same pattern; –If the amount of on-surface species exceeds certain threshold some of the species got “buried”.

12. The accretion process: –The cloud itself is not desaturated by accretion process, i.e. it stays constant for the millions of years; –the other factors such as heating, radiation, ionization, gravitation etc. are not taken in account. The chemistry: –as in the accretion process, the outside factors that could change chemistry flow are not counted. The accretion process: –The cloud itself is not desaturated by accretion process, i.e. it stays constant for the millions of years; –the other factors such as heating, radiation, ionization, gravitation etc. are not taken in account. The chemistry: –as in the accretion process, the outside factors that could change chemistry flow are not counted.

13. The disagreement with observations: –certain species abundances are far from observed. The disagreement with observations: –certain species abundances are far from observed.

14. Coupling with the full-scale gas model: –the accretion get adjusted by the outer chemistry model; Meet the Java open source code standards. –architecture, Javadocs; –automatic testing. Web interface (from xml config to plots). Thesis for MS. The Bioastronomy 2007 (San Juan PR), July 2007. Coupling with the full-scale gas model: –the accretion get adjusted by the outer chemistry model; Meet the Java open source code standards. –architecture, Javadocs; –automatic testing. Web interface (from xml config to plots). Thesis for MS. The Bioastronomy 2007 (San Juan PR), July 2007.