• 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.

• 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.

• The star birth process is “publicly” available, moreover the contemporary sciencecould give numbers forthe “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 sciencecould give numbers forthe “teenager” mass, expected lifespan etc. with impressive precision.

• But the star development process is still covered (literally) by the dark clouds.

• 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.

• 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.

• 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.

jacc

accacc jR

iRiP

)(

)()(

ajji mEh

aP 2

2exp0,

lil

ijijR

• 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

• 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”.

• 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.

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

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

• 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.