| NSF Org: |
AST Division Of Astronomical Sciences |
| Recipient: |
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| Initial Amendment Date: | February 4, 1991 |
| Latest Amendment Date: | January 15, 1993 |
| Award Number: | 9008166 |
| Award Instrument: | Continuing Grant |
| Program Manager: |
Edward G. Schmidt
AST Division Of Astronomical Sciences MPS Directorate for Mathematical and Physical Sciences |
| Start Date: | March 1, 1991 |
| End Date: | August 31, 1994 (Estimated) |
| Total Intended Award Amount: | $177,000.00 |
| Total Awarded Amount to Date: | $177,000.00 |
| Funds Obligated to Date: |
FY 1992 = $59,000.00 FY 1993 = $59,000.00 |
| History of Investigator: |
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| Recipient Sponsored Research Office: |
202 HIMES HALL BATON ROUGE LA US 70803-0001 (225)578-2760 |
| Sponsor Congressional District: |
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| Primary Place of Performance: |
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| Primary Place of
Performance Congressional District: |
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| Unique Entity Identifier (UEI): |
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| Parent UEI: |
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| NSF Program(s): | STELLAR ASTRONOMY & ASTROPHYSC |
| Primary Program Source: |
app-0193 |
| Program Reference Code(s): | |
| Program Element Code(s): |
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| Award Agency Code: | 4900 |
| Fund Agency Code: | 4900 |
| Assistance Listing Number(s): | 47.049 |
ABSTRACT
A major topic of study in astronomy concerns the way in which stars are formed from the gravitational collapse of interstellar gas clouds. The Principal Investigator (PI) wishes to extend earlier studies supported by the NSF of numerical simulations of proto- star under the mutual influence of gravity and rotation. The PI will use sophisticated new numerical techniques to compute models in two and three dimensions. Models will be computed to "follow" this collapse in time, with particular attention to the development of minor density fluctuations which could grow ultimately into planets or a secondary star. NSF support will include the purchase of a computer workstation so that movies of simulated collapses can be followed in "real time" over a wide range of test conditions. These results are expected to increase our understanding of how proto-stars lose angular momentum during their collapse and to define the conditions leading to the formation of two separate "binary" stars.
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