| Project/Area Number |
05640314
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| Research Category |
Grant-in-Aid for General Scientific Research (C)
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| Allocation Type | Single-year Grants |
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| Research Field |
Astronomy
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| Research Institution | Keio University |
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Principal Investigator |
KATO Mariko Dept of Astronomy, Keio University Associate Prof., 理工学部, 助教授 (50185873)
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| Project Period (FY) |
1993 – 1995
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| Project Status |
Completed (Fiscal Year 1995)
|
| Budget Amount *help |
¥2,100,000 (Direct Cost: ¥2,100,000)
Fiscal Year 1995: ¥600,000 (Direct Cost: ¥600,000)
Fiscal Year 1994: ¥700,000 (Direct Cost: ¥700,000)
Fiscal Year 1993: ¥800,000 (Direct Cost: ¥800,000)
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| Keywords | Nova / Stellar interior / Stellar wind |
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| Research Abstract |
Nova occurs in a close binary system which contain a white dwarf. Nova outburst is triggered by a thermonuclear shell flash on the white dwarf. What determins the speed class of novae has been a longstanding problem. I have answered this problem by making teoretical light curves with wide range of parameters : With the new opacity, optically thick wind theory gives theoretical light curves of novae with high quality that we can compare with the observational data in detail.
This light curve analysis is applicable to wide range of nova parameters. The optically thick wind mass loss seriously affects scenarios of binary evolution.
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