A theoretical systematic study of nova light curves
| Project/Area Number |
22540254
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| Research Category |
Grant-in-Aid for Scientific Research (C)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
Astronomy
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| Research Institution | Keio University |
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Principal Investigator |
KATO Mariko 慶應義塾大学, 理工学部, 教授 (50185873)
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| Project Period (FY) |
2010-04-01 – 2015-03-31
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| Project Status |
Completed (Fiscal Year 2014)
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| Budget Amount *help |
¥4,290,000 (Direct Cost: ¥3,300,000、Indirect Cost: ¥990,000)
Fiscal Year 2014: ¥650,000 (Direct Cost: ¥500,000、Indirect Cost: ¥150,000)
Fiscal Year 2013: ¥780,000 (Direct Cost: ¥600,000、Indirect Cost: ¥180,000)
Fiscal Year 2012: ¥780,000 (Direct Cost: ¥600,000、Indirect Cost: ¥180,000)
Fiscal Year 2011: ¥780,000 (Direct Cost: ¥600,000、Indirect Cost: ¥180,000)
Fiscal Year 2010: ¥1,300,000 (Direct Cost: ¥1,000,000、Indirect Cost: ¥300,000)
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| Keywords | 新星 / 白色矮星 / 連星系 / 理論天文学 / 星の種族 / 天体物理学 |
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| Outline of Final Research Achievements |
We found that, for less massive white dwarfs (WDs), the opticaly thick wind does not occur throughout the outburst or if it does it begins after a delay time for a transition. We also found the general evolution course in the color-color diagram (nova-giant sequence) that is common for various types of nova. This property is useful to estimate the interstellar extinction and distance. In the light curve analysis of slow novae, the contribution of photospheric emission cannot be neglected, whereas in the fast novae the free-free emission dominates. Novae in globular clusters may contain only massive WDs because of weak acceleration of the winds. We also calculated binary evolution including super-Chandrasekhar WD mass.
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Report
(6 results)
Research Products
(25 results)
