| Project/Area Number |
09640325
|
|---|
| Research Category |
Grant-in-Aid for Scientific Research (C)
|
| Allocation Type | Single-year Grants |
|---|
| Section | 一般 |
|---|
| Research Field |
Astronomy
|
|---|
| Research Institution | Keio University |
|---|
Principal Investigator |
KATO Mariko Keio University, Faculty of Science, Associate Prof., 理工学部, 助教授 (50185873)
|
|---|
| Project Period (FY) |
1997 – 2000
|
| Project Status |
Completed (Fiscal Year 2000)
|
| Budget Amount *help |
¥2,400,000 (Direct Cost: ¥2,400,000)
Fiscal Year 2000: ¥600,000 (Direct Cost: ¥600,000)
Fiscal Year 1999: ¥500,000 (Direct Cost: ¥500,000)
Fiscal Year 1998: ¥500,000 (Direct Cost: ¥500,000)
Fiscal Year 1997: ¥800,000 (Direct Cost: ¥800,000)
|
|---|
| Keywords | stellar mass-loss / white dwarfs / binary system / nova / supernova |
|---|
| Research Abstract |
The main results of this research is summarized as follows :
1. Light curve analysis of novae
I established light curve analysis of classical nova using optically thick wind theory. This is a new method to determine the white dwarf mass of binaries.
2. Progenitor of Type Ia Supernovae
The optically thick wind governs the binary evolution, because the wind carries away the angular momentum and the mass from the system. We include this effects of the wind into the binary evolution and found two new ways to type Ia supernova progenitor : Super-soft X-ray channel and the Symbiotic channel.
3. Relation between Recurrent Novae and Type Ia Supernova
Detailed light curve analysis of nine recurrent novae, we find that most of the recurrent nova is in the stage just before the type Ia supernova explosion.
4. Structure of Very Massive Main-Sequence
Very massive stars have a core-halo structure even in the main-sequence stage due to the iron peak in the opacity. The photospheric temperature decreases as the stellar mass increases, which is consistent with observational properties.
|
