MADEI PEMBENTUKAN PSR J1141-6545
<p>Abstract:<p align="justify"> <br /> WE investigate the candidates of PSR J1141-6545 system. The optical companion is probably a white dwarf which formed prior to the birth of the pulsar. The required mass of primary star to produce a white dwarf should be 6 M® I 8 Mo...
Saved in:
| Main Author: | |
|---|---|
| Format: | Theses |
| Language: | Indonesia |
| Online Access: | https://digilib.itb.ac.id/gdl/view/5296 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| Institution: | Institut Teknologi Bandung |
| Language: | Indonesia |
| id |
id-itb.:5296 |
|---|---|
| spelling |
id-itb.:52962006-02-16T15:18:05ZMADEI PEMBENTUKAN PSR J1141-6545 Irfan Hakim, Muhamad Indonesia Theses INSTITUT TEKNOLOGI BANDUNG https://digilib.itb.ac.id/gdl/view/5296 <p>Abstract:<p align="justify"> <br /> WE investigate the candidates of PSR J1141-6545 system. The optical companion is probably a white dwarf which formed prior to the birth of the pulsar. The required mass of primary star to produce a white dwarf should be 6 M® I 8 Mo. It has to transfer sufficiently mass to the secondary (which is initially lighter than the primary, q = M4°)/4i°) 1) in order for the latter to explode in a supernova. Before supernova, the secondary evolve through a common envelope (because q become more than 2.5) producing a helium star.<p align="justify"> <br /> We also discuss the constraint for the initial orbital period, cases of mass transfer, and efficiency factor (i) for common envelope evolution. text |
| institution |
Institut Teknologi Bandung |
| building |
Institut Teknologi Bandung Library |
| continent |
Asia |
| country |
Indonesia Indonesia |
| content_provider |
Institut Teknologi Bandung |
| collection |
Digital ITB |
| language |
Indonesia |
| description |
<p>Abstract:<p align="justify"> <br />
WE investigate the candidates of PSR J1141-6545 system. The optical companion is probably a white dwarf which formed prior to the birth of the pulsar. The required mass of primary star to produce a white dwarf should be 6 M® I 8 Mo. It has to transfer sufficiently mass to the secondary (which is initially lighter than the primary, q = M4°)/4i°) 1) in order for the latter to explode in a supernova. Before supernova, the secondary evolve through a common envelope (because q become more than 2.5) producing a helium star.<p align="justify"> <br />
We also discuss the constraint for the initial orbital period, cases of mass transfer, and efficiency factor (i) for common envelope evolution. |
| format |
Theses |
| author |
Irfan Hakim, Muhamad |
| spellingShingle |
Irfan Hakim, Muhamad MADEI PEMBENTUKAN PSR J1141-6545 |
| author_facet |
Irfan Hakim, Muhamad |
| author_sort |
Irfan Hakim, Muhamad |
| title |
MADEI PEMBENTUKAN PSR J1141-6545 |
| title_short |
MADEI PEMBENTUKAN PSR J1141-6545 |
| title_full |
MADEI PEMBENTUKAN PSR J1141-6545 |
| title_fullStr |
MADEI PEMBENTUKAN PSR J1141-6545 |
| title_full_unstemmed |
MADEI PEMBENTUKAN PSR J1141-6545 |
| title_sort |
madei pembentukan psr j1141-6545 |
| url |
https://digilib.itb.ac.id/gdl/view/5296 |
| _version_ |
1820663645850304512 |