Electromagnetic bursting of a rapidly rotating magnetized neutron star in a close binary system

1995 ◽  
Vol 231 (1-2) ◽  
pp. 437-440
Author(s):  
A. Treves ◽  
E. Szuszkiewicz ◽  
M. Tavani
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Close Binary System ◽  
Close Binary

On the formation of a neutron star in a close binary system

1971 ◽  
Vol 10 (3) ◽  
pp. 464-470 ◽  
Author(s):  
George E. McCluskey ◽  
Yoji Kondo
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Close Binary System ◽  
Close Binary

scholarly journals Origin of High Velocity Pulsar and Soft Gamma Ray Repeaters

1996 ◽  
Vol 160 ◽  
pp. 359-360
Author(s):  
Hitoshi Hanami
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
High Velocity ◽  
Relative Velocity ◽  
Gamma Ray ◽  
Center Of Mass ◽  
Supernova Explosion ◽  
Close Binary System ◽  
Close Binary ◽  
X Ray

AbstractWe consider a close binary system with separation ≃ 0.2 R⊙which consists of a (C+O) star of mass ≃ 4 M⊙and a neutron star as a progenitor of soft gamma-ray repeater (SGR) and a high velocity pulsar. After the event of the supernova explosion, both new and old neutron stars have high relative velocity of ≃ 1000km s−1to the center of mass of the ejecta. SGR activities can be induced by the episodic accretion of the supernova ejecta onto the old neutron star or the strange high rotating pulsar of the new neutron star. Future observations with fine positional resolution can clarify the position ambiguity between the gamma ray and X-ray sources.

Ariel 1118-61 ? A very close binary system or a slowly rotating neutron star?

1976 ◽  
Vol 42 (1) ◽  
pp. 161-164
Author(s):  
A. C. Fabian ◽  
J. E. Pringle ◽  
R. F. Webbink
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Close Binary System ◽  
Close Binary

scholarly journals Collapse of Accreting White Dwarf to Form a Neutron Star

1979 ◽  
Vol 53 ◽  
pp. 56-60 ◽  
Author(s):  
Ken’ichi Nomoto ◽  
Shigeki Miyaji ◽  
Daiichiro Sugimoto ◽  
Koichi Yokoi
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Mass Exchange ◽  
White Dwarf ◽  
Mass Range ◽  
Close Binary System ◽  
Roche Lobe ◽  
Close Binary ◽  
Primary Star ◽  
Companion Star

AbstractIn a close binary system with a primary star in the mass range 8-12 M⊙, the primary star leaves a white dwarf composed of 16O, 20Ne, and 24Mg as a result of mass exchange. When the companion star, fills its Roche lobe, overflowing matter accretes onto the white dwarf. We have computed the evolution of such an accreting O-Ne-Mg white dwarf and found that electron captures on 24Mg and 20Ne trigger the collapse when the mass reaches 1.38 M⊙. As a result of the collapse, oxygen begins to deflagrate but the effects of electron captures dominate over the oxygen deflagration. The white dwarf collapses to form a neutron star.

scholarly journals Marginally low mass ratio close binary system V1191 Cyg

New Astronomy ◽  
2012 ◽  
Vol 17 (1) ◽  
pp. 46-49 ◽  
Author(s):  
B. Ulaş ◽  
B. Kalomeni ◽  
V. Keskin ◽  
O. Köse ◽  
K. Yakut
Keyword(s):  
Binary System ◽  
Close Binary System ◽  
Close Binary ◽  
Mass Ratio ◽  
Low Mass ◽  
Low Mass Ratio

scholarly journals Asteroseismology in action: a test of spin-orbit synchronism in the close binary system Feige 48

2008 ◽  
Vol 483 (3) ◽  
pp. 875-885 ◽  
Author(s):  
V. Van Grootel ◽  
S. Charpinet ◽  
G. Fontaine ◽  
P. Brassard
Keyword(s):  
Binary System ◽  
Close Binary System ◽  
Close Binary ◽  
Spin Orbit
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