TY - JOUR
T1 - A formation scenario for the triple pulsar PSR J0337+1715
T2 - Breaking a binary system inside a common envelope
AU - Sabach, Efrat
AU - Soker, Noam
N1 - Publisher Copyright:
© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Copyright:
Copyright 2015 Elsevier B.V., All rights reserved.
PY - 2015/4/10
Y1 - 2015/4/10
N2 - We propose a scenario for the formation of the pulsar with two white dwarfs (WDs) triple system PSR J0337+1715. In our scenario, a close binary system is tidally and frictionally destroyed inside the envelope of a massive star that later goes through an accretion-induced collapse (AIC) and forms the neutron star (NS). The proposed scenario includes a new ingredient of a binary system that breaks up inside a common envelope. We use the BINARY_C software to calculate the post-break-up evolution of the system, and show that both low-mass stars end as helium WDs. One of the two lower mass stars that ends further out, the tertiary star, transfers mass to the ONeMg WD remnant of the massive star, and triggers the AIC. The inner low-mass main-sequence star evolves later, induces AIC if the tertiary had not done it already, and spins-up the NS to form a millisecond pulsar. This scenario is not extremely sensitive to many of the parameters, such as the eccentricity of the tertiary star and the orbital separation of the secondary star after the low-mass binary system breaks loose inside the envelope, and to the initial masses of these stars. The proposed scenario employs an efficient envelope removal by jets launched by the compact object immersed in the giant envelope, and the newly proposed grazing envelope evolution.
AB - We propose a scenario for the formation of the pulsar with two white dwarfs (WDs) triple system PSR J0337+1715. In our scenario, a close binary system is tidally and frictionally destroyed inside the envelope of a massive star that later goes through an accretion-induced collapse (AIC) and forms the neutron star (NS). The proposed scenario includes a new ingredient of a binary system that breaks up inside a common envelope. We use the BINARY_C software to calculate the post-break-up evolution of the system, and show that both low-mass stars end as helium WDs. One of the two lower mass stars that ends further out, the tertiary star, transfers mass to the ONeMg WD remnant of the massive star, and triggers the AIC. The inner low-mass main-sequence star evolves later, induces AIC if the tertiary had not done it already, and spins-up the NS to form a millisecond pulsar. This scenario is not extremely sensitive to many of the parameters, such as the eccentricity of the tertiary star and the orbital separation of the secondary star after the low-mass binary system breaks loose inside the envelope, and to the initial masses of these stars. The proposed scenario employs an efficient envelope removal by jets launched by the compact object immersed in the giant envelope, and the newly proposed grazing envelope evolution.
KW - Binaries: close
KW - Pulsars: individual: PSR J0337+1715
KW - Stars: mass-loss
KW - Stars: neutron
UR - http://www.scopus.com/inward/record.url?scp=84938151205&partnerID=8YFLogxK
U2 - 10.1093/mnras/stv717
DO - 10.1093/mnras/stv717
M3 - 文章
AN - SCOPUS:84938151205
VL - 450
SP - 1716
EP - 1723
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -