scholarly journals On the origin of GW190425

2020 ◽  
Vol 496 (1) ◽  
pp. L64-L69 ◽  
Author(s):  
Isobel M Romero-Shaw ◽  
Nicholas Farrow ◽  
Simon Stevenson ◽  
Eric Thrane ◽  
Xing-Jiang Zhu
Keyword(s):  
Mass Transfer ◽  
Neutron Star ◽  
Neutron Stars ◽  
Large Mass ◽  
Common Envelope ◽  
Binary Neutron Star ◽  
Unstable Case ◽  
Helium Star ◽  
The Masses ◽  
Short Time

ABSTRACT The LIGO/Virgo collaborations recently announced the detection of a binary neutron star merger, GW190425. The mass of GW190425 is significantly larger than the masses of Galactic double neutron stars known through radio astronomy. We hypothesize that GW190425 formed differently from Galactic double neutron stars, via unstable ‘case BB’ mass transfer. According to this hypothesis, the progenitor of GW190425 was a binary consisting of a neutron star and a ∼4–$5\, {\mathrm{ M}_\odot }$ helium star, which underwent common-envelope evolution. Following the supernova of the helium star, an eccentric double neutron star was formed, which merged in ${\lesssim }10\, {\rm Myr}$. The helium star progenitor may explain the unusually large mass of GW190425, while the short time to merger may explain why similar systems are not observed in radio. To test this hypothesis, we measure the eccentricity of GW190425 using publicly available LIGO/Virgo data. We constrain the eccentricity at $10\, {\rm Hz}$ to be e ≤ 0.007 with $90{{\ \rm per\ cent}}$ confidence. This provides no evidence for or against the unstable mass transfer scenario, because the binary is likely to have circularized to e ≲ 10−4 by the time it was detected. Future detectors will help to reveal the formation channel of mergers similar to GW190425 using eccentricity measurements.

scholarly journals The evolution of close helium star to neutron star binaries

2003 ◽  
Vol 212 ◽  
pp. 410-411
Author(s):  
Jasinta D.M. Dewi ◽  
Onno R. Pols
Keyword(s):  
Mass Transfer ◽  
Neutron Star ◽  
Binary Systems ◽  
High Mass ◽  
Lower Mass ◽  
Common Envelope ◽  
The Core ◽  
Helium Stars ◽  
Star Binary ◽  
Helium Star

We present the evolution of helium stars in binary systems with a 1.4 M⊙ neutron-star companion which will produce double neutron-star binaries, i.e., systems with helium stars more massive than 2.5 M⊙. We found that mass transfer from helium star less massive than ~ 3.3 M⊙ will end up in a common-envelope phase. If the neutron star has enough time to complete the spiral-in before the core of the helium star collapses, the system will become a very tight double neutron-star binary (P ≈ 0d.01). More massive helium stars do not go through a dynamically-unstable mass transfer. The outcome of binaries with helium star in this range of mass is double-neutron star systems with period of 0d.1-1d, suggesting them to be the progenitor of the observed Galactic double neutron-star pulsars B 1913+16 and B 15344+12. Wide DNS pulsars like J 1518+4904 are produced from helium star-neutron star binaries which avoid Roche-lobe overflow. We are also able to distinguish the progenitors of Type Ib supernovae (as the high-mass helium stars or systems in wide orbits) from those of Type Ic supernovae (as the lower-mass helium stars or systems in close orbits).

scholarly journals The Masses of the Neutron Stars in M15C

1996 ◽  
Vol 165 ◽  
pp. 279-285
Author(s):  
W.T.S. Deich ◽  
S.R. Kulkarni
Keyword(s):  
Neutron Star ◽  
Standard Model ◽  
Neutron Stars ◽  
Total Mass ◽  
Star System ◽  
Binary Neutron Star ◽  
The Standard Model ◽  
The Masses

Several years of timing the pulsar in the binary neutron star system M15C have yielded the masses of both stars: the total mass is MT = 2.7121(6) M⊙; the companion mass is mc = 1.36(4) M⊙; and the pulsar mass is mp = 1.35(4) M⊙. We argue that this system is not likely to have formed through accretion-induced collapse (AIC), and that the standard model also has problems in explaining the formation.

scholarly journals The Formation of Massive White Dwarfs in Cataclysmic Binaries

1982 ◽  
Vol 69 ◽  
pp. 447-451
Author(s):  
Wai-Yuen Law ◽  
Hans Ritter
Keyword(s):  
Mass Transfer ◽  
Mass Spectrum ◽  
White Dwarfs ◽  
Common Envelope ◽  
Cataclysmic Binaries ◽  
Low Mass ◽  
Binary Evolution ◽  
Chandrasekhar Limit ◽  
Helium Star ◽  
The Masses

AbstractIn contrast to the mass spectrum of single white dwarfs which has a single narrow peak at ~0.6 M⊙, the observed mass spectrum of white dwarfs of cataclysmic binaries (CB's) shows a rather uniform distribution of the masses in the range ~0.3 M⊙, to ~1.3 M⊙. The formation of CB's with white dwarfs of less than about 0.8 M⊙ can be understood as the result of a binary evolution according to low mass Case B or Case C with a subsequent spiraling-in in a common envelope. On the other hand the formation of massive white dwarfs of M ≲ 1 M⊙, can be explained as the result of a massive Case B mass transfer yielding a helium star which subsequently undergoes a second Case B mass transfer (so called Case BB evolution). The ultimate product of such an evolution is either a CO-white dwarf with a mass up to the Chandrasekhar limit or a neutron star. The formation of CB's via Case BB evolution requires the binary to undergo at least one, most probably two separate phases of spiraling-in in a common envelope.

scholarly journals Remnant massive neutron stars of binary neutron star mergers: Evolution process and gravitational waveform

2013 ◽  
Vol 88 (4) ◽  
Author(s):  
Kenta Hotokezaka ◽  
Kenta Kiuchi ◽  
Koutarou Kyutoku ◽  
Takayuki Muranushi ◽  
Yu-ichiro Sekiguchi ◽  
...  
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Evolution Process ◽  
Binary Neutron Star

scholarly journals The masses of two binary neutron star systems

1993 ◽  
Vol 405 ◽  
pp. L29 ◽  
Author(s):  
S. E. Thorsett ◽  
Z. Arzoumanian ◽  
M. M. McKinnon ◽  
J. H. Taylor
Keyword(s):  
Neutron Star ◽  
Binary Neutron Star ◽  
The Masses

scholarly journals Global simulations of strongly magnetized remnant massive neutron stars formed in binary neutron star mergers

2018 ◽  
Vol 97 (12) ◽  
Author(s):  
Kenta Kiuchi ◽  
Koutarou Kyutoku ◽  
Yuichiro Sekiguchi ◽  
Masaru Shibata
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Binary Neutron Star

scholarly journals SPINAR MODEL FOR BINARY NEUTRON STAR MERGER

2021 ◽  
Vol 53 ◽  
pp. 134-136
Author(s):  
A. R. Chasovnikov ◽  
V. M. Lipunov ◽  
E. S. Gorbovskoy
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Point Of View ◽  
Binary Neutron Star ◽  
Master System ◽  
Robotic Telescopes

We consider the neutron stars mergers from the point of view of the spinar model. We present calculations of the maximum luminosity of merging neutron stars, both total and in optical ranges. The possibility of observing such gamma-ray bursts using the MASTER system of robotic telescopes is also discussed.

scholarly journals On isolated millisecond pulsars formed by the coalescence of neutron stars and massive white dwarfs

2019 ◽  
Vol 36 ◽  
Author(s):  
Shengnan Sun ◽  
Lin Li ◽  
Helei Liu ◽  
Guoliang Lü ◽  
Zhaojun Wang ◽  
...  
Keyword(s):  
Mass Transfer ◽  
Neutron Star ◽  
Neutron Stars ◽  
White Dwarf ◽  
White Dwarfs ◽  
Birth Rate ◽  
Population Synthesis ◽  
Solar Mass ◽  
Millisecond Pulsars ◽  
The Stability

Abstract This paper uses population synthesis to investigate the possible origin of isolated millisecond pulsars as born from the coalescence of a neutron star and a white dwarf. Results show that the galactic birth rate of isolated millisecond pulsars is likely to lie between 5.8×10−5 yr−1 and 2.0×10−4 yr−1, depending on critical variables, such as the stability of mass transfer via the Roche lobe and the value of kick velocity. In addition to this, this paper estimates that the solar mass of isolated millisecond pulsars can range from 1.5 and 2.0 Mʘ, making them more massive than other ‘normal’ pulsars. Finally, the majority of isolated millisecond pulsars in our simulations have spin periods ranging from several to 20 ms, which is consistent with previous observations.

scholarly journals Constraints on Stellar Evolution from Observations of Compact Object Binaries

2004 ◽  
Vol 194 ◽  
pp. 266-266
Author(s):  
T. Bulik ◽  
R. Moderski ◽  
K. Belczyński
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gravitational Waves ◽  
Stellar Evolution ◽  
Compact Object ◽  
Selection Effects ◽  
Common Envelope ◽  
Mass Ratios ◽  
The Masses

The masses of compact object (black hole, neutron star) binaries depend strongly on the parameters describing stellar evolution. Such masses or their functions can be measured using gravitational waves or through microlensing searches. We analyze an example of the varying common envelope efficiency and show the dependence of distributions of the measured chirp masses in gravitational waves mass ratios through microlensing taking into account the relevant selection effects.

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