scholarly journals Simulating the Outcome of a Binary Neutron Star Merger in a Common Envelope Jets Supernova

2021 ◽  
Vol 923 (1) ◽  
pp. 55
Author(s):  
Muhammad Akashi ◽  
Noam Soker
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Three Dimensional ◽  
Dynamical Friction ◽  
Transient Event ◽  
Common Envelope ◽  
Binary Neutron Star ◽  
The Core ◽  
Merger Process ◽  
Triple Star

Abstract We simulate the influence of the energy that the merger process of two neutron stars (NSs) releases inside a red supergiant (RSG) star on the RSG envelope inner to the merger location. In the triple-star common envelope evolution (CEE) that we consider, a tight binary system of two NSs spiraling in inside an RSG envelope and because of mass accretion and dynamical friction, the two NSs merge. We deposit merger-explosion energies of 3 × 1050 and 1051 erg at distances of 25 and 50 R ⊙ from the center of the RSG, and with the three-dimensional hydrodynamical code FLASH we follow the evolution of the RSG envelope in inner regions. For the parameters we explore, we find that more than 90% of the RSG envelope mass inward of the merger site stays bound to the RSG. NSs that experience CEE are likely to accrete RSG envelope mass through an accretion disk that launches jets. These jets power a luminous transient event, a common envelope jets supernova (CEJSN). The merger process adds to the CEJSN energy. Our finding implies that the interaction of the merger product, a massive NS or a BH, with the envelope can continue to release more energy, both by further inspiraling and by mass accretion by the merger product. Massive RSG envelopes can force the merger product to spiral into the core of the RSG, leading to an even more energetic CEJSN.

scholarly journals Common envelope binaries and mass loss

1979 ◽  
Vol 83 ◽  
pp. 415-420
Author(s):  
A. Delgado
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Mass Loss ◽  
Free Parameter ◽  
Mass Ratio ◽  
Initial State ◽  
Helium Burning ◽  
Common Envelope ◽  
The Core ◽  
Before And After

In this work we calculate the evolution of a binary system with a common envelope, which consists of a blue supergiant and a neutron star. We consider as a free parameter the effectivity with which the energy liberated at the orbit produces mass loss from the system.The evolutionary calculations were made, using various values of this parameter, for a system with mass ratio 25:1. As initial state we choose a model in the phase of Hydrogen-shell burning, before and after the begin of Helium-burning in the core.We found that, under certain conditions, it is possible for the radius of the orbit and the period of the system to increase; the time scale for the “spiral-in” would be of the order of 104-105 years. Mass loss rates are between 10−3 M⊙/y and 10−4 M⊙/y.

scholarly journals Prospects of joint detections of neutron star mergers and short GRBs with Gaussian structured jets

2020 ◽  
Vol 493 (2) ◽  
pp. 1633-1639
Author(s):  
M Saleem
Keyword(s):  
Neutron Star ◽  
Joint Detection ◽  
Detection Rates ◽  
Binary Neutron Star ◽  
The Core ◽  
Relativistic Jet ◽  
Inclination Angles ◽  
Γ Ray ◽  
Short Grbs ◽  
Lower Inclination

ABSTRACT GW170817 was the first ever joint detection of gravitational waves (GW) from a binary neutron star (BNS) merger with the detections of short γ-ray burst (SGRB) counterparts. Analysis of the multiband afterglow observations of over more than a year revealed that the outflow from the merger end product was consistent with structured relativistic jet models with the core of the jet narrowly collimated to half-opening angles ∼5○. In this work, assuming that all the BNS mergers produce Gaussian structured jets with properties as inferred for GW170817, we explore the prospects of joint detections of BNS mergers and prompt γ-ray emission, expected during the current and upcoming upgrades of LIGO–Virgo–KAGRA detectors. We discuss three specific observational aspects: 1) the distribution of detected binary inclination angles, 2) the distance reach, and 3) the detection rates. Unlike GW-only detections, the joint detections are greatly restricted at large inclination angles, due to the structure of the jets. We find that at lower inclination angles (say below 20○), the distance reach as well as the detection rates of the joint detections are limited by GW detectability while at larger inclinations (say above 20○), they are limited by the γ-ray detectability.

scholarly journals CLOSE BINARY PROGENITORS OF HYPERNOVAE

2012 ◽  
Vol 08 ◽  
pp. 209-219 ◽  
Author(s):  
MAXIM V. BARKOV
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
Neutron Star ◽  
Binary Systems ◽  
Close Binary ◽  
Transient Event ◽  
Common Envelope ◽  
Starting Point ◽  
The Common ◽  
Rayet Star

In this paper we propose a new plausible mechanism of supernova explosions specific to close binary systems. The starting point is the common envelope phase in the evolution of a binary consisting of a red super giant and a neutron star. As the neutron star spirals towards the center of its companion it spins up via disk accretion. Depending on the specific angular momentum of gas captured by the neutron star via the Bondi-Hoyle mechanism, it may reach millisecond periods either when it is still inside the common envelope or after it has merged with the companion core. The high accretion rate may result in strong differential rotation of the neutron star and generation of a magnetar-strength magnetic field. The magnetar wind can blow away the common envelope if its magnetic field is as strong as 1015 G, and can destroy the entire companion if it is as strong as 1016 G. The total explosion energy can be comparable to the rotational energy of a millisecond pulsar and reach 1052 erg. The result is an unusual type-II supernova with very high luminosity during the plateau phase, followed by a sharp drop in brightness and a steep light-curve tail. The remnant is either a solitary magnetar or a close binary involving a Wolf-Rayet star and a magnetar. When this Wolf-Rayet star explodes this will be a third supernovae explosion in the same binary. A particularly interesting version of the binary progenitor involves merger of a red super giant star with an ultra-compact companion, neutron star or black hole. In the case if a strong magnetic field is not generated on the surface of a neutron star then it will collapse to a black hole. After that we expect the formation of a very long-lived accretion disk around the black hole. The Blandford-Znajek driven jet from this black hole may drive not only hypernovae explosion but produce a bright X-ray transient event on a time scale of 104 s.

scholarly journals Common envelope evolution

2011 ◽  
Vol 7 (S283) ◽  
pp. 95-102 ◽  
Author(s):  
Robert G. Izzard ◽  
Philip D. Hall ◽  
Thomas M. Tauris ◽  
Christopher A. Tout
Keyword(s):  
Binary System ◽  
Binary Systems ◽  
Binary Star ◽  
Short Review ◽  
Close Binary System ◽  
Asymptotic Giant Branch ◽  
Close Binary ◽  
Asymptotic Giant Branch Star ◽  
Common Envelope ◽  
The Core

AbstractMany binary star systems are not wide enough to contain the progenitor stars from which they were made. One explanation for this is that when one star becomes a red giant a common envelope forms around both stars in the binary system. The core of the giant and its companion star continue to orbit one another inside the envelope. Frictional energy deposited into the common envelope may lead to its ejection and, if so, a close binary system is formed from the core of the former giant star and its relatively untouched companion. When the primary is an asymptotic giant branch star the core becomes a hot carbon-oxygen white dwarf which may ionise the ejected envelope and illuminate a planetary nebula. Many other types of binary systems form through common envelope evolution such as low-mass X-ray binaries and cataclysmic variables. In the case of a failed envelope ejection when the cores merge, rapidly-rotating solitary giants similar to FK Comae stars form. In this short review we focus on attempts to constrain parameters of common envelope evolution models and also describe the latest efforts to model this elusive phase of binary stellar evolution.

scholarly journals Inclined jets inside a common envelope of a triple stellar system

2019 ◽  
Author(s):  
Ron Schreier ◽  
Shlomi Hillel ◽  
Noam Soker
Keyword(s):  
Binary System ◽  
Stellar System ◽  
Three Dimensional ◽  
Orbital Plane ◽  
Density Fluctuations ◽  
Rare Type ◽  
Giant Star ◽  
Common Envelope ◽  
Hydrodynamical Simulation ◽  
The Many

Abstract We conduct a three-dimensional hydrodynamical simulation to study the interaction of two opposite inclined jets inside the envelope of a giant star, and find that the jets induce many vortexes inside the envelope and that they efficiently remove mass from the envelope and form a very clumpy outflow. We assume that this very rare type of interaction occurs when a tight binary system enters the envelope of a giant star, and that the orbital plane of the tight binary system and that of the triple stellar system are inclined to each other. We further assume that one of the stars of the tight binary system accretes mass and launches two opposite jets and that the jets’ axis is inclined to the angular momentum axis of the triple stellar system. The many vortexes that the jets induce along the orbit of the tight binary system inside the giant envelope might play an important role in the common envelope evolution (CEE) by distributing energy in the envelope. The density fluctuations that accompany the vortexes lead to an outflow with many clumps that might facilitate the formation of dust. This outflow lacks any clear symmetry, and it might account for very rare types of ‘messy’ planetary nebulae and ‘messy’ nebulae around massive stars. On a broader scope, our study adds to the notion that jets can play important roles in the CEE, and that they can form a rich variety of shapes of nebulae around evolved stars.

scholarly journals Common-envelope evolution with an asymptotic giant branch star

2020 ◽  
Vol 644 ◽  
pp. A60
Author(s):  
Christian Sand ◽  
Sebastian T. Ohlmann ◽  
Fabian R. N. Schneider ◽  
Rüdiger Pakmor ◽  
Friedrich K. Röpke
Keyword(s):  
Binary Systems ◽  
Three Dimensional ◽  
Asymptotic Giant Branch ◽  
Orbital Energy ◽  
Primary Star ◽  
Stellar Envelope ◽  
Asymptotic Giant Branch Star ◽  
Common Envelope ◽  
The Core ◽  
Red Giant

Common-envelope phases are decisive for the evolution of many binary systems. Cases with asymptotic giant branch (AGB) primary stars are of particular interest because they are thought to be progenitors of various astrophysical transients. In three-dimensional hydrodynamic simulations with the moving-mesh code AREPO, we study the common-envelope evolution of a 1.0 M⊙ early-AGB star with companions of different masses. Although the stellar envelope of an AGB star is less tightly bound than that of a red giant, we find that the release of orbital energy of the core binary is insufficient to eject more than about twenty percent of the envelope mass. Ionization energy that is released in the expanding envelope, however, can lead to complete envelope ejection. Because recombination proceeds largely at high optical depths in our simulations, it is likely that this effect indeed plays a significant role in the considered systems. The efficiency of mass loss and the final orbital separation of the core binary system depend on the mass ratio between the companion and the primary star. Our results suggest a linear relation between the ratio of final to initial orbital separation and this parameter.

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 SUPERNOVA 1987A: CELEBRATING A SILVER JUBILEE

2013 ◽  
Vol 53 (A) ◽  
pp. 606-611
Author(s):  
Nino Panagia
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
Massive Star ◽  
Core Collapse ◽  
Single Star ◽  
The Core ◽  
Sn 1987A ◽  
Supernova 1987A ◽  
Collapse Process

The story of the SN 1987A explosion is briefly reviewed. Although this supernova was somewhat peculiar, the study of SN 1987A has clarified quite a number of important aspects of the nature and the properties of supernovae, such as the confirmation of the core collapse of a massive star as the cause of the explosion, as well the confirmation that the decays 56Ni–56Co–56Fe at early times and 44Ti–44Sc at late times, are the main sources of the energy radiated by the ejecta. Still we have not been able to ascertain whether the progenitor was a single star or a binary system, nor have we been able to detect the stellar remnant, a neutron star that should be produced in the core collapse process.

scholarly journals From SN 2010da to NGC 300 ULX-1: Ten Years of Observations of an Unusual High Mass X-Ray Binary in NGC 300

Galaxies ◽  
2020 ◽  
Vol 8 (1) ◽  
pp. 17
Author(s):  
Breanna A. Binder ◽  
Stefania Carpano ◽  
Marianne Heida ◽  
Ryan Lau
Keyword(s):  
Neutron Star ◽  
Binary System ◽  
South African ◽  
High Mass ◽  
Nearby Galaxy ◽  
Transient Event ◽  
X Ray ◽  
Amateur Astronomer ◽  
Multi Wavelength ◽  
Optical Transient

In May 2010, an intermediate luminosity optical transient was discovered in the nearby galaxy NGC 300 by a South African amateur astronomer. In the decade since its discovery, multi-wavelength observations of the misnamed “SN 2010da” have continually reshaped our understanding of this high mass X-ray binary system. In this review, we present an overview of the multi-wavelength observations and attempt to understand the 2010 transient event, and later, the reclassification of this system as NGC 300 ULX-1: a red supergiant + neutron star ultraluminous X-ray source.

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