scholarly journals Population synthesis of accreting white dwarfs: Rates and evolutionary pathways of H and He novae

2021 ◽  
Author(s):  
Alex J Kemp ◽  
Amanda I Karakas ◽  
Andrew R Casey ◽  
Robert G Izzard ◽  
Ashley J Ruiter ◽  
...  
Keyword(s):  
White Dwarfs ◽  
Binary Systems ◽  
Physical Parameters ◽  
Population Synthesis ◽  
Common Envelope ◽  
Evolutionary Pathways ◽  
Binary Evolution ◽  
Observational Estimate ◽  
Almost All ◽  
Event Rates

Abstract Novae are some of the most commonly detected optical transients and have the potential to provide valuable information about binary evolution. Binary population synthesis codes have emerged as the most effective tool for modelling populations of binary systems, but such codes have traditionally employed greatly simplified nova physics, precluding detailed study. In this work, we implement a model treating H and He novae as individual events into the binary population synthesis code binary_c. This treatment of novae represents a significant improvement on the ‘averaging’ treatment currently employed in modern population synthesis codes. We discuss the evolutionary pathways leading to these phenomena and present nova event rates and distributions of several important physical parameters. Most novae are produced on massive white dwarfs, with approximately 70 and 55 per cent of nova events occurring on O/Ne white dwarfs for H and He novae respectively. Only 15 per cent of H-nova systems undergo a common-envelope phase, but these systems are responsible for the majority of H nova events. All He-accreting He-nova systems are considered post-common-envelope systems, and almost all will merge with their donor star in a gravitational-wave driven inspiral. We estimate the current annual rate of novae in M31 (Andromeda) to be approximately 41 ± 4 for H novae, underpredicting the current observational estimate of $65^{+15}_{-16}$, and 0.14 ± 0.015 for He novae. When varying common-envelope parameters, the H nova rate varies between 20 and 80 events per year.

scholarly journals A closer look at non-interacting He stars as a channel for producing the old population of type Ia supernovae

2020 ◽  
Vol 641 ◽  
pp. A20
Author(s):  
Zhengwei Liu ◽  
Richard J. Stancliffe
Keyword(s):  
Binary Systems ◽  
Type Ia Supernovae ◽  
Population Synthesis ◽  
Thermonuclear Explosion ◽  
Delay Times ◽  
Type Ia ◽  
Binary Evolution ◽  
Chandrasekhar Limit ◽  
Ia Supernovae ◽  
Almost All

The nature of the progenitors of type Ia supernovae (SNe Ia) remains a mystery. Binary systems consisting of a white dwarf (WD) and a main-sequence (MS) donor are potential progenitors of SNe Ia, in which a thermonuclear explosion of the WD may occur when its mass reaches the Chandrasekhar limit during accretion of material from a companion star. In the present work, we address theoretical rates and delay times of a specific MS donor channel to SNe Ia, in which a helium (He) star + MS binary produced from a common envelope event subsequently forms a WD + MS system without the He star undergoing mass transfer by Roche lobe overflow. By combining the results of self-consistent binary evolution calculations with population synthesis models, we find that the contribution of SNe Ia in this channel is around 2.0 × 10−4 yr−1. In addition, we find that delay times of SNe Ia in this channel cover a range of about 1.0–2.6 Gyr, and almost all SNe Ia produced in this way (about 97%) have a delay time of ≳1 Gyr. While the rate of SN Ia in this work is about 10% of the overall SN Ia rate, the channel represents a possible contribution to the old population (1–3 Gyr) of observed SNe Ia.

scholarly journals Type IIb supernovae by the grazing envelope evolution

2019 ◽  
Author(s):  
Binyamin V Naiman ◽  
Efrat Sabach ◽  
Avishai Gilkis ◽  
Noam Soker
Keyword(s):  
Mass Loss ◽  
Binary Systems ◽  
The Other ◽  
Primary Star ◽  
Single Star ◽  
Common Envelope ◽  
Secondary Star ◽  
The Core ◽  
Free Parameters ◽  
Binary Evolution

Abstract We simulate the evolution of binary systems with a massive primary star of 15M⊙ where we introduce an enhanced mass loss due to jets that the secondary star might launch, and find that in many cases the enhanced mass loss brings the binary system to experience the grazing envelope evolution (GEE) and form a progenitor of Type IIb supernova (SN IIb). The jets, the Roche lobe overflow (RLOF), and a final stellar wind remove most of the hydrogen-rich envelope, leaving a blue-compact SN IIb progenitor. In many cases without this jet-driven mass loss the system enters a common envelope evolution (CEE) and does not form a SN IIb progenitor. We use the stellar evolutionary code MESA binary and mimic the jet-driven mass loss with a simple prescription and some free parameters. Our results show that the jet-driven mass loss, that some systems have during the GEE, increases the parameter space for stellar binary systems to form SN IIb progenitors. We estimate that the binary evolution channel with GEE contributes about a quarter of all SNe IIb, about equal to the contribution of each of the other three channels, binary evolution without a GEE, fatal CEE (where the secondary star merges with the core of the giant primary star), and the single star channel.

scholarly journals Population Synthesis of Type Ia SNe: Constraining Free Parameters from Observations

2011 ◽  
Vol 7 (S281) ◽  
pp. 240-243
Author(s):  
Maxwell Moe ◽  
Rosanne Di Stefano
Keyword(s):  
Mass Transfer ◽  
First Principles ◽  
Type Ia Supernovae ◽  
Population Synthesis ◽  
Common Envelope ◽  
Tidal Interactions ◽  
Type Ia ◽  
Free Parameters ◽  
Binary Evolution ◽  
Ia Supernovae

AbstractComputing the rate of Type Ia supernovae (SNe Ia) from first principles is difficult because there are large uncertainties regarding several key binary processes such as common envelope evolution, tidal interactions, and the efficiency of mass transfer. Fortunately, a range of observational parameters of binaries in intermediate stages of evolution can help us model these processes in a way that is likely to mirror the true binary evolution. We discuss how this observationally-motivated approach may have the effect of increasing the predicted rate of single degenerate progenitors of SNe Ia, while simultaneously decreasing the number of double degenerate progenitors.

scholarly journals The impact of close binary evolution on the properties of the WR-bump emission lines of Wolf-Rayet galaxies

2003 ◽  
Vol 212 ◽  
pp. 576-577
Author(s):  
Joris Van Bever ◽  
Dany Vanbeveren
Keyword(s):  
Mass Transfer ◽  
Neutron Stars ◽  
Supernova Explosion ◽  
Emission Lines ◽  
Close Binary ◽  
Population Synthesis ◽  
Common Envelope ◽  
Solar Metallicity ◽  
Binary Evolution ◽  
The Impact

We present the results of a study on the behaviour of the blue and red WR emission bumps (around 4650Å and 5808Å) and of the nebular contribution to He ii λ4686 in evolving young starburst regions (such as Wolf-Rayet galaxies), containing a non-negligible binary population. Calculations were made for solar metallicity and 1/20 solar. The population synthesis program uses an extended library of stellar evolutionary tracks of single stars and binaries, computed using the most recent stellar wind mass loss rates during RSG, LBV and WR stages. In the case of binaries, we account in detail for the effects of Roche lobe overflow, mass transfer and mass accretion, common envelope evolution, the spiral-in process, asymmetric kicks to neutron stars as a result of their supernova explosion, etc. This research is part of a more extensive project to explore every possible impact of massive binaries on stellar populations.

scholarly journals The origin of spin in binary black holes

2020 ◽  
Vol 635 ◽  
pp. A97 ◽  
Author(s):  
Simone S. Bavera ◽  
Tassos Fragos ◽  
Ying Qin ◽  
Emmanouil Zapartas ◽  
Coenraad J. Neijssel ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Wave ◽  
Scientific Progress ◽  
Hybrid Technique ◽  
Population Synthesis ◽  
Binary Black Holes ◽  
Common Envelope ◽  
The Common ◽  
Binary Evolution

Context. After years of scientific progress, the origin of stellar binary black holes is still a great mystery. Several formation channels for merging black holes have been proposed in the literature. As more merger detections are expected with future gravitational-wave observations, population synthesis studies can help to distinguish between them. Aims. We study the formation of coalescing binary black holes via the evolution of isolated field binaries that go through the common envelope phase in order to obtain the combined distributions of observables such as black-hole spins, masses and cosmological redshifts of mergers. Methods. To achieve this aim, we used a hybrid technique that combines the parametric binary population synthesis code COMPAS with detailed binary evolution simulations performed with the MESA code. We then convolved our binary evolution calculations with the redshift- and metallicity-dependent star-formation rate and the selection effects of gravitational-wave detectors to obtain predictions of observable properties. Results. By assuming efficient angular momentum transport, we are able to present a model that is capable of simultaneously predicting the following three main gravitational-wave observables: the effective inspiral spin parameter χeff, the chirp mass Mchirp and the cosmological redshift of merger zmerger. We find an excellent agreement between our model and the ten events from the first two advanced detector observing runs. We make predictions for the third observing run O3 and for Advanced LIGO design sensitivity. We expect approximately 80% of events with χeff <  0.1, while the remaining 20% of events with χeff ≥ 0.1 are split into ∼10% with Mchirp <  15 M⊙ and ∼10% with Mchirp ≥ 15 M⊙. Moreover, we find that Mchirp and χeff distributions are very weakly dependent on the detector sensitivity. Conclusions. The favorable comparison of the existing LIGO/Virgo observations with our model predictions gives support to the idea that the majority, if not all of the observed mergers, originate from the evolution of isolated binaries. The first-born black hole has negligible spin because it lost its envelope after it expanded to become a giant star, while the spin of the second-born black hole is determined by the tidal spin up of its naked helium star progenitor by the first-born black hole companion after the binary finished the common-envelope phase.

scholarly journals The Evolutionary Evidence for Most Be Stars Being Paired with Hot White Dwarfs

2000 ◽  
Vol 175 ◽  
pp. 693-696
Author(s):  
Natalya V. Raguzova
Keyword(s):  
Surface Temperature ◽  
Physical Properties ◽  
White Dwarf ◽  
White Dwarfs ◽  
Binary Systems ◽  
Compact Object ◽  
Be Stars ◽  
Be Star ◽  
Binary Evolution

AbstractUsing the “Scenario Machine” we study the number and physical properties of binary Be stars with white dwarfs taking into account cooling of the compact object and discuss the formation of such systems. According to our calculations the number of binary systems containing a Be star paired with a white dwarf in our galaxy is very large − 46% of all Be stars formed as a result of binary evolution must have a white dwarf as companion. These white dwarfs should be very hot with a surface temperature lying in the range from 30,000 to 60,000 K.

scholarly journals Deriving fundamental parameters of millisecond pulsars via AIC in white dwarfs

2012 ◽  
Vol 8 (S290) ◽  
pp. 177-178
Author(s):  
A. Taani ◽  
C. M. Zhang ◽  
Y. H. Zhao ◽  
A. Moraghan
Keyword(s):  
Magnetic Fields ◽  
Neutron Stars ◽  
White Dwarfs ◽  
Binary Systems ◽  
Millisecond Pulsars ◽  
Fundamental Parameters ◽  
Evolutionary Connection ◽  
Binary Evolution

AbstractWe present a study of the observational properties of Millisecond Pulsars (MSPs) by way of their magnetic fields, spin periods and masses. These measurements are derived through the scenario of Accretion Induced Collapse (AIC) of white dwarfs (WDs) in stellar binary systems, in order to provide a greater understanding of the characteristics of MSP populations. In addition, we demonstrate a strong evolutionary connection between neutron stars and WDs with binary companions from a stellar binary evolution perspective via the AIC process.

scholarly journals Astrometric Observations of X-ray Binaries Using Very Long Baseline Interferometry

2014 ◽  
Vol 31 ◽  
Author(s):  
James C. A. Miller-Jones
Keyword(s):  
Proper Motion ◽  
Binary Systems ◽  
Very Long Baseline Interferometry ◽  
Jet Physics ◽  
Physical Parameters ◽  
X Ray ◽  
Long Baseline ◽  
Binary Evolution ◽  
Motion Studies

AbstractI review the astrophysical insights arising from high-precision astrometric observations of X-ray binary systems, focussing primarily (but not exclusively) on recent results with very long baseline interferometry. Accurate, model-independent distances from geometric parallax measurements can help determine physical parameters of the host binary system and constrain black hole spins via broadband X-ray spectral modelling. Long-term proper motion studies, combined with binary evolution calculations, can provide observational constraints on the formation mechanism of black holes. Finally, the astrometric residuals from parallax and proper motion fits can provide information on orbital sizes and jet physics. I end by discussing prospects for future progress in this field.

scholarly journals The connection between merging double compact objects and the Ultraluminous X-ray Sources

2019 ◽  
Author(s):  
Samaresh Mondal ◽  
Krzysztof Belczyński ◽  
Grzegorz Wiktorowicz ◽  
Jean-Pierre Lasota ◽  
Andrew R King
Keyword(s):  
Dynamical Evolution ◽  
Compact Objects ◽  
Population Synthesis ◽  
Local Universe ◽  
X Ray ◽  
Common Envelope ◽  
Envelope Model ◽  
Rate Calculation ◽  
Binary Evolution ◽  
Merger Rate

Abstract We explore the different formation channels of merging double compact objects (DCOs: BH-BH/BH-NS/NS-NS) that went through a ultraluminous X-ray phase (ULX: X-ray sources with apparent luminosity exceeding $10^{39}\rm {\ erg\ s^{-1}}$). There are many evolutionary scenarios which can naturally explain the formation of merging DCO systems: isolated binary evolution, dynamical evolution inside dense clusters and chemically homogeneous evolution of field binaries. It is not clear which scenario is responsible for the majority of LIGO/Virgo sources. Finding connections between ULXs and DCOs can potentially point to the origin of merging DCOs as more and more ULXs are discovered. We use the StarTrack population synthesis code to show how many ULXs will form merging DCOs in the framework of isolated binary evolution. Our merger rate calculation shows that in the local Universe typically $50\%$ of merging BH-BH progenitor binaries have evolved through a ULX phase. This indicates that ULXs can be used to study the origin of LIGO/Virgo sources. We have also estimated that the fraction of observed ULXs that will form merging DCOs in future varies between $5\%$ to $40\%$ depending on common envelope model and metallicity.

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