A Comprehensive Study of Close Double White Dwarfs as Gravitational Wave Sources: Evolutionary Channels, Birth Rates, and Physical Properties

Liu, Jinzhong; Han, Zhanwen; Zhang, Fenghui; Zhang, Yu

doi:10.1088/0004-637x/719/2/1546

Cited by 30 publications

(30 citation statements)

References 44 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Once the WDs have exited this phase, the two WDs are driven together via gravitational wave radiation, the signature of which is expected to be a dominant component of the ambient gravitational wave sky (e.g. Lipunov, Postnov & Prokhorov 1987; Hils, Bender & Webbink 1990; Nelemans, Yungelson & Portegies Zwart 2004; Liu et al 2010).…”

Section: Introductionmentioning

confidence: 99%

How the merger of two white dwarfs depends on their mass ratio: orbital stability and detonations at contact

Dan¹,

Rosswog²,

Guillochon³

et al. 2012

Monthly Notices of the Royal Astronomical Society

111

156

View full text Add to dashboard Cite

Despite their unique astrophysical relevance, the outcome of white dwarf binary mergers has so far only been studied for a very restricted number of systems. Here we present the results of a survey with more than 200 simulations systematically scanning the white dwarf binary parameter space. We consider white dwarf masses ranging from 0.2 to 1.2 M⊙ and account for their different chemical compositions. We find excellent agreement with the orbital evolution predicted by mass transfer stability analysis. Much of our effort in this paper is dedicated to determining which binary systems are prone to a thermonuclear explosion just prior to merger or at surface contact. We find that a large fraction of He‐accreting binary systems explode: all dynamically unstable systems with accretor masses below 1.1 M⊙ and donor masses above ∼0.4 M⊙ are found to trigger a helium detonation at surface contact. A substantial fraction of these systems could explode at earlier times via detonations induced by instabilities in the accretion stream, as we have demonstrated in our previous work. We do not find definitive evidence for an explosion prior to merger or at surface contact in any of the studied double carbon–oxygen systems. Although we cannot exclude their occurrence if some helium is present, the available parameter space for a successful detonation in a white dwarf binary of pure carbon–oxygen composition is small. We demonstrate that a wide variety of dynamically unstable systems are viable Type Ia candidates. The next decade thus holds enormous promise for the study of these events, in particular with the advent of wide‐field synoptic surveys allowing a detailed characterization of their explosive properties.

show abstract

Section: Introductionmentioning

confidence: 99%

How the merger of two white dwarfs depends on their mass ratio: orbital stability and detonations at contact

Dan¹,

Rosswog²,

Guillochon³

et al. 2012

Monthly Notices of the Royal Astronomical Society

111

156

View full text Add to dashboard Cite

show abstract

“…The potential LISA sources include ultra-compact binaries in our Galaxy, supermassive black hole mergers, and extreme mass ratio inspirals (EMRIs) (Amaro-Seoane et al 2007). For the ultra-compact binaries, the possible sources can be classified into two sorts: the first one is compact detached binaries including double white dwarfs (WDs), WD -neutron star (NS) binaries, double neutron stars, and binary black holes (Nelemans et al 2001b;Liu et al 2010;Korol et al 2017;Breivik et al 2020;Kremer et al 2017aKremer et al , 2018Kremer et al , 2019Tauris 2018;Yu & Jeffery 2015;Tauris et al 2017;Lamberts et al 2018Lamberts et al , 2019Sesana et al 2020;Lau et al 2020;Andrews & Mandel 2019;Li et al 2020); the second one can be interacting binaries including cataclysmic variables (CVs), AM CVn stars, ultra-compact X-ray binaries (UCXBs) (Chen et al 2020), and compact intermediate-mass black hole X-ray binaries (Chen 2020).…”

Section: Introductionmentioning

confidence: 99%

On the Progenitors of AM CVn Stars as LISA Sources: The Evolved Donor Star Channel

Wei-min

Jiang

Chen

2021

ApJ

View full text Add to dashboard Cite

The space gravitational wave (GW) detector Laser Interferometer Space Antenna (LISA) that is planned to be launched in the early 2030s will detect the low-frequency GW signals in the Galaxy. AM CVn stars were generally thought to be important low-frequency GW sources. Employing the MESA code, in this work we calculate the evolution of a great number of binary systems consisting of a white dwarf (WD) and a main sequence (MS) star, and diagnose whether their descendant-AM CVn stars will be visible with LISA. The simulated results show that the progenitors of these LISA sources, within a distance of 1 kpc, are WD–MS binaries with a donor star of 1.0–1.4 M ⊙ (for initial WD mass of 0.5 M ⊙) or 1.0–2.0 M ⊙ (for initial WD mass of 0.7 M ⊙), and an initial orbital period slightly smaller than the bifurcation period. Our simulations also indicate that 10 verification AM CVn sources can be reproduced by the standard magnetic braking model, and are potential LISA sources. Based on the birth rate of AM CVn stars simulated by the population synthesis, the birth rate of AM CVn-LISA sources evolving from the evolved donor star channel within a distance of 1 kpc can be estimated to be (0.6–1.4) × 10−6 yr−1, and the predicted number of AM CVn-LISA sources is about 340–810. Therefore, the evolved donor star channel plays an important role in forming AM CVn-LISA sources in the Galaxy.

show abstract

“…Binary population synthesis (BPS) studies show that about several 10 7 DWDs exist in our Galaxy. Many DWDs will make contributions to the LISA noise (which is called confusion foreground noise), while (∼ 1 − 3) × 10 4 sources are expected to be individually detected by LISA (Evans et al 1987;Webbink & Han 1998;Nelemans et al 2001;Liu 2009;Liu et al 2010;Ruiter et al 2010;Yu & Jeffery 2010;Nissanke et al 2012;Korol et al 2017Korol et al , 2019Lamberts et al 2019, and references therein). Be-sides, a growing number of currently operational or future planned optical telescopes, e.g.…”

Section: Introductionmentioning

confidence: 99%

Gravitational-wave Radiation of Double Degenerates with Extremely Low-mass White Dwarf Companions

Chen

et al. 2020

ApJ

Self Cite

View full text Add to dashboard Cite

Double Degenerate systems (DDs) are supposed to be significant gravitational wave (GW) sources for future space-based gravitational-wave detectors, e.g., Laser Interferometer Space Antenna (LISA). Recently, one type of DDs with Extremely low-mass WD (ELM WD; 0.30 M ) companions has been largely found in the ELM Survey. They have very short orbital periods and are therefore important sources for LISA detection. Besides, due to the thick envelope of ELM WDs compared with massive WDs (e.g. CO WDs), they are much easier to be found by the combination of electromagnetic (EM) and GW observations. In this paper, we first obtain the population of ELM WDs in DDs with considering the detailed evolutionary tracks of ELM WDs, and then analyse the GW radiation of these systems. We found that about 6 × 10 3 sources could be solely detected by LISA, including ∼ 2 × 10 3 chirping sources, and ∼ 13 (∼ 107) more sources are expected to be detected by both LISA and ELM Survey (Gaia).

show abstract

A Comprehensive Study of Close Double White Dwarfs as Gravitational Wave Sources: Evolutionary Channels, Birth Rates, and Physical Properties

Cited by 30 publications

References 44 publications

How the merger of two white dwarfs depends on their mass ratio: orbital stability and detonations at contact

How the merger of two white dwarfs depends on their mass ratio: orbital stability and detonations at contact

On the Progenitors of AM CVn Stars as LISA Sources: The Evolved Donor Star Channel

Gravitational-wave Radiation of Double Degenerates with Extremely Low-mass White Dwarf Companions

Contact Info

Product

Resources

About