Binary white dwarfs and decihertz gravitational wave observations: From the Hubble constant to supernova astrophysics

Maselli, Andrea; Marassi, Stefania; Branchesi, M.

doi:10.1051/0004-6361/201936848

Cited by 20 publications

(18 citation statements)

References 101 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It is undetectable for LIGO and Einstein Telescope (which operate for GWs ranging from hertz to kilohertz), but is well within the sensitive range of the future LISA experiment (from millihertz to hertz). These GW events may also be targets of the B-DECIGO detector, as suggested by Maselli et al (2019). Also, we see that when the WD mass is larger, the cut-off frequency is also significantly higher.…”

Section: Numerical Resultssupporting

confidence: 60%

“…In the double-degenerate scenario, a strong GW emission is expected as the two degenerate WD stars spiral in before the final merging. Decihertz interferometers such as the DECIGO and B-DECIGO (Isoyama et al 2018;Sato et al 2017;Yagi & Seto 2011) can detect the most massive binary WDs in our Galaxy (Maselli et al 2019), and less massive binary WDs may be targets for detectors working in millihertz regime like LISA. On the contrary, in the single-degenerate scenario, GW emission should be weak during the whole process.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The Gravitational Wave Emission of Double White Dwarf Coalescences

Zou,

Zhou,

Huang

2020

Preprint

View full text Add to dashboard Cite

Type Ia Supernovae (SNe Ia) are widely used as standard candles to probe the Universe. However, how these fierce explosions are produced itself is still a highly debated issue. There are mainly two popular models for SNe Ia, i.e. the double-degenerate scenario and the single-degenerate scenario. The double-degenerate scenario suggests that SNe Ia are produced by the coalescence of two degenerate white dwarfs, while the singledegenerate scenario suggests that the continuous accretion of a single degenerate white dwarf from its normal stellar companion will finally lead to a disastrous explosion when it is over-massive, resulting in an SN Ia. The rapid development of the gravitational wave astronomy sheds new light on the nature of SNe Ia. In this study, we calculate the gravitational wave emissions of double white dwarf coalescences and compare them with the sensitivities of several upcoming detectors. It is found that the gravitational wave emissions from double white dwarf mergers in the locale universe are strong enough to be detected by LISA. We argue that LISA-like gravitational wave detectors sensitive in the frequency range of 0.01 -0.1 Hz will be a powerful tool to test the double-degenerate model of SNe Ia, and also to probe the Universe.

show abstract

Section: Numerical Resultssupporting

confidence: 60%

Section: Introductionmentioning

confidence: 99%

The Gravitational Wave Emission of Double White Dwarf Coalescences

Zou,

Zhou,

Huang

2020

Preprint

View full text Add to dashboard Cite

show abstract

“…Although LISA will not be able to observed extragalactic WD sources in large numbers, third-generation decihertz detectors (which propose to probe higher GW frequencies at greater sensitivity) may observe many extragalactic WD binaries. For instance, Maselli et al (2020) demonstrated that mergers of roughly 1 M e WDs can be resolved by DECIGO with signal-to-noise ratios of roughly 20 out to a distance of 1 Gpc, potentially enabling GW detection of roughly dozens of WD mergers formed in GCs per year.…”

Section: Estimating the Merger Rate And Prospects For Gw Detectionmentioning

confidence: 99%

White Dwarf Subsystems in Core-Collapsed Globular Clusters

Kremer

Rui

Weatherford

et al. 2021

ApJ

View full text Add to dashboard Cite

Numerical and observational evidence suggests that massive white dwarfs dominate the innermost regions of corecollapsed globular clusters by both number and total mass. Using NGC 6397 as a test case, we constrain the features of white dwarf populations in core-collapsed clusters, both at present day and throughout their lifetimes. The dynamics of these white dwarf subsystems have a number of astrophysical implications. We demonstrate that the collapse of globular cluster cores is ultimately halted by the dynamical burning of white dwarf binaries. We predict that core-collapsed clusters in the local universe yield a white dwarf merger rate of -- 10 Gpc yr 3 1 ( ) , roughly 0.1%-1% of the observed Type Ia supernova rate. We show that prior to merger, inspiraling white dwarf binaries will be observable as gravitational-wave sources at millihertz and decihertz frequencies. Over 90% of these mergers have a total mass greater than the Chandrasekhar limit. We argue that the merger/collision remnants, if not destroyed completely in an explosive transient, may be observed in core-collapsed clusters either as young neutron stars/pulsars/magnetars (in the event of accretion-induced collapse) or as young massive white dwarfs offset from the standard white dwarf cooling sequence. Finally, we show that collisions between white dwarfs and main-sequence stars, which may be detectable as bright transients, occur at a rate of -- 100 Gpc yr 3 1 ( ) in the local universe. We find that these collisions lead to depletion of blue straggler stars and main-sequence star binaries in the centers of core-collapsed clusters.

show abstract

“…Current detectors are not sensitive enough to probe the Universe at cosmological distances, not more than z ≲ 1. But, certainly, some promising projects like ET, CE and LISA will be able to detect GW events with great accuracy at cosmological distances and provide information for powerful cosmological tests [53][54][55][56][57][58][59][60][61][62][63][64][65][66][67][68][69][70].…”

Section: Introductionmentioning

confidence: 99%

Searching for modified gravity in the astrophysical gravitational wave background: Application to ground-based interferometers

Nunes

2020

Phys. Rev. D

View full text Add to dashboard Cite

We investigate how the propagation of an astrophysical gravitational wave background (AGWB) is modified over cosmological volumes when considering theories beyond general relativity of the type Horndeski gravity. We first deduce an amplitude correction on the AGWB induced for the presence of a possible running in the Planck mass. Then, we apply the spectral noise density from some ground-based interferometers, namely, the Advanced LIGO (aLIGO), Einstein Telescope (ET) and Cosmic Explore (CE), to evaluate the signal-to-noise ratio as a function of the amplitude of the running of the Planck mass for two different scenarios. We find that for observation time period ≳5 yrs and ≳1 yr, we can have a significant signal of the AGWB in the band [1-100] Hz from the ET and CE sensitivity, respectively. Finally, using Fisher information, we find some forecast bounds, and we deduce ≲27% and ≲18% correction at 1σ confidence level on the amplitude of the running of the Planck mass from ET and CE, respectively. It is clear that a detection of a AGWB in the future can open a new window to probe the nature of gravity with good accuracy.

show abstract

Binary white dwarfs and decihertz gravitational wave observations: From the Hubble constant to supernova astrophysics

Cited by 20 publications

References 101 publications

The Gravitational Wave Emission of Double White Dwarf Coalescences

The Gravitational Wave Emission of Double White Dwarf Coalescences

White Dwarf Subsystems in Core-Collapsed Globular Clusters

Searching for modified gravity in the astrophysical gravitational wave background: Application to ground-based interferometers

Contact Info

Product

Resources

About