scholarly journals Probing stellar binary black hole formation in galactic nuclei via the imprint of their center of mass acceleration on their gravitational wave signal

2017 ◽  
Vol 96 (6) ◽  
Author(s):  
Kohei Inayoshi ◽  
Nicola Tamanini ◽  
Chiara Caprini ◽  
Zoltán Haiman
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Center Of Mass ◽  
Galactic Nuclei ◽  
Hole Formation ◽  
Wave Signal ◽  
Black Hole Formation ◽  
Binary Black Hole

A Conversation among Young Astrophysicists

2021 ◽  
Vol 30 (6) ◽  
pp. 20-29
Author(s):  
Young-Min KIM ◽  
Miok PARK ◽  
Yeong-Bok BAE ◽  
Sungwook E HONG ◽  
Chan PARK
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Daily Life ◽  
Physical Significance ◽  
Hole Formation ◽  
Formation Theory ◽  
Black Hole Formation ◽  
Supermassive Black Hole ◽  
Nobel Prizes

Recently, many Nobel Prizes in Physics have been awarded in the field of astrophysics. Gravitational wave observations and contributions to LIGO in 2017, cosmology and exoplanets in 2019, and black hole formation theory and discovery of a supermassive black hole in 2020. Surprisingly, that these topics, which are somewhat distant from our daily life, have great physical significance and are being actively studied worldwide. We invited young astrophysicists at the forefront of astrophysic research to share their thoughts on astrophysics. That conversation took place online on June 2, 2021.

scholarly journals eLISA eccentricity measurements as tracers of binary black hole formation

2016 ◽  
Vol 94 (6) ◽  
Author(s):  
Atsushi Nishizawa ◽  
Emanuele Berti ◽  
Antoine Klein ◽  
Alberto Sesana
Keyword(s):  
Black Hole ◽  
Hole Formation ◽  
Black Hole Formation ◽  
Binary Black Hole

Trapping a geon: Black hole formation by an imploding gravitational wave

1992 ◽  
Vol 46 (10) ◽  
pp. R4117-R4121 ◽  
Author(s):  
Andrew M. Abrahams ◽  
Charles R. Evans
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Hole Formation ◽  
Black Hole Formation

scholarly journals The Eccentric and Accelerating Stellar Binary Black Hole Mergers in Galactic Nuclei: Observing in Ground and Space Gravitational-wave Observatories

2021 ◽  
Vol 923 (2) ◽  
pp. 139
Author(s):  
Fupeng Zhang ◽  
Xian Chen ◽  
Lijing Shao ◽  
Kohei Inayoshi
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Signal To Noise Ratio ◽  
Galactic Nuclei ◽  
Signal To Noise ◽  
High Eccentricity ◽  
Massive Black Hole ◽  
Binary Black Holes ◽  
Binary Black Hole ◽  
Space Observatories

Abstract We study the stellar binary black holes (BBHs) inspiraling/merging in galactic nuclei based on our numerical method GNC. We find that 3%–40% of all newborn BBHs will finally merge due to various dynamical effects. In a five-year mission, up to 104, 105, and ∼100 of BBHs inspiraling/merging in galactic nuclei can be detected with signal-to-noise ration >8 in Advanced LIGO (aLIGO), Einstein/DECIGO, and TianQin/LISA/TaiJi, respectively. Roughly tens are detectable in both LISA/TaiJi/TianQin and aLIGO. These BBHs have two unique characteristics. (1) Significant eccentricities: 1%–3%, 2%–7%, or 30%–90% of them have e i > 0.1 when they enter into aLIGO, Einstein, or space observatories, respectively. Such high eccentricities provide a possible explanation for that of GW190521. Most highly eccentric BBHs are not detectable in LISA/Tianqin/TaiJi before entering into aLIGO/Einstein, as their strain becomes significant only at f GW ≳ 0.1 Hz. DECIGO becomes an ideal observatory to detect those events, as it can fully cover the rising phase. (2) Up to 2% of BBHs can inspiral/merge at distances ≲103 r SW from the massive black hole, with significant accelerations, such that the Doppler phase drift of ∼10–105 of them can be detected with signal-to-noise ratio >8 in space observatories. The energy density of the gravitational-wave backgrounds (GWBs) contributed by these BBHs deviates from the power-law slope of 2/3 at f GW ≲ 1 mHz. The high eccentricity, significant accelerations, and the different profile of the GWB of these sources make them distinguishable, and thus interesting for future gravitational-wave detections and tests of relativities.

scholarly journals Inferring prompt black-hole formation in neutron star mergers from gravitational-wave data

2020 ◽  
Vol 101 (4) ◽  
Author(s):  
Michalis Agathos ◽  
Francesco Zappa ◽  
Sebastiano Bernuzzi ◽  
Albino Perego ◽  
Matteo Breschi ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gravitational Wave ◽  
Hole Formation ◽  
Black Hole Formation ◽  
Wave Data

scholarly journals Implications of Eccentric Observations on Binary Black Hole Formation Channels

2021 ◽  
Vol 921 (2) ◽  
pp. L43
Author(s):  
Michael Zevin ◽  
Isobel M. Romero-Shaw ◽  
Kyle Kremer ◽  
Eric Thrane ◽  
Paul D. Lasky
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
State Of The Art ◽  
Star Clusters ◽  
Selection Effects ◽  
Orbital Eccentricity ◽  
Hole Formation ◽  
Local Universe ◽  
Binary Black Holes ◽  
Binary Black Hole

Abstract Orbital eccentricity is one of the most robust discriminators for distinguishing between dynamical and isolated formation scenarios of binary black hole mergers using gravitational-wave observatories such as LIGO and Virgo. Using state-of-the-art cluster models, we show how selection effects impact the detectable distribution of eccentric mergers from clusters. We show that the observation (or lack thereof) of eccentric binary black hole mergers can significantly constrain the fraction of detectable systems that originate from dynamical environments, such as dense star clusters. After roughly 150 observations, observing no eccentric binary signals would indicate that clusters cannot make up the majority of the merging binary black hole population in the local universe (95% credibility). However, if dense star clusters dominate the rate of eccentric mergers and a single system is confirmed to be measurably eccentric in the first and second gravitational-wave transient catalogs, clusters must account for at least 14% of detectable binary black hole mergers. The constraints on the fraction of detectable systems from dense star clusters become significantly tighter as the number of eccentric observations grows and will be constrained to within 0.5 dex once 10 eccentric binary black holes are observed.

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