---
_id: '17517'
abstract:
- lang: eng
text: We present an analysis of NuSTAR X-ray observations of three active galactic
nuclei (AGN) that were identified as candidate subparsec binary supermassive black
hole (SMBH) systems in the Catalina Real-Time Transient Survey based on apparent
periodicity in their optical light curves. Simulations predict that close-separation
accreting SMBH binaries will have different X-ray spectra than single accreting
SMBHs. We previously observed these AGN with Chandra and found no differences
between their low-energy X-ray properties and the larger AGN population. However,
some models predict differences to be more prominent at energies higher than probed
by Chandra. We find that even at the higher energies probed by NuSTAR, the spectra
of these AGN are indistinguishable from the larger AGN population. This could
rule out models predicting large differences in the X-ray spectra in the NuSTAR
bands. Alternatively, it might mean that these three AGN are not binary SMBHs.
article_number: '104'
article_processing_charge: No
article_type: original
author:
- first_name: M. Lynne
full_name: Saade, M. Lynne
last_name: Saade
- first_name: Murray
full_name: Brightman, Murray
last_name: Brightman
- first_name: Daniel
full_name: Stern, Daniel
last_name: Stern
- first_name: Thomas
full_name: Connor, Thomas
last_name: Connor
- first_name: S. G.
full_name: Djorgovski, S. G.
last_name: Djorgovski
- first_name: Daniel J.
full_name: D’Orazio, Daniel J.
last_name: D’Orazio
- first_name: K. E. S.
full_name: Ford, K. E. S.
last_name: Ford
- first_name: Matthew J.
full_name: Graham, Matthew J.
last_name: Graham
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Hyunsung D.
full_name: Jun, Hyunsung D.
last_name: Jun
- first_name: Elias
full_name: Kammoun, Elias
last_name: Kammoun
- first_name: Ralph P.
full_name: Kraft, Ralph P.
last_name: Kraft
- first_name: Barry
full_name: McKernan, Barry
last_name: McKernan
- first_name: Alexei
full_name: Vikhlinin, Alexei
last_name: Vikhlinin
- first_name: Dominic J.
full_name: Walton, Dominic J.
last_name: Walton
citation:
ama: Saade ML, Brightman M, Stern D, et al. NuSTAR observations of candidate subparsec
binary supermassive black holes. The Astrophysical Journal. 2024;966(1).
doi:10.3847/1538-4357/ad372e
apa: Saade, M. L., Brightman, M., Stern, D., Connor, T., Djorgovski, S. G., D’Orazio,
D. J., … Walton, D. J. (2024). NuSTAR observations of candidate subparsec binary
supermassive black holes. The Astrophysical Journal. American Astronomical
Society. https://doi.org/10.3847/1538-4357/ad372e
chicago: Saade, M. Lynne, Murray Brightman, Daniel Stern, Thomas Connor, S. G. Djorgovski,
Daniel J. D’Orazio, K. E. S. Ford, et al. “NuSTAR Observations of Candidate Subparsec
Binary Supermassive Black Holes.” The Astrophysical Journal. American Astronomical
Society, 2024. https://doi.org/10.3847/1538-4357/ad372e.
ieee: M. L. Saade et al., “NuSTAR observations of candidate subparsec binary
supermassive black holes,” The Astrophysical Journal, vol. 966, no. 1.
American Astronomical Society, 2024.
ista: Saade ML, Brightman M, Stern D, Connor T, Djorgovski SG, D’Orazio DJ, Ford
KES, Graham MJ, Haiman Z, Jun HD, Kammoun E, Kraft RP, McKernan B, Vikhlinin A,
Walton DJ. 2024. NuSTAR observations of candidate subparsec binary supermassive
black holes. The Astrophysical Journal. 966(1), 104.
mla: Saade, M. Lynne, et al. “NuSTAR Observations of Candidate Subparsec Binary
Supermassive Black Holes.” The Astrophysical Journal, vol. 966, no. 1,
104, American Astronomical Society, 2024, doi:10.3847/1538-4357/ad372e.
short: M.L. Saade, M. Brightman, D. Stern, T. Connor, S.G. Djorgovski, D.J. D’Orazio,
K.E.S. Ford, M.J. Graham, Z. Haiman, H.D. Jun, E. Kammoun, R.P. Kraft, B. McKernan,
A. Vikhlinin, D.J. Walton, The Astrophysical Journal 966 (2024).
date_created: 2024-09-05T08:57:37Z
date_published: 2024-04-29T00:00:00Z
date_updated: 2024-09-10T14:31:31Z
day: '29'
doi: 10.3847/1538-4357/ad372e
extern: '1'
intvolume: ' 966'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ad372e
month: '04'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: NuSTAR observations of candidate subparsec binary supermassive black holes
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 966
year: '2024'
...
---
_id: '17531'
abstract:
- lang: eng
text: The astrophysical origin of stellar-mass black hole (BH) mergers discovered
through gravitational waves (GWs) is widely debated. Mergers in the disks of active
galactic nuclei (AGNs) represent promising environments for at least a fraction
of these events, with possible observational clues in the GW data. An additional
clue to unveil AGN merger environments is provided by possible electromagnetic
emission from postmerger accreting BHs. Associated with BH mergers in AGN disks,
emission from shocks emerging around jets launched by accreting merger remnants
is expected. Here we compute the properties of the emission produced during breakout
and the subsequent adiabatic expansion phase of the shocks, and we then apply
this model to optical flares suggested to be possibly associated with GW events.
We find that the majority of the reported flares can be explained by breakout
and shock cooling emission. If the optical flares are produced by shock cooling
emission, they would display moderate color evolution, possibly color variations
among different events, and a positive correlation between delay time and flare
duration and would be preceded by breakout emission in X-rays. If the breakout
emission dominates the observed lightcurve, we predict the color to be distributed
in a narrow range in the optical band and the delay time from GW to electromagnetic
emission to be longer than ∼2 days. Hence, further explorations of delay time
distributions, flare color evolution, and associated X-ray emission will be useful
to test the proposed emission model for the observed flares.
article_number: '21'
article_processing_charge: No
article_type: original
author:
- first_name: Hiromichi
full_name: Tagawa, Hiromichi
last_name: Tagawa
- first_name: Shigeo S
full_name: Kimura, Shigeo S
last_name: Kimura
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Rosalba
full_name: Perna, Rosalba
last_name: Perna
- first_name: Imre
full_name: Bartos, Imre
last_name: Bartos
citation:
ama: Tagawa H, Kimura SS, Haiman Z, Perna R, Bartos I. Shock cooling and breakout
emission for optical flares associated with gravitational-wave events. The
Astrophysical Journal. 2024;966(1). doi:10.3847/1538-4357/ad2e0b
apa: Tagawa, H., Kimura, S. S., Haiman, Z., Perna, R., & Bartos, I. (2024).
Shock cooling and breakout emission for optical flares associated with gravitational-wave
events. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ad2e0b
chicago: Tagawa, Hiromichi, Shigeo S Kimura, Zoltán Haiman, Rosalba Perna, and Imre
Bartos. “Shock Cooling and Breakout Emission for Optical Flares Associated with
Gravitational-Wave Events.” The Astrophysical Journal. American Astronomical
Society, 2024. https://doi.org/10.3847/1538-4357/ad2e0b.
ieee: H. Tagawa, S. S. Kimura, Z. Haiman, R. Perna, and I. Bartos, “Shock cooling
and breakout emission for optical flares associated with gravitational-wave events,”
The Astrophysical Journal, vol. 966, no. 1. American Astronomical Society,
2024.
ista: Tagawa H, Kimura SS, Haiman Z, Perna R, Bartos I. 2024. Shock cooling and
breakout emission for optical flares associated with gravitational-wave events.
The Astrophysical Journal. 966(1), 21.
mla: Tagawa, Hiromichi, et al. “Shock Cooling and Breakout Emission for Optical
Flares Associated with Gravitational-Wave Events.” The Astrophysical Journal,
vol. 966, no. 1, 21, American Astronomical Society, 2024, doi:10.3847/1538-4357/ad2e0b.
short: H. Tagawa, S.S. Kimura, Z. Haiman, R. Perna, I. Bartos, The Astrophysical
Journal 966 (2024).
date_created: 2024-09-05T09:38:53Z
date_published: 2024-04-23T00:00:00Z
date_updated: 2024-09-11T09:15:47Z
day: '23'
doi: 10.3847/1538-4357/ad2e0b
extern: '1'
intvolume: ' 966'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ad2e0b
month: '04'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Shock cooling and breakout emission for optical flares associated with gravitational-wave
events
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 966
year: '2024'
...
---
_id: '17546'
abstract:
- lang: eng
text: We show that gas disks around the components of an orbiting binary system
(so-called minidisks) may be susceptible to a resonant instability that causes
the minidisks to become significantly eccentric. Eccentricity is injected by,
and also induces, regular impacts between the minidisks at roughly the orbital
period of the binary. Such eccentric minidisks are seen in vertically integrated,
two-dimensional simulations of a circular, equal-mass binary accreting from a
circumbinary gas disk with a Γ-law equation of state. Minidisk eccentricity is
suppressed by the use of an isothermal equation of state. However, the instability
still operates and can be revealed in a minimal disk-binary simulation by removing
the circumbinary disk and feeding the minidisks from the component positions.
Minidisk eccentricity is also suppressed when the gravitational softening length
is large (≳4% of the binary semimajor axis), suggesting that its absence could
be an artifact of widely adopted numerical approximations; a follow-up study in
three dimensions with well-resolved, geometrically thin minidisks (aspect ratios
≲0.02) may be needed to assess whether eccentric minidisks can occur in real astrophysical
environments. If they can, the electromagnetic signature may be important for
discriminating between binary and single black hole scenarios for quasiperiodic
oscillations in active galactic nuclei; in turn, this might aid in targeted searches
with pulsar timing arrays for individual supermassive black hole binary sources
of low-frequency gravitational waves.
article_number: '76'
article_processing_charge: No
article_type: original
author:
- first_name: John Ryan
full_name: Westernacher-Schneider, John Ryan
last_name: Westernacher-Schneider
- first_name: Jonathan
full_name: Zrake, Jonathan
last_name: Zrake
- first_name: Andrew
full_name: MacFadyen, Andrew
last_name: MacFadyen
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: Westernacher-Schneider JR, Zrake J, MacFadyen A, Haiman Z. Eccentric minidisks
in accreting binaries. The Astrophysical Journal. 2024;962(1). doi:10.3847/1538-4357/ad1a17
apa: Westernacher-Schneider, J. R., Zrake, J., MacFadyen, A., & Haiman, Z. (2024).
Eccentric minidisks in accreting binaries. The Astrophysical Journal. American
Astronomical Society. https://doi.org/10.3847/1538-4357/ad1a17
chicago: Westernacher-Schneider, John Ryan, Jonathan Zrake, Andrew MacFadyen, and
Zoltán Haiman. “Eccentric Minidisks in Accreting Binaries.” The Astrophysical
Journal. American Astronomical Society, 2024. https://doi.org/10.3847/1538-4357/ad1a17.
ieee: J. R. Westernacher-Schneider, J. Zrake, A. MacFadyen, and Z. Haiman, “Eccentric
minidisks in accreting binaries,” The Astrophysical Journal, vol. 962,
no. 1. American Astronomical Society, 2024.
ista: Westernacher-Schneider JR, Zrake J, MacFadyen A, Haiman Z. 2024. Eccentric
minidisks in accreting binaries. The Astrophysical Journal. 962(1), 76.
mla: Westernacher-Schneider, John Ryan, et al. “Eccentric Minidisks in Accreting
Binaries.” The Astrophysical Journal, vol. 962, no. 1, 76, American Astronomical
Society, 2024, doi:10.3847/1538-4357/ad1a17.
short: J.R. Westernacher-Schneider, J. Zrake, A. MacFadyen, Z. Haiman, The Astrophysical
Journal 962 (2024).
date_created: 2024-09-05T10:06:09Z
date_published: 2024-02-08T00:00:00Z
date_updated: 2024-09-18T09:16:14Z
day: '08'
doi: 10.3847/1538-4357/ad1a17
extern: '1'
intvolume: ' 962'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ad1a17
month: '02'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Eccentric minidisks in accreting binaries
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 962
year: '2024'
...
---
_id: '17590'
abstract:
- lang: eng
text: Close encounters between stellar-mass black holes (BHs) and stars occur frequently
in dense star clusters and in the disks of active galactic nuclei. Recent studies
have shown that in highly eccentric close encounters, the star can be tidally
disrupted by the BH in a microtidal disruption event (microTDE), resulting in
rapid mass accretion and possibly bright electromagnetic signatures. Here we consider
a scenario in which the star might approach the stellar-mass BH in a gradual,
nearly circular inspiral, under the influence of dynamical friction in a circum-binary
gas disk or three-body interactions in a star cluster. We perform hydrodynamics
simulations of this scenario using the smoothed particle hydrodynamics code PHANTOM.
We find that under certain circumstances (for initial eccentricity e0 ≳ 0.4 and
penetration factor β = 1, or e0 < 0.4 and β ≲ 0.67), the mass of the star is slowly
stripped away by the BH. We call this gradual tidal disruption a "tidal-peeling
event." Additionally, we discover that some low-eccentricity microTDEs (e0 < 0.4
and β = 1) are a new form of fast luminous transients similar to parabolic microTDEs.
Depending on the initial distance and eccentricity of the encounter, these low-eccentricity
microTDEs might exhibit significant accretion rates and orbital evolution distinct
from those of a typical (eccentric) microTDE.
article_number: '149'
article_processing_charge: No
article_type: original
author:
- first_name: Chengcheng
full_name: Xin, Chengcheng
last_name: Xin
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Rosalba
full_name: Perna, Rosalba
last_name: Perna
- first_name: Yihan
full_name: Wang, Yihan
last_name: Wang
- first_name: Taeho
full_name: Ryu, Taeho
last_name: Ryu
citation:
ama: 'Xin C, Haiman Z, Perna R, Wang Y, Ryu T. “Tidal Peeling Events”: Low-eccentricity
tidal disruption of a star by a stellar-mass black hole. The Astrophysical
Journal. 2024;961(2). doi:10.3847/1538-4357/ad11d3'
apa: 'Xin, C., Haiman, Z., Perna, R., Wang, Y., & Ryu, T. (2024). “Tidal Peeling
Events”: Low-eccentricity tidal disruption of a star by a stellar-mass black hole.
The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ad11d3'
chicago: 'Xin, Chengcheng, Zoltán Haiman, Rosalba Perna, Yihan Wang, and Taeho Ryu.
“‘Tidal Peeling Events’: Low-Eccentricity Tidal Disruption of a Star by a Stellar-Mass
Black Hole.” The Astrophysical Journal. American Astronomical Society,
2024. https://doi.org/10.3847/1538-4357/ad11d3.'
ieee: 'C. Xin, Z. Haiman, R. Perna, Y. Wang, and T. Ryu, “‘Tidal Peeling Events’:
Low-eccentricity tidal disruption of a star by a stellar-mass black hole,” The
Astrophysical Journal, vol. 961, no. 2. American Astronomical Society, 2024.'
ista: 'Xin C, Haiman Z, Perna R, Wang Y, Ryu T. 2024. “Tidal Peeling Events”: Low-eccentricity
tidal disruption of a star by a stellar-mass black hole. The Astrophysical Journal.
961(2), 149.'
mla: 'Xin, Chengcheng, et al. “‘Tidal Peeling Events’: Low-Eccentricity Tidal Disruption
of a Star by a Stellar-Mass Black Hole.” The Astrophysical Journal, vol.
961, no. 2, 149, American Astronomical Society, 2024, doi:10.3847/1538-4357/ad11d3.'
short: C. Xin, Z. Haiman, R. Perna, Y. Wang, T. Ryu, The Astrophysical Journal 961
(2024).
date_created: 2024-09-05T12:36:41Z
date_published: 2024-01-22T00:00:00Z
date_updated: 2024-09-19T12:21:53Z
day: '22'
doi: 10.3847/1538-4357/ad11d3
extern: '1'
intvolume: ' 961'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ad11d3
month: '01'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: '“Tidal Peeling Events”: Low-eccentricity tidal disruption of a star by a stellar-mass
black hole'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 961
year: '2024'
...
---
_id: '17584'
abstract:
- lang: eng
text: Some Seyfert galaxies are detected in high-energy gamma rays, but the mechanism
and site of gamma-ray emission are unknown. Also, the origins of the cosmic high-energy
neutrino and MeV gamma-ray backgrounds have been veiled in mystery since their
discoveries. We propose emission from stellar-mass BHs (sBHs) embedded in disks
of active galactic nuclei as their possible sources. These sBHs are predicted
to launch jets due to the Blandford–Znajek mechanism, which can produce intense
electromagnetic, neutrino, and cosmic-ray emissions. We investigate whether these
emissions can be the sources of cosmic high-energy particles. We find that emission
from internal shocks in the jets can explain gamma rays from nearby radio-quiet
Seyfert galaxies including NGC 1068, if the Lorentz factor of the jets (Γj) is
high. On the other hand, for moderate Γj, the emission can significantly contribute
to the background gamma-ray and neutrino intensities in the ~MeV and ≲PeV bands,
respectively. Furthermore, for moderate Γj with efficient amplification of the
magnetic field and cosmic-ray acceleration, the neutrino emission from NGC 1068
and the ultrahigh-energy cosmic rays can be explained. These results suggest that
the neutrino flux from NGC 1068 as well as the background intensities of MeV gamma
rays, neutrinos, and the ultrahigh-energy cosmic rays can be explained by a unified
model. Future MeV gamma-ray satellites will test our scenario for neutrino emission.
article_number: '23'
article_processing_charge: No
article_type: original
author:
- first_name: Hiromichi
full_name: Tagawa, Hiromichi
last_name: Tagawa
- first_name: Shigeo S.
full_name: Kimura, Shigeo S.
last_name: Kimura
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: Tagawa H, Kimura SS, Haiman Z. High-energy electromagnetic, neutrino, and cosmic-ray
emission by stellar-mass black holes in disks of active galactic nuclei. The
Astrophysical Journal. 2023;955(1). doi:10.3847/1538-4357/ace71d
apa: Tagawa, H., Kimura, S. S., & Haiman, Z. (2023). High-energy electromagnetic,
neutrino, and cosmic-ray emission by stellar-mass black holes in disks of active
galactic nuclei. The Astrophysical Journal. American Astronomical Society.
https://doi.org/10.3847/1538-4357/ace71d
chicago: Tagawa, Hiromichi, Shigeo S. Kimura, and Zoltán Haiman. “High-Energy Electromagnetic,
Neutrino, and Cosmic-Ray Emission by Stellar-Mass Black Holes in Disks of Active
Galactic Nuclei.” The Astrophysical Journal. American Astronomical Society,
2023. https://doi.org/10.3847/1538-4357/ace71d.
ieee: H. Tagawa, S. S. Kimura, and Z. Haiman, “High-energy electromagnetic, neutrino,
and cosmic-ray emission by stellar-mass black holes in disks of active galactic
nuclei,” The Astrophysical Journal, vol. 955, no. 1. American Astronomical
Society, 2023.
ista: Tagawa H, Kimura SS, Haiman Z. 2023. High-energy electromagnetic, neutrino,
and cosmic-ray emission by stellar-mass black holes in disks of active galactic
nuclei. The Astrophysical Journal. 955(1), 23.
mla: Tagawa, Hiromichi, et al. “High-Energy Electromagnetic, Neutrino, and Cosmic-Ray
Emission by Stellar-Mass Black Holes in Disks of Active Galactic Nuclei.” The
Astrophysical Journal, vol. 955, no. 1, 23, American Astronomical Society,
2023, doi:10.3847/1538-4357/ace71d.
short: H. Tagawa, S.S. Kimura, Z. Haiman, The Astrophysical Journal 955 (2023).
date_created: 2024-09-05T12:28:06Z
date_published: 2023-09-12T00:00:00Z
date_updated: 2024-09-19T11:45:10Z
day: '12'
doi: 10.3847/1538-4357/ace71d
extern: '1'
intvolume: ' 955'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ace71d
month: '09'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: High-energy electromagnetic, neutrino, and cosmic-ray emission by stellar-mass
black holes in disks of active galactic nuclei
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 955
year: '2023'
...
---
_id: '17594'
abstract:
- lang: eng
text: The origin of stellar-mass black hole mergers discovered through gravitational
waves is being widely debated. Mergers in the disks of active galactic nuclei
(AGNs) represent a promising source of origin, with possible observational clues
in the gravitational-wave data. Beyond gravitational waves, a unique signature
of AGN-assisted mergers is electromagnetic emission from the accreting black holes.
Here we show that jets launched by accreting black holes merging in an AGN disk
can be detected as peculiar transients by infrared, optical, and X-ray observatories.
We further show that this emission mechanism can explain the possible associations
between gravitational-wave events and the optical transient ZTF 19abanrhr and
the proposed gamma-ray counterparts GW150914-GBM and LVT151012-GBM. We demonstrate
how these associations, if genuine, can be used to reconstruct the properties
of these events’ environments. Searching for infrared and X-ray counterparts to
similar electromagnetic transients in the future, once host galaxies are localized
by optical observations, could provide a smoking-gun signature of the mergers’
AGN origin.
article_number: '13'
article_processing_charge: No
article_type: original
author:
- first_name: Hiromichi
full_name: Tagawa, Hiromichi
last_name: Tagawa
- first_name: Shigeo S.
full_name: Kimura, Shigeo S.
last_name: Kimura
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Rosalba
full_name: Perna, Rosalba
last_name: Perna
- first_name: Imre
full_name: Bartos, Imre
last_name: Bartos
citation:
ama: Tagawa H, Kimura SS, Haiman Z, Perna R, Bartos I. Observable signature of merging
stellar-mass black holes in active galactic nuclei. The Astrophysical Journal.
2023;950(1). doi:10.3847/1538-4357/acc4bb
apa: Tagawa, H., Kimura, S. S., Haiman, Z., Perna, R., & Bartos, I. (2023).
Observable signature of merging stellar-mass black holes in active galactic nuclei.
The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/acc4bb
chicago: Tagawa, Hiromichi, Shigeo S. Kimura, Zoltán Haiman, Rosalba Perna, and
Imre Bartos. “Observable Signature of Merging Stellar-Mass Black Holes in Active
Galactic Nuclei.” The Astrophysical Journal. American Astronomical Society,
2023. https://doi.org/10.3847/1538-4357/acc4bb.
ieee: H. Tagawa, S. S. Kimura, Z. Haiman, R. Perna, and I. Bartos, “Observable signature
of merging stellar-mass black holes in active galactic nuclei,” The Astrophysical
Journal, vol. 950, no. 1. American Astronomical Society, 2023.
ista: Tagawa H, Kimura SS, Haiman Z, Perna R, Bartos I. 2023. Observable signature
of merging stellar-mass black holes in active galactic nuclei. The Astrophysical
Journal. 950(1), 13.
mla: Tagawa, Hiromichi, et al. “Observable Signature of Merging Stellar-Mass Black
Holes in Active Galactic Nuclei.” The Astrophysical Journal, vol. 950,
no. 1, 13, American Astronomical Society, 2023, doi:10.3847/1538-4357/acc4bb.
short: H. Tagawa, S.S. Kimura, Z. Haiman, R. Perna, I. Bartos, The Astrophysical
Journal 950 (2023).
date_created: 2024-09-05T12:41:47Z
date_published: 2023-06-06T00:00:00Z
date_updated: 2024-09-23T12:36:58Z
day: '06'
doi: 10.3847/1538-4357/acc4bb
extern: '1'
intvolume: ' 950'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/acc4bb
month: '06'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Observable signature of merging stellar-mass black holes in active galactic
nuclei
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 950
year: '2023'
...
---
_id: '17553'
abstract:
- lang: eng
text: 'Linear analysis of gas flows around orbiting binaries suggests that a centrifugal
barrier ought to clear a low-density cavity around the binary and inhibit mass
transfer onto it. Modern hydrodynamics simulations have confirmed the low-density
cavity, but show that any mass flowing from large scales into the circumbinary
disk is eventually transferred onto the binary components. Even though many numerical
studies confirm this picture, it is still not understood precisely how gas parcels
overcome the centrifugal barrier and ultimately accrete. We present a detailed
analysis of the binary accretion process, using an accurate prescription for evolving
grid-based hydrodynamics with Lagrangian tracer particles that track the trajectories
of individual gas parcels. We find that binary accretion can be described in four
phases: (1) gas is viscously transported through the circumbinary disk up to the
centrifugal barrier at the cavity wall, (2) the cavity wall is tidally distorted
into accretion streams consisting of near-ballistic gas parcels on eccentric orbits,
(3) the portion of each stream moving inwards of an ``accretion horizon'''' radius
r¯≃a -- the radius beyond which no material is returned to the cavity wall --
becomes bound to a minidisk orbiting an individual binary component, and (4) the
minidisk gas accretes onto the binary component through the combined effect of
viscous and tidal stresses.'
article_number: '24'
article_processing_charge: No
article_type: original
author:
- first_name: Christopher
full_name: Tiede, Christopher
last_name: Tiede
- first_name: Jonathan
full_name: Zrake, Jonathan
last_name: Zrake
- first_name: Andrew
full_name: MacFadyen, Andrew
last_name: MacFadyen
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: 'Tiede C, Zrake J, MacFadyen A, Haiman Z. How binaries accrete: Hydrodynamic
simulations with passive tracer particles. The Astrophysical Journal. 2022;932(1).
doi:10.3847/1538-4357/ac6c2b'
apa: 'Tiede, C., Zrake, J., MacFadyen, A., & Haiman, Z. (2022). How binaries
accrete: Hydrodynamic simulations with passive tracer particles. The Astrophysical
Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ac6c2b'
chicago: 'Tiede, Christopher, Jonathan Zrake, Andrew MacFadyen, and Zoltán Haiman.
“How Binaries Accrete: Hydrodynamic Simulations with Passive Tracer Particles.”
The Astrophysical Journal. American Astronomical Society, 2022. https://doi.org/10.3847/1538-4357/ac6c2b.'
ieee: 'C. Tiede, J. Zrake, A. MacFadyen, and Z. Haiman, “How binaries accrete: Hydrodynamic
simulations with passive tracer particles,” The Astrophysical Journal,
vol. 932, no. 1. American Astronomical Society, 2022.'
ista: 'Tiede C, Zrake J, MacFadyen A, Haiman Z. 2022. How binaries accrete: Hydrodynamic
simulations with passive tracer particles. The Astrophysical Journal. 932(1),
24.'
mla: 'Tiede, Christopher, et al. “How Binaries Accrete: Hydrodynamic Simulations
with Passive Tracer Particles.” The Astrophysical Journal, vol. 932, no.
1, 24, American Astronomical Society, 2022, doi:10.3847/1538-4357/ac6c2b.'
short: C. Tiede, J. Zrake, A. MacFadyen, Z. Haiman, The Astrophysical Journal 932
(2022).
date_created: 2024-09-05T10:17:13Z
date_published: 2022-06-13T00:00:00Z
date_updated: 2024-09-18T10:18:01Z
day: '13'
doi: 10.3847/1538-4357/ac6c2b
extern: '1'
intvolume: ' 932'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ac6c2b
month: '06'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'How binaries accrete: Hydrodynamic simulations with passive tracer particles'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 932
year: '2022'
...
---
_id: '17560'
abstract:
- lang: eng
text: Observations of the most luminous quasars at high redshifts (z>6) have revealed
that the largest supermassive black holes (SMBHs) at those epochs tend to be substantially
overmassive relative to their host galaxies compared to the local relations, suggesting
they experienced rapid early growth phases. We propose an assembly model for the
SMBHs that end up in rare massive ∼1012 M⊙ host halos at z∼6−7, applying a kinetic
feedback prescription for BHs accreting above the Eddington rate, provided by
radiation hydrodynamic simulations for the long-term evolution of the accretion-flow
structure. The large inflow rates into these halos during their assembly enable
the formation of >109 M⊙ SMBHs by z∼6, even starting from stellar-mass seeds at
z∼30, and even in the presence of outflows that reduce the BH feeding rate, especially
at early times. This mechanism also naturally yields a high BH-to-galaxy mass
ratio of >0.01 before the SMBH mass reaches MBH>109 M⊙ by z∼6. These fast-growing
SMBH progenitors are bright enough to be detected by upcoming observations with
the James Webb Space Telescope over a wide range of redshift (7The Astrophysical Journal. 2022;935(2). doi:10.3847/1538-4357/ac7daa'
apa: 'Hu, H., Inayoshi, K., Haiman, Z., Li, W., Quataert, E., & Kuiper, R. (2022).
Supercritical growth pathway to overmassive black holes at cosmic dawn: Coevolution
with massive quasar hosts. The Astrophysical Journal. American Astronomical
Society. https://doi.org/10.3847/1538-4357/ac7daa'
chicago: 'Hu, Haojie, Kohei Inayoshi, Zoltán Haiman, Wenxiu Li, Eliot Quataert,
and Rolf Kuiper. “Supercritical Growth Pathway to Overmassive Black Holes at Cosmic
Dawn: Coevolution with Massive Quasar Hosts.” The Astrophysical Journal.
American Astronomical Society, 2022. https://doi.org/10.3847/1538-4357/ac7daa.'
ieee: 'H. Hu, K. Inayoshi, Z. Haiman, W. Li, E. Quataert, and R. Kuiper, “Supercritical
growth pathway to overmassive black holes at cosmic dawn: Coevolution with massive
quasar hosts,” The Astrophysical Journal, vol. 935, no. 2. American Astronomical
Society, 2022.'
ista: 'Hu H, Inayoshi K, Haiman Z, Li W, Quataert E, Kuiper R. 2022. Supercritical
growth pathway to overmassive black holes at cosmic dawn: Coevolution with massive
quasar hosts. The Astrophysical Journal. 935(2), 140.'
mla: 'Hu, Haojie, et al. “Supercritical Growth Pathway to Overmassive Black Holes
at Cosmic Dawn: Coevolution with Massive Quasar Hosts.” The Astrophysical Journal,
vol. 935, no. 2, 140, American Astronomical Society, 2022, doi:10.3847/1538-4357/ac7daa.'
short: H. Hu, K. Inayoshi, Z. Haiman, W. Li, E. Quataert, R. Kuiper, The Astrophysical
Journal 935 (2022).
date_created: 2024-09-05T12:00:42Z
date_published: 2022-08-23T00:00:00Z
date_updated: 2024-09-18T12:31:26Z
day: '23'
doi: 10.3847/1538-4357/ac7daa
extern: '1'
intvolume: ' 935'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ac7daa
month: '08'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Supercritical growth pathway to overmassive black holes at cosmic dawn: Coevolution
with massive quasar hosts'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 935
year: '2022'
...
---
_id: '17568'
abstract:
- lang: eng
text: Stellar-mass BHs (sBHs) are predicted to be embedded in active galactic nuclei
(AGN) disks due to gravitational drag and in-situ star formation. However, we
find that due to a high gas density in an AGN disk environment, compact objects
may rapidly grow to intermediate-mass BHs and deplete matter from the AGN disk
unless accretion is suppressed by some feedback process(es). These consequences
are inconsistent with AGN observations and the dynamics of the Galactic center.
Here we consider mechanical feedback mechanisms for the reduction of gas accretion.
Rapidly accreting sBHs launch winds and/or jets via the Blandford-Znajek mechanism,
which produce high-pressure shocks and cocoons. Such a shock and cocoon can spread
laterally in the plane of the disk, eject the outer regions of a circum-sBH disk
(CsBD) and puncture a hole in the AGN disk with horizontal size comparable to
the disk scale-height. Since the depletion timescale of the bound CsBD is much
shorter than the resupply timescale of gas to the sBH, the time-averaged accretion
rate onto sBHs is reduced by this process by a factor of ∼10--100. This feedback
mechanism can therefore help alleviate the sBH over-growth and AGN-disk depletion
problems. On the other hand, we find that cocoons of jets can unbind a large fraction
of the gas accreting in the disks of less massive SMBHs, which may help explain
the dearth of high-Eddington ratio AGNs with SMBH mass ≲105M⊙.
article_number: '41'
article_processing_charge: No
article_type: original
author:
- first_name: Hiromichi
full_name: Tagawa, Hiromichi
last_name: Tagawa
- first_name: Shigeo S.
full_name: Kimura, Shigeo S.
last_name: Kimura
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Rosalba
full_name: Perna, Rosalba
last_name: Perna
- first_name: Hidekazu
full_name: Tanaka, Hidekazu
last_name: Tanaka
- first_name: Imre
full_name: Bartos, Imre
last_name: Bartos
citation:
ama: Tagawa H, Kimura SS, Haiman Z, Perna R, Tanaka H, Bartos I. Can stellar-mass
black hole growth disrupt disks of active galactic nuclei? The role of mechanical
feedback. The Astrophysical Journal. 2022;927(1). doi:10.3847/1538-4357/ac45f8
apa: Tagawa, H., Kimura, S. S., Haiman, Z., Perna, R., Tanaka, H., & Bartos,
I. (2022). Can stellar-mass black hole growth disrupt disks of active galactic
nuclei? The role of mechanical feedback. The Astrophysical Journal. American
Astronomical Society. https://doi.org/10.3847/1538-4357/ac45f8
chicago: Tagawa, Hiromichi, Shigeo S. Kimura, Zoltán Haiman, Rosalba Perna, Hidekazu
Tanaka, and Imre Bartos. “Can Stellar-Mass Black Hole Growth Disrupt Disks of
Active Galactic Nuclei? The Role of Mechanical Feedback.” The Astrophysical
Journal. American Astronomical Society, 2022. https://doi.org/10.3847/1538-4357/ac45f8.
ieee: H. Tagawa, S. S. Kimura, Z. Haiman, R. Perna, H. Tanaka, and I. Bartos, “Can
stellar-mass black hole growth disrupt disks of active galactic nuclei? The role
of mechanical feedback,” The Astrophysical Journal, vol. 927, no. 1. American
Astronomical Society, 2022.
ista: Tagawa H, Kimura SS, Haiman Z, Perna R, Tanaka H, Bartos I. 2022. Can stellar-mass
black hole growth disrupt disks of active galactic nuclei? The role of mechanical
feedback. The Astrophysical Journal. 927(1), 41.
mla: Tagawa, Hiromichi, et al. “Can Stellar-Mass Black Hole Growth Disrupt Disks
of Active Galactic Nuclei? The Role of Mechanical Feedback.” The Astrophysical
Journal, vol. 927, no. 1, 41, American Astronomical Society, 2022, doi:10.3847/1538-4357/ac45f8.
short: H. Tagawa, S.S. Kimura, Z. Haiman, R. Perna, H. Tanaka, I. Bartos, The Astrophysical
Journal 927 (2022).
date_created: 2024-09-05T12:13:22Z
date_published: 2022-03-03T00:00:00Z
date_updated: 2024-09-18T14:57:06Z
day: '03'
doi: 10.3847/1538-4357/ac45f8
extern: '1'
intvolume: ' 927'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ac45f8
month: '03'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Can stellar-mass black hole growth disrupt disks of active galactic nuclei?
The role of mechanical feedback
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 927
year: '2022'
...
---
_id: '17572'
abstract:
- lang: eng
text: The LIGO–Virgo–KAGRA Collaboration recently detected gravitational waves (GWs)
from the merger of black hole–neutron star (BHNS) binary systems GW200105 and
GW200115. No coincident electromagnetic (EM) counterparts were detected. While
the mass ratio and BH spin in both systems were not sufficient to tidally disrupt
the NS outside the BH event horizon, other, magnetospheric mechanisms for EM emission
exist in this regime and depend sensitively on the NS magnetic field strength.
Combining GW measurements with EM flux upper limits, we place upper limits on
the NS surface magnetic field strength above which magnetospheric emission models
would have generated an observable EM counterpart. We consider fireball models
powered by the black hole battery mechanism, where energy is output in gamma rays
over ≲1 s. Consistency with no detection by Fermi-GBM or INTEGRAL SPI-ACS constrains
the NS surface magnetic field to ≲1015 G. Hence, joint GW detection and EM upper
limits rule out the theoretical possibility that the NSs in GW200105 and GW200115,
and the putative NS in GW190814, retain dipolar magnetic fields ≳1015 G until
merger. They also rule out formation scenarios where strongly magnetized magnetars
quickly merge with BHs. We alternatively rule out operation of the BH-battery-powered
fireball mechanism in these systems. This is the first multimessenger constraint
on NS magnetic fields in BHNS systems and a novel approach to probe fields at
this point in NS evolution. This demonstrates the constraining power that multimessenger
analyses of BHNS mergers have on BHNS formation scenarios, NS magnetic field evolution,
and the physics of BHNS magnetospheric interactions.
article_number: '56'
article_processing_charge: No
article_type: original
author:
- first_name: Daniel J.
full_name: D’Orazio, Daniel J.
last_name: D’Orazio
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Janna
full_name: Levin, Janna
last_name: Levin
- first_name: Johan
full_name: Samsing, Johan
last_name: Samsing
- first_name: Alejandro
full_name: Vigna-Gómez, Alejandro
last_name: Vigna-Gómez
citation:
ama: D’Orazio DJ, Haiman Z, Levin J, Samsing J, Vigna-Gómez A. Multimessenger constraints
on magnetic fields in merging black hole–neutron star binaries. The Astrophysical
Journal. 2022;927(1). doi:10.3847/1538-4357/ac4bdb
apa: D’Orazio, D. J., Haiman, Z., Levin, J., Samsing, J., & Vigna-Gómez, A.
(2022). Multimessenger constraints on magnetic fields in merging black hole–neutron
star binaries. The Astrophysical Journal. American Astronomical Society.
https://doi.org/10.3847/1538-4357/ac4bdb
chicago: D’Orazio, Daniel J., Zoltán Haiman, Janna Levin, Johan Samsing, and Alejandro
Vigna-Gómez. “Multimessenger Constraints on Magnetic Fields in Merging Black Hole–Neutron
Star Binaries.” The Astrophysical Journal. American Astronomical Society,
2022. https://doi.org/10.3847/1538-4357/ac4bdb.
ieee: D. J. D’Orazio, Z. Haiman, J. Levin, J. Samsing, and A. Vigna-Gómez, “Multimessenger
constraints on magnetic fields in merging black hole–neutron star binaries,” The
Astrophysical Journal, vol. 927, no. 1. American Astronomical Society, 2022.
ista: D’Orazio DJ, Haiman Z, Levin J, Samsing J, Vigna-Gómez A. 2022. Multimessenger
constraints on magnetic fields in merging black hole–neutron star binaries. The
Astrophysical Journal. 927(1), 56.
mla: D’Orazio, Daniel J., et al. “Multimessenger Constraints on Magnetic Fields
in Merging Black Hole–Neutron Star Binaries.” The Astrophysical Journal,
vol. 927, no. 1, 56, American Astronomical Society, 2022, doi:10.3847/1538-4357/ac4bdb.
short: D.J. D’Orazio, Z. Haiman, J. Levin, J. Samsing, A. Vigna-Gómez, The Astrophysical
Journal 927 (2022).
date_created: 2024-09-05T12:15:46Z
date_published: 2022-01-01T00:00:00Z
date_updated: 2024-09-19T07:25:13Z
doi: 10.3847/1538-4357/ac4bdb
extern: '1'
intvolume: ' 927'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ac4bdb
month: '01'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Multimessenger constraints on magnetic fields in merging black hole–neutron
star binaries
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 927
year: '2022'
...
---
_id: '17608'
abstract:
- lang: eng
text: We study the long-term evolution of the global structure of axisymmetric accretion
flows onto a black hole (BH) at rates substantially higher than the Eddington
value (M˙Edd), performing two-dimensional hydrodynamical simulations with and
without radiative diffusion. In the high-accretion optically-thick limit, where
the radiation energy is efficiently trapped within the inflow, the accretion flow
becomes adiabatic and comprises of turbulent gas in the equatorial region and
strong bipolar outflows. As a result, the mass inflow rate decreases toward the
center as M˙in∝rp with p∼0.5−0.7 and a small fraction of the inflowing gas feeds
the nuclear BH. Thus, super-Eddington accretion is sustained only when a larger
amount of gas is supplied from larger radii at >100−1000 M˙Edd. The global structure
of the flow settles down to a quasi-steady state in millions of the orbital timescale
at the BH event horizon, which is >10−100 times longer than that addressed in
previous (magneto-)RHD simulation studies. Energy transport via radiative diffusion
accelerates the outflow near the poles in the inner region but does not change
the overall properties of the accretion flow compared to the cases without diffusion.
Based on our simulation results, we provide a mechanical feedback model for super-Eddington
accreting BHs. This can be applied as a sub-grid model in large-scale cosmological
simulations that do not sufficiently resolve galactic nuclei, and to the formation
of the heaviest gravitational-wave sources via accretion in dense environments.
article_number: '132'
article_processing_charge: No
article_type: original
author:
- first_name: Haojie
full_name: Hu, Haojie
last_name: Hu
- first_name: Kohei
full_name: Inayoshi, Kohei
last_name: Inayoshi
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Eliot
full_name: Quataert, Eliot
last_name: Quataert
- first_name: Rolf
full_name: Kuiper, Rolf
last_name: Kuiper
citation:
ama: 'Hu H, Inayoshi K, Haiman Z, Quataert E, Kuiper R. Long-term evolution of supercritical
black hole accretion with outflows: A subgrid feedback model for cosmological
simulations. The Astrophysical Journal. 2022;934(2). doi:10.3847/1538-4357/ac75d8'
apa: 'Hu, H., Inayoshi, K., Haiman, Z., Quataert, E., & Kuiper, R. (2022). Long-term
evolution of supercritical black hole accretion with outflows: A subgrid feedback
model for cosmological simulations. The Astrophysical Journal. American
Astronomical Society. https://doi.org/10.3847/1538-4357/ac75d8'
chicago: 'Hu, Haojie, Kohei Inayoshi, Zoltán Haiman, Eliot Quataert, and Rolf Kuiper.
“Long-Term Evolution of Supercritical Black Hole Accretion with Outflows: A Subgrid
Feedback Model for Cosmological Simulations.” The Astrophysical Journal.
American Astronomical Society, 2022. https://doi.org/10.3847/1538-4357/ac75d8.'
ieee: 'H. Hu, K. Inayoshi, Z. Haiman, E. Quataert, and R. Kuiper, “Long-term evolution
of supercritical black hole accretion with outflows: A subgrid feedback model
for cosmological simulations,” The Astrophysical Journal, vol. 934, no.
2. American Astronomical Society, 2022.'
ista: 'Hu H, Inayoshi K, Haiman Z, Quataert E, Kuiper R. 2022. Long-term evolution
of supercritical black hole accretion with outflows: A subgrid feedback model
for cosmological simulations. The Astrophysical Journal. 934(2), 132.'
mla: 'Hu, Haojie, et al. “Long-Term Evolution of Supercritical Black Hole Accretion
with Outflows: A Subgrid Feedback Model for Cosmological Simulations.” The
Astrophysical Journal, vol. 934, no. 2, 132, American Astronomical Society,
2022, doi:10.3847/1538-4357/ac75d8.'
short: H. Hu, K. Inayoshi, Z. Haiman, E. Quataert, R. Kuiper, The Astrophysical
Journal 934 (2022).
date_created: 2024-09-05T13:17:38Z
date_published: 2022-08-01T00:00:00Z
date_updated: 2024-09-23T14:23:12Z
day: '01'
doi: 10.3847/1538-4357/ac75d8
extern: '1'
intvolume: ' 934'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ac75d8
month: '08'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Long-term evolution of supercritical black hole accretion with outflows: A
subgrid feedback model for cosmological simulations'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 934
year: '2022'
...
---
_id: '17509'
abstract:
- lang: eng
text: The recently discovered gravitational wave sources GW190521 and GW190814 have
shown evidence of BH mergers with masses and spins outside of the range expected
from isolated stellar evolution. These merging objects could have undergone previous
mergers. Such hierarchical mergers are predicted to be frequent in active galactic
nuclei (AGNs) disks, where binaries form and evolve efficiently by dynamical interactions
and gaseous dissipation. Here we compare the properties of these observed events
to the theoretical models of mergers in AGN disks, which are obtained by performing
one-dimensional N-body simulations combined with semi-analytical prescriptions.
The high BH masses in GW190521 are consistent with mergers of high-generation
(high-g) BHs where the initial progenitor stars had high metallicity, 2g BHs if
the original progenitors were metal-poor, or 1g BHs that had gained mass via super-Eddington
accretion. Other measured properties related to spin parameters in GW190521 are
also consistent with mergers in AGN disks. Furthermore, mergers in the lower mass
gap or those with low mass ratio as found in GW190814 and GW190412 are also reproduced
by mergers of 2g–1g or 1g–1g objects with significant accretion in AGN disks.
Finally, due to gas accretion, the massive neutron star merger reported in GW190425
can be produced in an AGN disk.
article_number: '194'
article_processing_charge: No
article_type: original
author:
- first_name: Hiromichi
full_name: Tagawa, Hiromichi
last_name: Tagawa
- first_name: Bence
full_name: Kocsis, Bence
last_name: Kocsis
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Imre
full_name: Bartos, Imre
last_name: Bartos
- first_name: Kazuyuki
full_name: Omukai, Kazuyuki
last_name: Omukai
- first_name: Johan
full_name: Samsing, Johan
last_name: Samsing
citation:
ama: Tagawa H, Kocsis B, Haiman Z, Bartos I, Omukai K, Samsing J. Mass-gap mergers
in active galactic nuclei. The Astrophysical Journal. 2021;908(2). doi:10.3847/1538-4357/abd555
apa: Tagawa, H., Kocsis, B., Haiman, Z., Bartos, I., Omukai, K., & Samsing,
J. (2021). Mass-gap mergers in active galactic nuclei. The Astrophysical Journal.
American Astronomical Society. https://doi.org/10.3847/1538-4357/abd555
chicago: Tagawa, Hiromichi, Bence Kocsis, Zoltán Haiman, Imre Bartos, Kazuyuki Omukai,
and Johan Samsing. “Mass-Gap Mergers in Active Galactic Nuclei.” The Astrophysical
Journal. American Astronomical Society, 2021. https://doi.org/10.3847/1538-4357/abd555.
ieee: H. Tagawa, B. Kocsis, Z. Haiman, I. Bartos, K. Omukai, and J. Samsing, “Mass-gap
mergers in active galactic nuclei,” The Astrophysical Journal, vol. 908,
no. 2. American Astronomical Society, 2021.
ista: Tagawa H, Kocsis B, Haiman Z, Bartos I, Omukai K, Samsing J. 2021. Mass-gap
mergers in active galactic nuclei. The Astrophysical Journal. 908(2), 194.
mla: Tagawa, Hiromichi, et al. “Mass-Gap Mergers in Active Galactic Nuclei.” The
Astrophysical Journal, vol. 908, no. 2, 194, American Astronomical Society,
2021, doi:10.3847/1538-4357/abd555.
short: H. Tagawa, B. Kocsis, Z. Haiman, I. Bartos, K. Omukai, J. Samsing, The Astrophysical
Journal 908 (2021).
date_created: 2024-09-05T08:47:46Z
date_published: 2021-02-24T00:00:00Z
date_updated: 2024-09-10T12:36:17Z
day: '24'
doi: 10.3847/1538-4357/abd555
extern: '1'
intvolume: ' 908'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/abd555
month: '02'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Mass-gap mergers in active galactic nuclei
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 908
year: '2021'
...
---
_id: '17515'
abstract:
- lang: eng
text: 'The disks of active galactic nuclei (AGNs) have emerged as a rich environment
for the evolution of stars and their compact remnants. The very dense medium favors
rapid accretion, while torques and migration traps enhance binary formation and
mergers. Both long and short gamma-ray bursts are hence expected. We show that
AGN disks constitute an ideal environment for another interesting phenomenon:
the accretion-induced collapse (AIC) of neutron stars (NSs) to black holes (BHs).
Rapid accretion in the dense disks can cause NSs to grow to the point of exceeding
the maximum mass allowed by their equation of state. General relativistic magnetohydrodynamical
simulations have shown that electromagnetic signatures are expected if the NS
is surrounded by a minidisk prior to collapse, which then rapidly accretes onto
the BH, and/or if the NS is highly magnetized, from reconnection of the magnetosphere
during collapse. Here we compute the rates of AICs and their locations within
the disks for both isolated NSs and for (initially stable) NSs formed from NS-NS
mergers. We find that the global AIC rates are ∼0.07–20 Gpc−3 yr−1, and we discuss
their observable prospects and signatures as they emerge from the dense disk environments.'
article_number: '10'
article_processing_charge: No
article_type: original
author:
- first_name: Rosalba
full_name: Perna, Rosalba
last_name: Perna
- first_name: Hiromichi
full_name: Tagawa, Hiromichi
last_name: Tagawa
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Imre
full_name: Bartos, Imre
last_name: Bartos
citation:
ama: Perna R, Tagawa H, Haiman Z, Bartos I. Accretion-induced collapse of neutron
stars in the disks of active galactic nuclei. The Astrophysical Journal.
2021;915(1). doi:10.3847/1538-4357/abfdb4
apa: Perna, R., Tagawa, H., Haiman, Z., & Bartos, I. (2021). Accretion-induced
collapse of neutron stars in the disks of active galactic nuclei. The Astrophysical
Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/abfdb4
chicago: Perna, Rosalba, Hiromichi Tagawa, Zoltán Haiman, and Imre Bartos. “Accretion-Induced
Collapse of Neutron Stars in the Disks of Active Galactic Nuclei.” The Astrophysical
Journal. American Astronomical Society, 2021. https://doi.org/10.3847/1538-4357/abfdb4.
ieee: R. Perna, H. Tagawa, Z. Haiman, and I. Bartos, “Accretion-induced collapse
of neutron stars in the disks of active galactic nuclei,” The Astrophysical
Journal, vol. 915, no. 1. American Astronomical Society, 2021.
ista: Perna R, Tagawa H, Haiman Z, Bartos I. 2021. Accretion-induced collapse of
neutron stars in the disks of active galactic nuclei. The Astrophysical Journal.
915(1), 10.
mla: Perna, Rosalba, et al. “Accretion-Induced Collapse of Neutron Stars in the
Disks of Active Galactic Nuclei.” The Astrophysical Journal, vol. 915,
no. 1, 10, American Astronomical Society, 2021, doi:10.3847/1538-4357/abfdb4.
short: R. Perna, H. Tagawa, Z. Haiman, I. Bartos, The Astrophysical Journal 915
(2021).
date_created: 2024-09-05T08:55:06Z
date_published: 2021-06-28T00:00:00Z
date_updated: 2024-09-10T13:47:31Z
day: '28'
doi: 10.3847/1538-4357/abfdb4
extern: '1'
intvolume: ' 915'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/abfdb4
month: '06'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Accretion-induced collapse of neutron stars in the disks of active galactic
nuclei
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 915
year: '2021'
...
---
_id: '17598'
abstract:
- lang: eng
text: The successive discoveries of binary merger events by Advanced LIGO-Virgo
have been revealing the statistical properties of binary black hole (BBH) populations.
A stochastic gravitational wave background (GWB) is a useful tool to probe the
cosmological evolution of those compact mergers. In this paper, we study the upper
bound on a GWB produced by BBH mergers, whose stellar progenitors dominate the
reionization process at the cosmic dawn. Since early reionization by those progenitors
yields a high optical depth of the universe inconsistent with the {\it Planck}
measurements, the cumulative mass density is limited to ρ⋆≲107 M⊙ Mpc−3. Even
with this upper bound, the amplitude of a GWB owing to the high-z BBH mergers
is expected to be as high as Ωgw≃1.48+1.80−1.27×10−9 at f≃25 Hz, while their merger
rate at the present-day is consistent or lower than the observed GW event rate.
This level of GWB is detectable at the design sensitivity of Advanced LIGO-Virgo
and would indicate a major contribution of the high-z BBH population to the local
GW events. The spectral index is expected to be substantially flatter than the
canonical value of ≃2/3 generically produced by lower-redshift and less massive
BBHs. Moreover, if their mass function is more top-heavy than in the local universe,
the GWB spectrum is even more skewed toward lower frequencies, which would allow
us to extract information on the mass function of merging BBHs at high redshifts.
article_number: '41'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Kohei
full_name: Inayoshi, Kohei
last_name: Inayoshi
- first_name: Kazumi
full_name: Kashiyama, Kazumi
last_name: Kashiyama
- first_name: Eli
full_name: Visbal, Eli
last_name: Visbal
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: 'Inayoshi K, Kashiyama K, Visbal E, Haiman Z. Gravitational wave backgrounds
from coalescing black hole binaries at cosmic dawn: An upper bound. The Astrophysical
Journal. 2021;919(1). doi:10.3847/1538-4357/ac106d'
apa: 'Inayoshi, K., Kashiyama, K., Visbal, E., & Haiman, Z. (2021). Gravitational
wave backgrounds from coalescing black hole binaries at cosmic dawn: An upper
bound. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ac106d'
chicago: 'Inayoshi, Kohei, Kazumi Kashiyama, Eli Visbal, and Zoltán Haiman. “Gravitational
Wave Backgrounds from Coalescing Black Hole Binaries at Cosmic Dawn: An Upper
Bound.” The Astrophysical Journal. American Astronomical Society, 2021.
https://doi.org/10.3847/1538-4357/ac106d.'
ieee: 'K. Inayoshi, K. Kashiyama, E. Visbal, and Z. Haiman, “Gravitational wave
backgrounds from coalescing black hole binaries at cosmic dawn: An upper bound,”
The Astrophysical Journal, vol. 919, no. 1. American Astronomical Society,
2021.'
ista: 'Inayoshi K, Kashiyama K, Visbal E, Haiman Z. 2021. Gravitational wave backgrounds
from coalescing black hole binaries at cosmic dawn: An upper bound. The Astrophysical
Journal. 919(1), 41.'
mla: 'Inayoshi, Kohei, et al. “Gravitational Wave Backgrounds from Coalescing Black
Hole Binaries at Cosmic Dawn: An Upper Bound.” The Astrophysical Journal,
vol. 919, no. 1, 41, American Astronomical Society, 2021, doi:10.3847/1538-4357/ac106d.'
short: K. Inayoshi, K. Kashiyama, E. Visbal, Z. Haiman, The Astrophysical Journal
919 (2021).
date_created: 2024-09-05T12:46:25Z
date_published: 2021-09-22T00:00:00Z
date_updated: 2024-09-23T13:08:15Z
day: '22'
doi: 10.3847/1538-4357/ac106d
extern: '1'
external_id:
arxiv:
- '2103.12755'
intvolume: ' 919'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: ' https://doi.org/10.48550/arXiv.2103.12755'
month: '09'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Gravitational wave backgrounds from coalescing black hole binaries at cosmic
dawn: An upper bound'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 919
year: '2021'
...
---
_id: '17529'
abstract:
- lang: eng
text: The astrophysical origin of gravitational wave (GW) events is one of the most
timely problems in the wake of the LIGO/Virgo discoveries. In active galactic
nuclei (AGN), binaries form and evolve efficiently by dynamical interactions and
gaseous dissipation. Previous studies have suggested that binary black hole (BBH)
mergers in AGN disks can contribute significantly to BBH mergers observed by GW
interferometers. Here we examine the distribution of the effective spin parameter
χeff of this GW source population. We extend our semi-analytical model of binary
formation and evolution in AGN disks by following the evolution of the binary
orbital angular momenta and black hole (BH) spins. BH spins change due to gas
accretion and BH mergers, while the binary orbital angular momenta evolve due
to gas accretion and binary-single interactions. We find that the distribution
of χeff predicted by our AGN model is similar to the distribution observed during
LIGO/Virgo O1 and O2. On the other hand, if radial migration of BHs is inefficient,
χeff is skewed toward higher values compared with the observed distribution, because
of the paucity of scattering events that would randomize spin directions relative
to the orbital plane. We suggest that high binary masses and the positive correlation
between binary mass and the standard deviation of χeff for chirp masses up to
≈20 M⊙, can be possible signatures for mergers originating in AGN disks. Finally,
hierarchical mergers in AGN disks naturally produce properties of the recent GW
event GW190412, including a low mass ratio, a high primary BH spin, and a significant
spin component in the orbital plane.
article_number: '26'
article_processing_charge: No
article_type: original
author:
- first_name: Hiromichi
full_name: Tagawa, Hiromichi
last_name: Tagawa
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Imre
full_name: Bartos, Imre
last_name: Bartos
- first_name: Bence
full_name: Kocsis, Bence
last_name: Kocsis
citation:
ama: Tagawa H, Haiman Z, Bartos I, Kocsis B. Spin evolution of stellar-mass black
hole binaries in active galactic nuclei. The Astrophysical Journal. 2020;899(1).
doi:10.3847/1538-4357/aba2cc
apa: Tagawa, H., Haiman, Z., Bartos, I., & Kocsis, B. (2020). Spin evolution
of stellar-mass black hole binaries in active galactic nuclei. The Astrophysical
Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/aba2cc
chicago: Tagawa, Hiromichi, Zoltán Haiman, Imre Bartos, and Bence Kocsis. “Spin
Evolution of Stellar-Mass Black Hole Binaries in Active Galactic Nuclei.” The
Astrophysical Journal. American Astronomical Society, 2020. https://doi.org/10.3847/1538-4357/aba2cc.
ieee: H. Tagawa, Z. Haiman, I. Bartos, and B. Kocsis, “Spin evolution of stellar-mass
black hole binaries in active galactic nuclei,” The Astrophysical Journal,
vol. 899, no. 1. American Astronomical Society, 2020.
ista: Tagawa H, Haiman Z, Bartos I, Kocsis B. 2020. Spin evolution of stellar-mass
black hole binaries in active galactic nuclei. The Astrophysical Journal. 899(1),
26.
mla: Tagawa, Hiromichi, et al. “Spin Evolution of Stellar-Mass Black Hole Binaries
in Active Galactic Nuclei.” The Astrophysical Journal, vol. 899, no. 1,
26, American Astronomical Society, 2020, doi:10.3847/1538-4357/aba2cc.
short: H. Tagawa, Z. Haiman, I. Bartos, B. Kocsis, The Astrophysical Journal 899
(2020).
date_created: 2024-09-05T09:36:37Z
date_published: 2020-08-10T00:00:00Z
date_updated: 2024-09-11T09:11:55Z
day: '10'
doi: 10.3847/1538-4357/aba2cc
extern: '1'
intvolume: ' 899'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/aba2cc
month: '08'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Spin evolution of stellar-mass black hole binaries in active galactic nuclei
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 899
year: '2020'
...
---
_id: '17542'
abstract:
- lang: eng
text: 'We present a new semianalytic model of the formation of the first stars.
Our method takes dark matter halo merger trees (including three-dimensional spatial
information) from cosmological N-body simulations as input and applies analytic
prescriptions to compute both the Population III and metal-enriched star formation
histories. We have developed a novel method to accurately compute the major feedback
processes affecting Population III star formation: H2 photodissociation from Lyman–Werner
(LW) radiation, suppression of star formation due to inhomogeneous reionization,
and metal enrichment via supernova winds. Our method utilizes a grid-based approach
relying on fast Fourier transforms to rapidly track the LW intensity, ionization
fraction, and metallicity in three dimensions throughout the simulation box. We
present simulations for a wide range of astrophysical model parameters from z
≈ 30 to 6. Initially long-range LW feedback and local metal enrichment and reionization
feedback dominate. However, for z ≲ 15 we find that the star formation rate density
(SFRD) of Population III stars is impacted by the combination of external metal
enrichment (metals from one halo polluting other pristine halos) and inhomogeneous
reionization. We find that the interplay of these processes is particularly important
for the Population III SFRD at z ≲ 10. Reionization feedback delays star formation
long enough for metal bubbles to reach halos that would otherwise form Population
III stars. Including these effects can lead to more than an order-of-magnitude
decrease in the Population III SFRD at z = 6 compared to LW feedback alone.'
article_number: '95'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Eli
full_name: Visbal, Eli
last_name: Visbal
- first_name: Greg L.
full_name: Bryan, Greg L.
last_name: Bryan
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: Visbal E, Bryan GL, Haiman Z. Self-consistent semianalytic modeling of feedback
during primordial star formation and reionization. The Astrophysical Journal.
2020;897(1). doi:10.3847/1538-4357/ab994e
apa: Visbal, E., Bryan, G. L., & Haiman, Z. (2020). Self-consistent semianalytic
modeling of feedback during primordial star formation and reionization. The
Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ab994e
chicago: Visbal, Eli, Greg L. Bryan, and Zoltán Haiman. “Self-Consistent Semianalytic
Modeling of Feedback during Primordial Star Formation and Reionization.” The
Astrophysical Journal. American Astronomical Society, 2020. https://doi.org/10.3847/1538-4357/ab994e.
ieee: E. Visbal, G. L. Bryan, and Z. Haiman, “Self-consistent semianalytic modeling
of feedback during primordial star formation and reionization,” The Astrophysical
Journal, vol. 897, no. 1. American Astronomical Society, 2020.
ista: Visbal E, Bryan GL, Haiman Z. 2020. Self-consistent semianalytic modeling
of feedback during primordial star formation and reionization. The Astrophysical
Journal. 897(1), 95.
mla: Visbal, Eli, et al. “Self-Consistent Semianalytic Modeling of Feedback during
Primordial Star Formation and Reionization.” The Astrophysical Journal,
vol. 897, no. 1, 95, American Astronomical Society, 2020, doi:10.3847/1538-4357/ab994e.
short: E. Visbal, G.L. Bryan, Z. Haiman, The Astrophysical Journal 897 (2020).
date_created: 2024-09-05T09:58:26Z
date_published: 2020-07-07T00:00:00Z
date_updated: 2024-09-12T13:28:25Z
day: '07'
doi: 10.3847/1538-4357/ab994e
extern: '1'
external_id:
arxiv:
- '2001.11118'
intvolume: ' 897'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: ' https://doi.org/10.48550/arXiv.2001.11118'
month: '07'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Self-consistent semianalytic modeling of feedback during primordial star formation
and reionization
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 897
year: '2020'
...
---
_id: '17579'
abstract:
- lang: eng
text: Approximately 200 supermassive black holes (SMBHs) have been discovered within
the first ∼gigayear after the Big Bang. One pathway for the formation of SMBHs
is through the collapse of supermassive stars (SMSs). A possible obstacle to this
scenario is that the collapsing gas fragments and forms a cluster of main-sequence
stars. Here, we raise the possibility that stellar collisions may be sufficiently
frequent and energetic to inhibit the contraction of the massive protostar, avoiding
strong UV radiation driven outflows, and allowing it to continue growing into
an SMS. We investigate this scenario with semianalytic models incorporating star
formation; gas accretion; dynamical friction from stars and gas; stellar collisions;
and gas ejection. We find that when the collapsing gas fragments at a density
of ≲3 × 1010 cm−3, the central protostar contracts due to infrequent stellar mergers,
and in turn photoevaporates the remaining collapsing gas, resulting in the formation
of a ≲104 M⊙ object. On the other hand, when the collapsing gas fragments at higher
densities (expected for a metal-poor cloud with Z ≲ 10−5 Z⊙ with suppressed H2
abundance) the central protostar avoids contraction and keeps growing via frequent
stellar mergers, reaching masses as high as ∼105–106 M⊙. We conclude that frequent
stellar mergers represent a possible pathway to form massive BHs in the early
universe.
article_number: '36'
article_processing_charge: No
article_type: original
author:
- first_name: Hiromichi
full_name: Tagawa, Hiromichi
last_name: Tagawa
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Bence
full_name: Kocsis, Bence
last_name: Kocsis
citation:
ama: Tagawa H, Haiman Z, Kocsis B. Making a supermassive star by stellar bombardment.
The Astrophysical Journal. 2020;892(1). doi:10.3847/1538-4357/ab7922
apa: Tagawa, H., Haiman, Z., & Kocsis, B. (2020). Making a supermassive star
by stellar bombardment. The Astrophysical Journal. American Astronomical
Society. https://doi.org/10.3847/1538-4357/ab7922
chicago: Tagawa, Hiromichi, Zoltán Haiman, and Bence Kocsis. “Making a Supermassive
Star by Stellar Bombardment.” The Astrophysical Journal. American Astronomical
Society, 2020. https://doi.org/10.3847/1538-4357/ab7922.
ieee: H. Tagawa, Z. Haiman, and B. Kocsis, “Making a supermassive star by stellar
bombardment,” The Astrophysical Journal, vol. 892, no. 1. American Astronomical
Society, 2020.
ista: Tagawa H, Haiman Z, Kocsis B. 2020. Making a supermassive star by stellar
bombardment. The Astrophysical Journal. 892(1), 36.
mla: Tagawa, Hiromichi, et al. “Making a Supermassive Star by Stellar Bombardment.”
The Astrophysical Journal, vol. 892, no. 1, 36, American Astronomical Society,
2020, doi:10.3847/1538-4357/ab7922.
short: H. Tagawa, Z. Haiman, B. Kocsis, The Astrophysical Journal 892 (2020).
date_created: 2024-09-05T12:22:41Z
date_published: 2020-03-24T00:00:00Z
date_updated: 2024-09-19T11:21:17Z
day: '24'
doi: 10.3847/1538-4357/ab7922
extern: '1'
intvolume: ' 892'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ab7922
month: '03'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Making a supermassive star by stellar bombardment
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 892
year: '2020'
...
---
_id: '17581'
abstract:
- lang: eng
text: We present analysis of Chandra X-ray observations of seven quasars that were
identified as candidate subparsec binary supermassive black hole (SMBH) systems
in the Catalina Real-Time Transient Survey based on the apparent periodicity in
their optical light curves. Simulations predict that close-separation accreting
SMBH binaries will have different X-ray spectra than single accreting SMBHs, including
harder or softer X-ray spectra, ripple-like profiles in the Fe K-α line, and distinct
peaks in the spectrum due to the separation of the accretion disk into a circumbinary
disk and mini disks around each SMBH. We obtained Chandra observations to test
these models and assess whether these quasars could contain binary SMBHs. We instead
find that the quasar spectra are all well fit by simple absorbed power-law models,
with the rest-frame 2–10 keV photon indices, Γ, and the X-ray-to-optical power
slopes, αOX, indistinguishable from those of the larger quasar population. This
may indicate that these seven quasars are not truly subparsec binary SMBH systems,
or it may simply reflect that our sample size was too small to robustly detect
any differences. Alternatively, the X-ray spectral changes might only be evident
at energies higher than probed by Chandra. Given the available models and current
data, no firm conclusions are drawn. These observations will help motivate and
direct further work on theoretical models of binary SMBH systems, such as modeling
systems with thinner accretion disks and larger binary separations.
article_number: '148'
article_processing_charge: No
article_type: original
author:
- first_name: M. Lynne
full_name: Saade, M. Lynne
last_name: Saade
- first_name: Daniel
full_name: Stern, Daniel
last_name: Stern
- first_name: Murray
full_name: Brightman, Murray
last_name: Brightman
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: S. G.
full_name: Djorgovski, S. G.
last_name: Djorgovski
- first_name: Daniel
full_name: D’Orazio, Daniel
last_name: D’Orazio
- first_name: K. E. S.
full_name: Ford, K. E. S.
last_name: Ford
- first_name: Matthew J.
full_name: Graham, Matthew J.
last_name: Graham
- first_name: Hyunsung D.
full_name: Jun, Hyunsung D.
last_name: Jun
- first_name: Ralph P.
full_name: Kraft, Ralph P.
last_name: Kraft
- first_name: Barry
full_name: McKernan, Barry
last_name: McKernan
- first_name: Alexei
full_name: Vikhlinin, Alexei
last_name: Vikhlinin
- first_name: Dominic J.
full_name: Walton, Dominic J.
last_name: Walton
citation:
ama: Saade ML, Stern D, Brightman M, et al. Chandra observations of candidate subparsec
binary supermassive black holes. The Astrophysical Journal. 2020;900(2).
doi:10.3847/1538-4357/abad31
apa: Saade, M. L., Stern, D., Brightman, M., Haiman, Z., Djorgovski, S. G., D’Orazio,
D., … Walton, D. J. (2020). Chandra observations of candidate subparsec binary
supermassive black holes. The Astrophysical Journal. American Astronomical
Society. https://doi.org/10.3847/1538-4357/abad31
chicago: Saade, M. Lynne, Daniel Stern, Murray Brightman, Zoltán Haiman, S. G. Djorgovski,
Daniel D’Orazio, K. E. S. Ford, et al. “Chandra Observations of Candidate Subparsec
Binary Supermassive Black Holes.” The Astrophysical Journal. American Astronomical
Society, 2020. https://doi.org/10.3847/1538-4357/abad31.
ieee: M. L. Saade et al., “Chandra observations of candidate subparsec binary
supermassive black holes,” The Astrophysical Journal, vol. 900, no. 2.
American Astronomical Society, 2020.
ista: Saade ML, Stern D, Brightman M, Haiman Z, Djorgovski SG, D’Orazio D, Ford
KES, Graham MJ, Jun HD, Kraft RP, McKernan B, Vikhlinin A, Walton DJ. 2020. Chandra
observations of candidate subparsec binary supermassive black holes. The Astrophysical
Journal. 900(2), 148.
mla: Saade, M. Lynne, et al. “Chandra Observations of Candidate Subparsec Binary
Supermassive Black Holes.” The Astrophysical Journal, vol. 900, no. 2,
148, American Astronomical Society, 2020, doi:10.3847/1538-4357/abad31.
short: M.L. Saade, D. Stern, M. Brightman, Z. Haiman, S.G. Djorgovski, D. D’Orazio,
K.E.S. Ford, M.J. Graham, H.D. Jun, R.P. Kraft, B. McKernan, A. Vikhlinin, D.J.
Walton, The Astrophysical Journal 900 (2020).
date_created: 2024-09-05T12:25:06Z
date_published: 2020-09-11T00:00:00Z
date_updated: 2024-09-19T11:29:46Z
day: '11'
doi: 10.3847/1538-4357/abad31
extern: '1'
intvolume: ' 900'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/abad31
month: '09'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Chandra observations of candidate subparsec binary supermassive black holes
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 900
year: '2020'
...
---
_id: '17587'
abstract:
- lang: eng
text: 'The astrophysical origin of gravitational wave (GW) events discovered by
LIGO/VIRGO remains an outstanding puzzle. In active galactic nuclei (AGNs), compact-object
binaries form, evolve, and interact with a dense star cluster and a gas disk.
An important question is whether and how binaries merge in these environments.
To address this question, we have performed one-dimensional N-body simulations
combined with a semianalytical model that includes the formation, disruption,
and evolution of binaries self-consistently. We point out that binaries can form
in single–single interactions through the dissipation of kinetic energy in a gaseous
medium. This "gas-capture" binary formation channel contributes up to 97% of gas-driven
mergers and leads to a high merger rate in AGN disks even without preexisting
binaries. We find the merger rate to be in the range of ∼0.02–60 Gpc−3 yr−1. The
results are insensitive to the assumptions on the gaseous hardening processes:
we find that once they are formed, binaries merge efficiently via binary–single
interactions even if these gaseous processes are ignored. We find that the average
number of mergers per black hole (BH) is 0.4, and the probability for repeated
mergers in 30 Myr is ∼0.21–0.45. High BH masses due to repeated mergers, high
eccentricities, and a significant Doppler drift of GWs are promising signatures
that distinguish this merger channel from others. Furthermore, we find that gas-capture
binaries reproduce the distribution of low-mass X-ray binaries in the Galactic
center, including an outer cutoff at ∼1 pc due to the competition between migration
and hardening by gas torques.'
article_number: '25'
article_processing_charge: No
article_type: original
author:
- first_name: Hiromichi
full_name: Tagawa, Hiromichi
last_name: Tagawa
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Bence
full_name: Kocsis, Bence
last_name: Kocsis
citation:
ama: Tagawa H, Haiman Z, Kocsis B. Formation and evolution of compact-object binaries
in AGN disks. The Astrophysical Journal. 2020;898(1). doi:10.3847/1538-4357/ab9b8c
apa: Tagawa, H., Haiman, Z., & Kocsis, B. (2020). Formation and evolution of
compact-object binaries in AGN disks. The Astrophysical Journal. American
Astronomical Society. https://doi.org/10.3847/1538-4357/ab9b8c
chicago: Tagawa, Hiromichi, Zoltán Haiman, and Bence Kocsis. “Formation and Evolution
of Compact-Object Binaries in AGN Disks.” The Astrophysical Journal. American
Astronomical Society, 2020. https://doi.org/10.3847/1538-4357/ab9b8c.
ieee: H. Tagawa, Z. Haiman, and B. Kocsis, “Formation and evolution of compact-object
binaries in AGN disks,” The Astrophysical Journal, vol. 898, no. 1. American
Astronomical Society, 2020.
ista: Tagawa H, Haiman Z, Kocsis B. 2020. Formation and evolution of compact-object
binaries in AGN disks. The Astrophysical Journal. 898(1), 25.
mla: Tagawa, Hiromichi, et al. “Formation and Evolution of Compact-Object Binaries
in AGN Disks.” The Astrophysical Journal, vol. 898, no. 1, 25, American
Astronomical Society, 2020, doi:10.3847/1538-4357/ab9b8c.
short: H. Tagawa, Z. Haiman, B. Kocsis, The Astrophysical Journal 898 (2020).
date_created: 2024-09-05T12:33:11Z
date_published: 2020-07-20T00:00:00Z
date_updated: 2024-09-19T11:59:23Z
day: '20'
doi: 10.3847/1538-4357/ab9b8c
extern: '1'
intvolume: ' 898'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.3847/1538-4357/ab9b8c
month: '07'
oa: 1
oa_version: Published Version
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Formation and evolution of compact-object binaries in AGN disks
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 898
year: '2020'
...
---
_id: '17596'
abstract:
- lang: eng
text: Binary black hole mergers encode information about their environment and the
astrophysical processes that led to their formation. Measuring the redshift dependence
of their merger rate will help probe the formation and evolution of galaxies and
the evolution of the star formation rate. Here we compute the cosmic evolution
of the merger rate for stellar-mass binaries in the disks of active galactic nuclei
(AGNs). We focus on recent evolution out to redshift z = 2, covering the accessible
range of current Earth-based gravitational-wave observatories. On this scale,
the AGN population density is the main contributor to redshift dependence. We
find that the AGN-assisted merger rate varies by less than a factor of two in
the range 0 < z ≤ 2, comparable to the expected level of evolution for globular
clusters, but much smaller than the order-of-magnitude evolution for field binaries.
article_number: '138'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Y.
full_name: Yang, Y.
last_name: Yang
- first_name: I.
full_name: Bartos, I.
last_name: Bartos
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: B.
full_name: Kocsis, B.
last_name: Kocsis
- first_name: S.
full_name: Márka, S.
last_name: Márka
- first_name: H.
full_name: Tagawa, H.
last_name: Tagawa
citation:
ama: Yang Y, Bartos I, Haiman Z, Kocsis B, Márka S, Tagawa H. Cosmic evolution of
stellar-mass black hole merger rate in active galactic nuclei. The Astrophysical
Journal. 2020;896(2). doi:10.3847/1538-4357/ab91b4
apa: Yang, Y., Bartos, I., Haiman, Z., Kocsis, B., Márka, S., & Tagawa, H. (2020).
Cosmic evolution of stellar-mass black hole merger rate in active galactic nuclei.
The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ab91b4
chicago: Yang, Y., I. Bartos, Zoltán Haiman, B. Kocsis, S. Márka, and H. Tagawa.
“Cosmic Evolution of Stellar-Mass Black Hole Merger Rate in Active Galactic Nuclei.”
The Astrophysical Journal. American Astronomical Society, 2020. https://doi.org/10.3847/1538-4357/ab91b4.
ieee: Y. Yang, I. Bartos, Z. Haiman, B. Kocsis, S. Márka, and H. Tagawa, “Cosmic
evolution of stellar-mass black hole merger rate in active galactic nuclei,” The
Astrophysical Journal, vol. 896, no. 2. American Astronomical Society, 2020.
ista: Yang Y, Bartos I, Haiman Z, Kocsis B, Márka S, Tagawa H. 2020. Cosmic evolution
of stellar-mass black hole merger rate in active galactic nuclei. The Astrophysical
Journal. 896(2), 138.
mla: Yang, Y., et al. “Cosmic Evolution of Stellar-Mass Black Hole Merger Rate in
Active Galactic Nuclei.” The Astrophysical Journal, vol. 896, no. 2, 138,
American Astronomical Society, 2020, doi:10.3847/1538-4357/ab91b4.
short: Y. Yang, I. Bartos, Z. Haiman, B. Kocsis, S. Márka, H. Tagawa, The Astrophysical
Journal 896 (2020).
date_created: 2024-09-05T12:43:28Z
date_published: 2020-06-22T00:00:00Z
date_updated: 2024-09-23T12:59:52Z
day: '22'
doi: 10.3847/1538-4357/ab91b4
extern: '1'
external_id:
arxiv:
- '2003.08564'
intvolume: ' 896'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: ' https://doi.org/10.48550/arXiv.2003.08564'
month: '06'
oa: 1
oa_version: Preprint
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Cosmic evolution of stellar-mass black hole merger rate in active galactic
nuclei
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 896
year: '2020'
...