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Impact of baryonic streaming velocities on the formation of supermassive black holes via direct collapse
Cosmology and Nongalactic Astrophysics · Submitted 22 Nov 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim They also delay the collapse of halos for a few million years, but do not have any significant impact on the halo properties such as turbulent energy, radial velocity, density and accretion rates.
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The abstract, sentence by sentence
Baryonic streaming motions produced prior to the epoch of recombination became supersonic during the cosmic dark ages. Various studies suggest that such streaming velocities change the halo statistics and also influence the formation of Population III stars. In this study, we aim to explore the impact of streaming velocities on the formation of supermassive black holes at $z>10$ via the direct collapse scenario. To accomplish this goal, we perform cosmological large eddy simulations for two halos of a few times $\rm 10^{7} M_{\odot}$ with initial streaming velocities of 3, 6 and 9 $\rm km/s$. These massive primordial halos illuminated by the strong Lyman Werner flux are the potential cradles for the formation of direct collapse seed black holes. To study the evolution for longer times, we employ sink particles and track the accretion for 10,000 years. Our findings show that higher streaming velocities increase the circular velocities from about 14 $\rm km/s$ to 16 $\rm km/s$. They also delay the collapse of halos for a few million years, but do not have any significant impact on the halo properties such as turbulent energy, radial velocity, density and accretion rates. Sink particles of about $\rm \sim 10^5 M_{\odot}$ are formed at the end of our simulations and no clear distribution of sink masses is observed in the presence of streaming motions. It is further found that the impact of streaming velocities is less severe in massive halos compared to the minihalos as reported in the previous studies.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Baryonic streaming motions produced prior to the epoch of recombination became supersonic during the cosmic dark ages. | background 1.00 | 0.05 | 0.02 | asserted 1.00 |
| s1 | Various studies suggest that such streaming velocities change the halo statistics and also influence the formation of Population III stars. | background 1.00 | 0.03 | 0.02 | hedged possibility 1.00 |
| s2 | In this study, we aim to explore the impact of streaming velocities on the formation of supermassive black holes at $z>10$ via the direct collapse scenario. | contribution 0.98 | 0.29 | 0.03 | unclear 0.75 |
| s3 | To accomplish this goal, we perform cosmological large eddy simulations for two halos of a few times $\rm 10^{7} M_{\odot}$ with initial streaming velocities of 3, 6 and 9 $\rm km/s$. | method 0.99 | 0.95 | 0.02 | asserted 0.96 |
| s4 | These massive primordial halos illuminated by the strong Lyman Werner flux are the potential cradles for the formation of direct collapse seed black holes. | background 0.79 | 0.09 | 0.03 | hedged possibility 0.92 |
| s5 | To study the evolution for longer times, we employ sink particles and track the accretion for 10,000 years. | method 1.00 | 0.93 | 0.02 | asserted 0.93 |
| s6 | Our findings show that higher streaming velocities increase the circular velocities from about 14 $\rm km/s$ to 16 $\rm km/s$. | result 1.00 | 0.96 | 0.21 | asserted 1.00 |
| s7 | They also delay the collapse of halos for a few million years, but do not have any significant impact on the halo properties such as turbulent energy, radial velocity, density and accretion rates. | result 1.00 | 0.94 | 0.57 | asserted 1.00 |
| s8 | Sink particles of about $\rm \sim 10^5 M_{\odot}$ are formed at the end of our simulations and no clear distribution of sink masses is observed in the presence of streaming motions. | result 1.00 | 0.96 | 0.08 | asserted 1.00 |
| s9 | It is further found that the impact of streaming velocities is less severe in massive halos compared to the minihalos as reported in the previous studies. | result 0.81 | 0.64 | 0.21 | asserted 0.99 |
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Original abstract
Baryonic streaming motions produced prior to the epoch of recombination became supersonic during the cosmic dark ages. Various studies suggest that such streaming velocities change the halo statistics and also influence the formation of Population III stars. In this study, we aim to explore the impact of streaming velocities on the formation of supermassive black holes at $z>10$ via the direct collapse scenario. To accomplish this goal, we perform cosmological large eddy simulations for two halos of a few times $\rm 10^{7} M_{\odot}$ with initial streaming velocities of 3, 6 and 9 $\rm km/s$. These massive primordial halos illuminated by the strong Lyman Werner flux are the potential cradles for the formation of direct collapse seed black holes. To study the evolution for longer times, we employ sink particles and track the accretion for 10,000 years. Our findings show that higher streaming velocities increase the circular velocities from about 14 $\rm km/s$ to 16 $\rm km/s$. They also delay the collapse of halos for a few million years, but do not have any significant impact on the halo properties such as turbulent energy, radial velocity, density and accretion rates. Sink particles of about $\rm \sim 10^5 M_{\odot}$ are formed at the end of our simulations and no clear distribution of sink masses is observed in the presence of streaming motions. It is further found that the impact of streaming velocities is less severe in massive halos compared to the minihalos as reported in the previous studies.
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2 arXiv papers cite this in 2 sentences
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A number of authors [ref] have studied the effect that streaming velocities can have on the formation of MBH seeds at early times.
Massive Black Holes in Galactic Nuclei · Baryonic Streaming Motions · 0.93
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