The Astrophysical Journal最新文献_第8页

General Relativity Can Prevent a Runaway Greenhouse on Potentially Habitable Planets Orbiting White Dwarfs 广义相对论可以防止围绕白矮星运行的潜在宜居行星上的温室失控

The Astrophysical Journal Pub Date : 2025-10-08 DOI: 10.3847/1538-4357/ae07c6

Eva Stafne and Juliette Becker

引用次数: 0

Confined Circumstellar Material as a Dust Formation Site in Type II Supernovae 受限星周物质作为II型超新星的尘埃形成点

The Astrophysical Journal Pub Date : 2025-10-08 DOI: 10.3847/1538-4357/ae0466

Yuki Takei, Kunihito Ioka and Masaru Shibata

{"title":"Confined Circumstellar Material as a Dust Formation Site in Type II Supernovae","authors":"Yuki Takei, Kunihito Ioka and Masaru Shibata","doi":"10.3847/1538-4357/ae0466","DOIUrl":"https://doi.org/10.3847/1538-4357/ae0466","url":null,"abstract":"We propose a model for dust formation in Type II supernovae (SNe) interacting with confined circumstellar material (CSM), motivated by recent time-domain surveys that have revealed a substantial fraction of SN progenitors to be surrounded by CSM ejected shortly before core collapse. We simulate the pre-SN mass eruption and the resulting confined CSM using the open-source code CHIPS, and follow the subsequent evolution of the SN ejecta and its interaction with the CSM. We show that a cold dense shell (CDS) is formed at the radiative shock under a wide range of conditions and later undergoes rapid adiabatic cooling during free expansion, leading to efficient dust condensation. The resulting dust mass ranges from ∼10−3M⊙ to 0.1 M⊙, depending on the mass and spatial extent of the CSM. We further calculate the infrared (IR) emission from the newly formed dust and find broad consistency with observations of SN 1998S. Notably, the IR light curve exhibits a rapid rise within ≲10 days, closely resembling that of kilonovae (KNe). This suggests that dust emission powered by confined CSM interaction may be also discovered in KN searches. Moreover, the high-density environment of the CDS may allow dust grains to grow to larger sizes, enhancing their survivability against destruction by reverse shocks propagating from the interstellar medium at later times.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145246691","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Cosmic-Ray Mass Composition around the Knee via Principal Component Analysis 通过主成分分析得出的膝关节周围宇宙射线质量组成

The Astrophysical Journal Pub Date : 2025-10-08 DOI: 10.3847/1538-4357/ae09a9

Nicusor Arsene

{"title":"Cosmic-Ray Mass Composition around the Knee via Principal Component Analysis","authors":"Nicusor Arsene","doi":"10.3847/1538-4357/ae09a9","DOIUrl":"https://doi.org/10.3847/1538-4357/ae09a9","url":null,"abstract":"In this paper, we apply principal component analysis (PCA) to experimental data recorded by the KASCADE experiment to reconstruct the mass composition of cosmic rays around the knee region. A set of four extensive air shower parameters sensitive to the primary particle mass (LCm, Nμ, Ne, and lateral shower age) was considered, whose coordinates were transformed into a new orthogonal basis that maximally captures the data variance. Based on the experimental distributions of the first two principal components (PCA0 versus PCA1) and full Monte Carlo simulations of the KASCADE array considering five types of primary particles (p, He, C, Si, and Fe) and three hadronic interaction models (EPOS-LHC, QGSjet-II-04, and SIBYLL 2.3d), we obtained the evolution of the abundance of each primary species as a function of energy, as well as the evolution of the mean logarithmic mass with energy. We found that the reconstruction of the mass composition resulting from this comprehensive analysis significantly reduces dependence on the hadronic interaction model used in the simulation process, even though the initial input parameters are model dependent. Moreover, the results support the idea that around the knee region, the abundance of the light component (protons) decreases, while the heavy component shows a slight increase. The evolution of as a function of energy derived from this analysis shows excellent agreement with recent results from the LHAASO–KM2A experiment and aligns very well with the predictions of the data-driven Global Spline Fit model.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"106 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145246740","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries 用盖亚RVs探测恒星双星的统计框架。1 .对未解决二进制的敏感性

The Astrophysical Journal Pub Date : 2025-10-08 DOI: 10.3847/1538-4357/adfb68

Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David and Adrian M. Price-Whelan

{"title":"paired: A Statistical Framework for Detecting Stellar Binarity with Gaia RVs. I. Sensitivity to Unresolved Binaries","authors":"Quadry Chance, Daniel Foreman-Mackey, Sarah Ballard, Andrew R. Casey, Trevor J. David and Adrian M. Price-Whelan","doi":"10.3847/1538-4357/adfb68","DOIUrl":"https://doi.org/10.3847/1538-4357/adfb68","url":null,"abstract":"Data Release 3 (DR3) from the Gaia Mission includes radial velocity measurements of over 33 million targets. Among many scientific applications, the overlap of this stellar sample with targeted exoplanet transit survey stars presents an opportunity to understand planet occurrence in the context of stellar multiplicity on a large scale. Yet, any interpretation of occurrence relies upon an understanding of survey sensitivity. While the sensitivity to planets in transit surveys is well-understood, a characterization of the sensitivity of Gaia to unresolved binaries is also critical. We describe here a statistical framework called paired, which we developed to enable the forward modeling of Gaia radial velocity observables for large samples of stars. The paired machinery links the reported radial velocity noise for a given star from Gaia to the probability of a spatially unresolved stellar companion. We demonstrate how this enables the user, given an observed distribution of individual binary “probabilities” for a set of stars, to understand this distribution within the sensitivity limits of Gaia. For the subset of stars with the highest probability of excess radial velocity noise, we describe the ability of paired to constrain the semi-amplitude of the stellar binary. Where possible, we benchmark our inferred radial velocity semi-amplitudes against those from ground-based radial velocity surveys, as well as the subset published by Gaia DR3 itself. We aim for paired to be a community tool for the exploration of the effects of binarity on planets at a population level, but also for any user interested in stellar populations.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"29 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145246775","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Spectral Properties of Globally Distributed ENA Fluxes across Diverse Regions of the Heliosphere 日球层不同区域全球分布的ENA通量的光谱特性

The Astrophysical Journal Pub Date : 2025-10-08 DOI: 10.3847/1538-4357/ae0183

Thomas K. Kim, Daniel B. Reisenfeld, Eric J. Zirnstein, Paul H. Janzen, Asher S. Merrill, Sung Jun Noh, Nehpreet K. Walia, Yue Chen, Fan Guo, Dave Osthus, Lauren J. Beesley, Dae-Kyu Shin, Justyna M. Sokół, Maciej Bzowski, Marzena A. Kubiak, Czeslaw Porowski and Herbert O. Funsten

{"title":"Spectral Properties of Globally Distributed ENA Fluxes across Diverse Regions of the Heliosphere","authors":"Thomas K. Kim, Daniel B. Reisenfeld, Eric J. Zirnstein, Paul H. Janzen, Asher S. Merrill, Sung Jun Noh, Nehpreet K. Walia, Yue Chen, Fan Guo, Dave Osthus, Lauren J. Beesley, Dae-Kyu Shin, Justyna M. Sokół, Maciej Bzowski, Marzena A. Kubiak, Czeslaw Porowski and Herbert O. Funsten","doi":"10.3847/1538-4357/ae0183","DOIUrl":"https://doi.org/10.3847/1538-4357/ae0183","url":null,"abstract":"This study analyzes energetic neutral atom (ENA) spectral properties across distinct regions of globally distributed flux (GDF) sky maps, using Interstellar Boundary Explorer data from a full solar cycle, corrected for time dispersion. By time-shifting the data to the heliosheath using GDF source distances from D. B. Reisenfeld et al., we achieve a more accurate representation of heliosheath GDF energy spectra. We quantify ENA spectral characteristics, heliosheath line-of-sight-integrated proton pressure, and heliosheath proton temperature, comparing these to solar wind properties at 1 au and interplanetary scintillation-derived solar wind data. Our findings show that the spectral index is generally anticorrelated with heliosheath proton temperature and pressure, except in the central tail, where a partial positive correlation is observed. The lowest spectral index values occur when high-latitude heliosheath regions are dominated by fast solar wind from polar coronal holes. The south pole exhibits the flattest energy spectra due to plasma heating from both fast solar wind and a late-2014 pressure pulse. The central tail shows shorter variability (5–6 yr) for spectral index and heliosheath proton temperature, while proton pressure follows the 11 yr solar cycle. Most spectral shapes exhibit a “knee” distribution, peaking during solar maximum, with an “ankle” shape observed only at the south pole during solar cycle transitions. Asymmetry in proton pressure in the lobes is driven by the draping effect of the local interstellar magnetic field. This study provides insights into the energetic properties of GDF across the heliosphere, enhancing our understanding of the heliospheric environment.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"101 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145246681","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Testing the Young Fast Radio Burst Progenitor Hypothesis: A Crossmatch of Catalog-1 CHIME Bursts with Historic Local Universe Supernovae 验证年轻的快速射电暴祖先假说：目录-1 CHIME爆发与历史上的局部宇宙超新星的交叉匹配

The Astrophysical Journal Pub Date : 2025-10-08 DOI: 10.3847/1538-4357/adff5c

Wanqing Liu, Mohit Bhardwaj and Ben Margalit

{"title":"Testing the Young Fast Radio Burst Progenitor Hypothesis: A Crossmatch of Catalog-1 CHIME Bursts with Historic Local Universe Supernovae","authors":"Wanqing Liu, Mohit Bhardwaj and Ben Margalit","doi":"10.3847/1538-4357/adff5c","DOIUrl":"https://doi.org/10.3847/1538-4357/adff5c","url":null,"abstract":"Fast radio bursts (FRBs) are among the most energetic and enigmatic transients in the radio sky, with mounting evidence suggesting newborn, highly magnetized neutron stars formed in core-collapse supernovae (CCSNe) as their sources. A definitive spatial association between an FRB and a historic CCSN would confirm this link and tightly constrain young neutron-star source models. Here we report on the first systematic crossmatching of 886 spectroscopically classified CCSNe in the local Universe (z ≤ 0.043) against 241 CHIME/FRB Catalog 1 events, applying rigorous spatial, dispersion measure (DM), and scattering time (τ) criteria. We identify four positional overlaps, all consistent with a chance alignment; however, one pair, FRB 20190412B–SN 2009gi, also satisfies independent host-DM and τ constraints, making it a promising candidate for targeted follow-up. Next, we search for compact (persistent or transient) radio emission at all matched supernova sites using multiepoch Very Large Array Sky Survey data and detect none. Treating every CCSN sight line as a nondetection, we derive Poisson upper limits on the FRB burst rate at these locations, which lie well below the rates observed for the most active repeaters unless their activity is heavily suppressed by beaming, intermittency, or residual free–free absorption. We then develop a galaxy-integrated FRB-rate model that incorporates an intrinsic spectral index, secular magnetar-activity decay, and frequency-dependent free–free opacity. Applying this formalism to existing FRB data shows that reproducing the observed CHIME/CRAFT all-sky rate ratio requires a steep decline in magnetar burst rate with age. Finally, our work underscores the necessity of subarcsecond localizations and multiwavelength follow-up to definitively test the young neutron star source hypothesis.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"24 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145246637","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A Detection of Helium in the Bright Superluminous Supernova SN 2024rmj 超亮超新星SN 2024rmj中氦的探测

The Astrophysical Journal Pub Date : 2025-10-08 DOI: 10.3847/1538-4357/adff7e

Harsh Kumar, Edo Berger, Peter K. Blanchard, Daichi Hiramatsu, Sebastian Gomez, Alex Gagliano, Moira Andrews, K. Azalee Bostroem, Joseph Farah, D. Andrew Howell and Curtis McCully

{"title":"A Detection of Helium in the Bright Superluminous Supernova SN 2024rmj","authors":"Harsh Kumar, Edo Berger, Peter K. Blanchard, Daichi Hiramatsu, Sebastian Gomez, Alex Gagliano, Moira Andrews, K. Azalee Bostroem, Joseph Farah, D. Andrew Howell and Curtis McCully","doi":"10.3847/1538-4357/adff7e","DOIUrl":"https://doi.org/10.3847/1538-4357/adff7e","url":null,"abstract":"We present extensive ultraviolet, optical, and near-infrared (NIR) photometric and spectroscopic observations of the nearby hydrogen-poor superluminous supernova (SLSN-I) SN 2024rmj at z = 0.1189. SN 2024rmj reached a peak absolute magnitude of Mg ≈ −21.9, placing it at the luminous end of the SLSN-I distribution. The light curve exhibits a pronounced prepeak bump (≈60 days before the main peak) and a postpeak bump (≈55 days after the main peak). The bulk of the light curve is otherwise well fit by a magnetar spin-down model, with typical values (spin: ≈2.1 ms; magnetic field: ≈6 × 1013 G; ejecta mass: ≈12 M⊙). The optical spectra exhibit characteristic SLSN-I features and evolution, but with a relatively high velocity of ≈8000 km s−1 postpeak. Most significantly, we find a clear detection of helium in the NIR spectra at He iλ1.083 μm and λ2.058 μm, blueshifted by ≈15,000 km s−1 (13 days before peak) and ≈13,000 km s−1 (40 days after peak), indicating that helium is confined to the outermost ejecta; based on these NIR detections, we also identify likely contribution from He iλ5876 in the optical spectra on a similar range of timescales. This represents the most definitive detection of helium in a bright SLSN-I to date, and indicates that progenitors with a thin helium layer can still explode as SLSNe.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"19 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145246682","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries? Ap/Bp星的异常磁制动能否解释algol型双星的轨道衰变？

The Astrophysical Journal Pub Date : 2025-10-08 DOI: 10.3847/1538-4357/ae0331

Guan-Long Wu, Zhao-Yu Zuo and Wen-Cong Chen

{"title":"Can the Anomalous Magnetic Braking of Ap/Bp Stars Explain the Orbital Decay of Algol-type Binaries?","authors":"Guan-Long Wu, Zhao-Yu Zuo and Wen-Cong Chen","doi":"10.3847/1538-4357/ae0331","DOIUrl":"https://doi.org/10.3847/1538-4357/ae0331","url":null,"abstract":"Several Algol-type binaries were detected to be experiencing rapid orbital decay, which is in contradiction with the conservative mass transfer model. In this work, we investigate whether anomalous magnetic braking (MB) of intermediate-mass Ap/Bp stars, characterized by surface magnetic fields of ∼102–104 G, could drive orbital decay through magnetic wind–field coupling. Using the stellar evolution code MESA, we simulate the evolution of several main-sequence binaries containing Ap/Bp stars, with typical initial parameters of Algol binaries. Our models indicate that the anomalous MB mechanism could induce orbital decay in long timescales (hundreds of Myr to several Gyr), reproducing several basic Algol parameters such as the effective temperatures and luminosities of donor stars. However, the predicted orbital period decay rates are much lower than those observed in several Algol systems. We analyze the limitations of the anomalous MB model and discuss alternative mechanisms that could account for the long- or short-term orbital period variations observed in Algol systems, including a surrounding circumbinary disk, stellar expansion, the Applegate mechanism, and the light-travel-time effect. Long-term observations are still required to distinguish between these mechanisms in the future.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"33 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145246689","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST 用FAST研究毫秒脉冲星B1937+21的星际闪烁

The Astrophysical Journal Pub Date : 2025-10-08 DOI: 10.3847/1538-4357/ae0452

Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen and Chengbing Lyu

{"title":"Investigation of Interstellar Scintillation of the Millisecond Pulsar B1937+21 with the FAST","authors":"Zhigang Wen, Hui Wang, Zhen Wang, Jianping Yuan, Na Wang, Wenming yan, Wei Han, Xuefeng Duan, Honguang Wang, Pengcheng He, Jianling Chen and Chengbing Lyu","doi":"10.3847/1538-4357/ae0452","DOIUrl":"https://doi.org/10.3847/1538-4357/ae0452","url":null,"abstract":"Pulsar scintillation serves as a valuable tool for investigating interstellar scattering screens and their properties. In this paper, we report on multiepoch interstellar scintillation from the millisecond pulsar B1937+21 (J1939+2134) using Five-hundred-meter Aperture Spherical radio Telescope (FAST) observations at 1250 MHz with 500 MHz bandwidth. The diffractive scintillation properties are investigated for an observing baseline of 3 yr. The scintillation timescale, exponential index, and decorrelation bandwidth are determined to be 7.67 ± 1.61 minutes, 1.54 ± 0.09, and 0.56 ± 0.25 MHz, respectively, from the autocorrelation functions of the dynamic spectra. These scintillation parameters are found to vary temporally. The frequency dependencies of scintillation parameters exhibit single-power spectral behaviors; however, the derived spectral indices deviate from the theoretical Kolmogorov spectrum. The fringe pattern that forms from interference of scattered waves is revealed in the secondary spectrum as a parabolic arc with a well-determined curvature of 0.95 ± 0.50 s3. The parabolic arc is present contemporaneously over a wide frequency range and scales with frequency as a power law with an index of −0.80 ± 0.18, indicating the broadband nature of the scintillation arc. The arc curvature exhibits annual variation and is well approximated by a one-dimensional scattering screen located approximately 95% of the distance toward the pulsar. These findings will contribute to a deeper understanding of the underlying physics of the ionized interstellar medium.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"15 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145246690","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A Novel Formation Channel for Supermassive Black Hole Binaries in the Early Universe via Primordial Black Holes 通过原始黑洞形成早期宇宙中超大质量黑洞双星的新通道

The Astrophysical Journal Pub Date : 2025-10-08 DOI: 10.3847/1538-4357/ae061c

Saiyang Zhang, Boyuan Liu and Volker Bromm

{"title":"A Novel Formation Channel for Supermassive Black Hole Binaries in the Early Universe via Primordial Black Holes","authors":"Saiyang Zhang, Boyuan Liu and Volker Bromm","doi":"10.3847/1538-4357/ae061c","DOIUrl":"https://doi.org/10.3847/1538-4357/ae061c","url":null,"abstract":"We present a novel formation channel for supermassive black hole (SMBH) binaries in the early Universe, driven by primordial black holes (PBHs). Using high-resolution hydrodynamical simulations, we explore the role of massive PBHs (mBH ∼ 106M⊙) in catalyzing the formation of direct-collapse black holes (DCBHs), providing a natural in situ pathway for binary SMBH formation. PBHs enhance local overdensities, accelerate structure formation, and exert thermal feedback on the surrounding medium via accretion. Lyman–Werner radiation from accreting PBHs suppresses H2 cooling, shifting the dominant gas coolant to atomic hydrogen. When combined with significant baryon–dark matter streaming velocities (vbχ ≳ 0.8σbχ, where σbχ is the rms streaming velocity), these effects facilitate the formation of dense, gravitationally unstable atomically cooling gas clouds in the PBH’s wake. These clouds exhibit sustained high inflow rates ( yr−1), providing ideal conditions for DCBH formation from rapidly growing supermassive stars of ∼105M⊙ at redshift z ∼ 20–10. The resulting systems form SMBH binaries with initial mass ratios and separations of ∼10 pc. Such PBH-DCBH binaries provide testable predictions for JWST and Atacama Large Millimeter/submillimeter Array, potentially explaining select high-z sources like little red dots, and represent gravitational-wave sources for future missions like LISA and TianQin—bridging early-Universe black hole physics, multimessenger astronomy, and dark matter theory.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-10-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145246727","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0