Monthly Notices of the Royal Astronomical Society最新文献_第6页

A Systematic Study of Planetary Envelope Growth with 3D Radiation-Hydrodynamics Simulations 利用三维辐射流体力学模拟对行星包层生长的系统研究

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2126

Avery Bailey, James M Stone, Jeffrey Fung

{"title":"A Systematic Study of Planetary Envelope Growth with 3D Radiation-Hydrodynamics Simulations","authors":"Avery Bailey, James M Stone, Jeffrey Fung","doi":"10.1093/mnras/stae2126","DOIUrl":"https://doi.org/10.1093/mnras/stae2126","url":null,"abstract":"In the core accretion model of planet formation, envelope cooling regulates the accretion of material and ultimately sets the timescale to form a giant planet. Given the diversity of planet-forming environments, opacity uncertainties, and the advective transport of energy by 3-dimensional recycling flows, it is unclear whether 1D models can adequately describe envelope structure and accretion in all regimes. Even in 3D models, it is unclear whether approximate radiative transfer methods sufficiently model envelope cooling particularly at the planetary photosphere. To address these uncertainties, we present a suite of 3D radiation hydrodynamics simulations employing methods that directly solve the transfer equation. We perform a parameter space study, formulated in terms of dimensionless parameters, for a variety of envelope optical depths and cooling times. We find that the thermodynamic structure of the envelope ranges from adiabatic to isothermal based on the cooling time and by extension, the background disk temperature and density. By adopting a dimensionless framework, these models can be applied to a wide range of formation conditions and assumed opacities. In particular, we dimensionalize them to the case of a super-Earth and proto-Jupiter and place upper limits on the 3D mass accretion rates prior to runaway growth. Finally, we evaluate the fidelity of approximate radiative transfer methods and find that even in the most challenging cases, more approximate methods are sufficiently accurate and worth their savings in computational cost.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"17 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256117","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Unfruitful chemical pathway for interstellar furan: formation of the four isomers of 1-butenol-3-yne 星际呋喃的不成功化学途径：1-丁烯-3-炔的四种异构体的形成

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2118

J García de la Concepción, V M Rivilla

{"title":"Unfruitful chemical pathway for interstellar furan: formation of the four isomers of 1-butenol-3-yne","authors":"J García de la Concepción, V M Rivilla","doi":"10.1093/mnras/stae2118","DOIUrl":"https://doi.org/10.1093/mnras/stae2118","url":null,"abstract":"Heterocycles have not been detected in the interstellar medium (ISM) yet. However, the direct involvement of some pentagonal heterocycles within the formation of key biomolecules for the origin of life makes the search for these systems in the ISM relevant for understanding whether some of the bricks of life could be formed in the ISM. We have explored the possible formation of the simple heterocycle furan (c-C4H4O) under interstellar conditions, through the reaction between two interstellar species, syn-vinyl alcohol (syn-VA) and the CCH radical. We employed state-of-the-art quantum-chemical calculations to elucidate the reaction mechanism between the reaction of CCH radical and syn-VA. Kinetic simulations were carried out aiming to quantitatively assess the viability of this reaction in the ISM. We have found a reaction pathway to furan where all energy barriers are submerged. However, the formation of this heterocycle is not feasible because the intermediates leading to furan can evolve through more favourable routes. In contrast, we have found viable pathways for the formation of the four isomers of 1-butenol-3-yne (HCCCHCHOH) (Z-syn, E-syn, E-anti and Z-anti), which thus are promising species to be detected in the ISM. Our theoretical work indicates that the four isomers of 1-butenol-3-yne should be present in the ISM, because the precursors are known interstellar species, and the kinetic simulations indicates that their formation is very likely. We then encourage the observational search of these molecules in the ISM.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"23 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256118","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Multi-messenger signatures of delayed choked jets in tidal disruption events 潮汐扰动事件中延迟窒息射流的多信使特征

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2080

Mainak Mukhopadhyay, Mukul Bhattacharya, Kohta Murase

{"title":"Multi-messenger signatures of delayed choked jets in tidal disruption events","authors":"Mainak Mukhopadhyay, Mukul Bhattacharya, Kohta Murase","doi":"10.1093/mnras/stae2080","DOIUrl":"https://doi.org/10.1093/mnras/stae2080","url":null,"abstract":"Recent radio observations and coincident neutrino detections suggest that some tidal disruption events (TDEs) exhibit late-time activities, relative to the optical ehmission peak, and these may be due to delayed outflows launched from the central supermassive black hole. We investigate te possibility that jets launched with a time delay of days to months, interact with a debris that may expand outwards. We discuss the effects of the time delay and expansion velocity on the outcomes of jet breakout and collimation. We find that a jet with an isotropic-equivalent luminosity of ≲ 5 × 1045 erg/s is likely to be choked for a delay time of ∼3 months. We also study the observational signatures of such delayed choked jets. The jet-debris interaction preceding the breakout would lead to particle acceleration and the resulting synchrotron emission can be detected by current and near-future radio, optical and X-ray telescopes, and the expanding jet-driven debris could explain late-time radio emission. We discuss high-energy neutrino production in delayed choked jets, and the time delay can significantly alleviate the difficulty of the hidden jet scenario in explaining neutrino coincidences.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"44 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256125","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The PIPER survey. II. The globular cluster systems of low surface brightness galaxies in the perseus cluster PIPER 调查。II.perseus星团中低表面亮度星系的球状星团系统

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2137

Steven R Janssens, Duncan A Forbes, Aaron J Romanowsky, Jonah Gannon, Joel Pfeffer, Warrick J Couch, Jean P Brodie, William E Harris, Patrick R Durrell, Kenji Bekki

{"title":"The PIPER survey. II. The globular cluster systems of low surface brightness galaxies in the perseus cluster","authors":"Steven R Janssens, Duncan A Forbes, Aaron J Romanowsky, Jonah Gannon, Joel Pfeffer, Warrick J Couch, Jean P Brodie, William E Harris, Patrick R Durrell, Kenji Bekki","doi":"10.1093/mnras/stae2137","DOIUrl":"https://doi.org/10.1093/mnras/stae2137","url":null,"abstract":"We present Hubble Space Telescope ACS/WFC and WFC3/UVIS imaging for a sample of 50 low surface brightness (LSB) galaxies in the ∼1015 M⊙ Perseus cluster, which were originally identified in ground-based imaging. We measure the structural properties of these galaxies and estimate the total number of globular clusters (GCs) they host. Around half of our sample galaxies meet the strict definition of an ultra-diffuse galaxy (UDG), while the others are UDG-like but are either somewhat more compact or slightly brighter. A small number of galaxies reveal systems with many tens of GCs, rivalling some of the richest GC systems known around UDGs in the Coma cluster. We find the sizes of rich GC systems, in terms of their half-number radii, extending to ∼1.2 times the half-light radii of their host galaxy on average. The mean colours of the GC systems are the same, within the uncertainties, as those of their host galaxy stars. This suggests that GCs and galaxy field stars may have formed at the same epoch from the same enriched gas. It may also indicate a significant contribution from disrupted GCs to the stellar component of the host galaxy as might be expected in the ‘failed galaxy’ formation scenario for UDGs.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"1 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256201","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

A calibrated model for N-body dynamical friction acting on supermassive black holes 作用于超大质量黑洞的 N-body 动力摩擦校准模型

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2144

Anna Genina, Volker Springel, Antti Rantala

{"title":"A calibrated model for N-body dynamical friction acting on supermassive black holes","authors":"Anna Genina, Volker Springel, Antti Rantala","doi":"10.1093/mnras/stae2144","DOIUrl":"https://doi.org/10.1093/mnras/stae2144","url":null,"abstract":"Black holes are believed to be crucial in regulating star formation in massive galaxies, which makes it essential to faithfully represent the physics of these objects in cosmological hydrodynamics simulations. Limited spatial and mass resolution and the associated discreteness noise make following the dynamics of black holes especially challenging. In particular, dynamical friction, which is responsible for driving massive black holes towards the centres of galaxies, cannot be accurately modelled with softened N-body interactions. A number of subgrid models have been proposed to mimic dynamical friction or directly include its full effects in simulations. Each of these methods has its individual benefits and shortcomings, while all suffer from a common issue of being unable to represent black holes with masses below a few times the simulated dark matter particle mass. In this paper, we propose a correction for unresolved dynamical friction, which has been calibrated on simulations run with the code KETJU, in which gravitational interactions of black holes are not softened. We demonstrate that our correction is able to sink black holes with masses greater than the dark matter particle mass at the correct rate. We show that the impact of stochasticity is significant for low-mass black holes (MBH ≤ 5MDM) and propose a correction for stochastic heating. Combined, this approach is applicable to next generation cosmological hydrodynamics simulations that jointly track galaxy and black hole growth with realistic black hole orbits.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"54 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256116","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The only inflated brown dwarf in an eclipsing white dwarf–brown dwarf binary: WD1032+011B 食白矮星-褐矮星双星中唯一的膨胀褐矮星：WD1032+011B

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2121

Jenni R French, Sarah L Casewell, Rachael C Amaro, Joshua D Lothringer, L C Mayorga, Stuart P Littlefair, Ben W P Lew, Yifan Zhou, Daniel Apai, Mark S Marley, Vivien Parmentier, Xianyu Tan

{"title":"The only inflated brown dwarf in an eclipsing white dwarf–brown dwarf binary: WD1032+011B","authors":"Jenni R French, Sarah L Casewell, Rachael C Amaro, Joshua D Lothringer, L C Mayorga, Stuart P Littlefair, Ben W P Lew, Yifan Zhou, Daniel Apai, Mark S Marley, Vivien Parmentier, Xianyu Tan","doi":"10.1093/mnras/stae2121","DOIUrl":"https://doi.org/10.1093/mnras/stae2121","url":null,"abstract":"Due to their short orbital periods and relatively high flux ratios, irradiated brown dwarfs in binaries with white dwarfs offer better opportunities to study irradiated atmospheres than hot Jupiters, which have lower planet-to-star flux ratios. WD1032+011 is an eclipsing, tidally locked white dwarf–brown dwarf binary with a 9950 K white dwarf orbited by a 69.7 MJup brown dwarf in a 0.09 day orbit. We present time-resolved Hubble Space Telescope Wide Field Camera 3 spectrophotometric data of WD1032+011. We isolate the phase-dependent spectra of WD1032+011B, finding a 210 K difference in brightness temperature between the dayside and nightside. The spectral type of the brown dwarf is identified as L1 peculiar, with atmospheric retrievals and comparison to field brown dwarfs showing evidence for a cloud-free atmosphere. The retrieved temperature of the dayside is 1748$^{+66}_{-67}$ K, with a nightside temperature of 1555$^{+76}_{-62}$ K, showing an irradiation-driven temperature contrast coupled with inefficient heat redistribution from the dayside to the nightside. The brown dwarf radius is inflated, likely due to the constant irradiation from the white dwarf, making it the only known inflated brown dwarf in an eclipsing white dwarf–brown dwarf binary.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"16 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256121","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Selection functions of strong lens finding neural networks 强透镜搜索神经网络的选择功能

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2106

A Herle, C M O’Riordan, S Vegetti

{"title":"Selection functions of strong lens finding neural networks","authors":"A Herle, C M O’Riordan, S Vegetti","doi":"10.1093/mnras/stae2106","DOIUrl":"https://doi.org/10.1093/mnras/stae2106","url":null,"abstract":"We show that Convolution Neural Networks trained to find strong gravitational lens systems are biased towards systems with larger Einstein radii and large concentrated sources. This selection function is key to fully realising the potential of the large samples of strong gravitational lens systems that will be found in upcoming wide-field surveys. In this paper, we use a CNN and three training datasets to quantify the network selection function and its implication for the many scientific applications of strong gravitational lensing. We use CNNs with similar architecture as is commonly found in the literature. The networks preferentially select systems with larger Einstein radii and larger sources with more concentrated source-light distributions. Increasing the detection significance threshold to 12σ from 8σ results in 50percnt of the selected strong lens systems having Einstein radii θE ≥ 1.04 arcsec from θE ≥ 0.879 arcsec, source radii RS ≥ 0.194 arcsec from RS ≥ 0.178 arcsec and source Sérsic indices $n_{mathrm{Sc}}^{mathrm{S}}$ ≥ 2.62 from $n_{mathrm{Sc}}^{mathrm{S}}$ ≥ 2.55. The model trained to find lensed quasars shows a stronger preference for higher lens ellipticities than those trained to find lensed galaxies. The selection function is independent of the slope of the power-law of the mass profiles, hence measurements of this quantity will be unaffected. The lens finder selection function reinforces that of the lensing cross-section, and thus we expect our findings to be a general result for all galaxy-galaxy and galaxy-quasar lens finding neural networks.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"17 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256124","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Influence of the lense-thirring effect on stellar orbits around a spinning supermassive black hole 围绕旋转超大质量黑洞的恒星轨道的光栅-旋光效应的影响

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2123

Yashvardhan Tomar, Cuc Dinh, Gongjie Li, Douglas Lin

{"title":"Influence of the lense-thirring effect on stellar orbits around a spinning supermassive black hole","authors":"Yashvardhan Tomar, Cuc Dinh, Gongjie Li, Douglas Lin","doi":"10.1093/mnras/stae2123","DOIUrl":"https://doi.org/10.1093/mnras/stae2123","url":null,"abstract":"Rotating super-massive black holes drive Lense-Thirring effects, which induce orbit nodal and eccentricity vector precession in their vicinity. Typically, these relativistic effects are quite small, but for the case of close-in orbits that are additionally perturbed by an outer intermediate mass companion (IMC), we show that the Lense-Thirring effects can lead to markedly different dynamical behaviour. Using REBOUND N-body simulations, we show that resonances occur considering both the Lense-Thirring effect and secular perturbations from the IMC, and it can excite the inclination of the orbits, an order of magnitude higher than that achieved solely due to secular three-body effects. We also examine the sensitivity of the inclination growth on the profile of the IMC and find that the excitation is highest for a companion to SMBH mass ratio of 1:1000 and for companions that orbit the SMBH on closer-in orbits. In addition, we investigate how varying the spin direction of the SMBH affects the inclination of the orbits. We find no excitation in the eccentricity of the orbits since the resonance is on the nodal angle, and the fast precession suppresses Kozai cycles. Finally, we note how the Lense-Thirring effect reduces the stability of the three-body system, enhancing the scattering rate between the test particles and the IMC, and thus making disruption events more likely in the system.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"12 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256159","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

The LOFAR two metre sky survey data release 2: probabilistic spectral source classifications and faint radio source demographics LOFAR 两米巡天数据第 2 版：概率光谱源分类和暗射电源人口统计

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2117

A B Drake, D J B Smith, M J Hardcastle, P N Best, R Kondapally, M I Arnaudova, S Das, S Shenoy, K J Duncan, H J A Röttgering, C Tasse

{"title":"The LOFAR two metre sky survey data release 2: probabilistic spectral source classifications and faint radio source demographics","authors":"A B Drake, D J B Smith, M J Hardcastle, P N Best, R Kondapally, M I Arnaudova, S Das, S Shenoy, K J Duncan, H J A Röttgering, C Tasse","doi":"10.1093/mnras/stae2117","DOIUrl":"https://doi.org/10.1093/mnras/stae2117","url":null,"abstract":"We present an analysis of 152,355 radio sources identified in the second data release of the LOFAR Two Metre Sky Survey (LoTSS-DR2) with Sloan Digital Sky Survey (SDSS) spectroscopic redshifts in the range 0.00 &lt; z &lt; 0.57. Using Monte Carlo simulations we determine the reliability of each source exhibiting an excess in radio luminosity relative to that predicted from their Hα emission, and, for a subset of 124,023 sources we combine this measurement with a full BPT analysis. Using these two independent diagnostics we determine the reliability of each source hosting a supermassive black hole of high or low Eddington-scaled accretion rate, and combine the measurements to determine the reliability of sources belonging to each of four physical classes of objects: star forming galaxies (SFGs), radio-quiet active galactic nuclei (RQAGN), and high- or low-excitation radio galaxies (HERGs or emission-line LERGs). The result is a catalogue which enables user-defined samples of radio sources with a reliability threshold suited to their science goal e.g. prioritising purity or completeness. Here we select high-confidence samples of radio sources (&gt;90% reliability) to report: 38,588 radio-excess AGN in the LoTSS DR2 sample (362 HERGs, and 12,648 emission-line LERGs), together with 38,729 SFGs, and 18,726 RQAGN. We validate these results through comparison to literature using independent emission-line measurements, and to widely-adopted WISE photometric selection techniques. While our use of SDSS spectroscopy limits our current analysis to ∼4 percent of the LoTSS-DR2 catalogue, our method is directly applicable to data from the forthcoming WEAVE-LOFAR survey which will obtain over a million spectra of 144 MHz selected sources.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"54 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256120","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Gravitational waves from mergers of Population III binary black holes: roles played by two evolution channels 来自种群 III 双黑洞合并的引力波：两个演化通道的作用

IF 4.8 3区物理与天体物理

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-09-13 DOI: 10.1093/mnras/stae2120

Boyuan Liu, Tilman Hartwig, Nina S Sartorio, Irina Dvorkin, Guglielmo Costa, Filippo Santoliquido, Anastasia Fialkov, Ralf S Klessen, Volker Bromm

{"title":"Gravitational waves from mergers of Population III binary black holes: roles played by two evolution channels","authors":"Boyuan Liu, Tilman Hartwig, Nina S Sartorio, Irina Dvorkin, Guglielmo Costa, Filippo Santoliquido, Anastasia Fialkov, Ralf S Klessen, Volker Bromm","doi":"10.1093/mnras/stae2120","DOIUrl":"https://doi.org/10.1093/mnras/stae2120","url":null,"abstract":"The gravitational wave (GW) signal from binary black hole (BBH) mergers is a promising probe of Population III (Pop III) stars. To fully unleash the power of the GW probe, one important step is to understand the relative importance and features of different BBH evolution channels. We model two channels, isolated binary stellar evolution (IBSE) and nuclear star cluster-dynamical hardening (NSC-DH), in one theoretical framework based on the semi-analytical code a-sloth, under various assumptions on Pop III initial mass function (IMF), initial binary statistics and high-z nuclear star clusters (NSCs). The NSC-DH channel contributes $sim 8-95{{%}}$ of Pop III BBH mergers across cosmic history, with higher contributions achieved by initially wider binary stars, more top-heavy IMFs, and more abundant high-z NSCs. The dimensionless stochastic GW background (SGWB) produced by Pop III BBH mergers has peak values $Omega ^{rm peak}_{rm GW}sim 10^{-11}-8times 10^{-11}$ around observer-frame frequencies $nu sim 10-100 rm Hz$. The Pop III contribution can be a non-negligible ($sim 2-32{{%}}$) component in the total SGWB at $nu lesssim 10 rm Hz$. The estimated detection rates of Pop III BBH mergers by the Einstein Telescope are $sim 6-230 rm yr^{-1}$ and $sim 30-1230 rm yr^{-1}$ for the NSC-DH and IBSE channels, respectively. Pop III BBH mergers in NSCs are more massive than those from IBSE, so they dominate the Pop III SGWB below 20 Hz in most cases. Besides, the detection rate of Pop III BBH mergers involving at least one intermediate-mass BH above $100 rm M_odot$ by the Einstein Telescope is $sim 0.5-200 rm yr^{-1}$ in NSCs but remains below $0.1 rm yr^{-1}$ for IBSE.","PeriodicalId":18930,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"54 1","pages":""},"PeriodicalIF":4.8,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142256123","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0