Monthly Notices of the Royal Astronomical Society最新文献_第4页

Randomness and Retention: Using Weak Mean Motion Resonances to Constrain Neptune’s Late-Stage Migration 随机性与保留：利用弱平均运动共振来约束海王星的后期迁移

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-05-10 DOI: 10.1093/mnras/stae1246

Arcelia Hermosillo Ruiz, Harriet C.P. Lau, R. Murray-Clay

{"title":"Randomness and Retention: Using Weak Mean Motion Resonances to Constrain Neptune’s Late-Stage Migration","authors":"Arcelia Hermosillo Ruiz, Harriet C.P. Lau, R. Murray-Clay","doi":"10.1093/mnras/stae1246","DOIUrl":"https://doi.org/10.1093/mnras/stae1246","url":null,"abstract":"\u0000 Planet-planetesimal interactions cause a planet to migrate, manifesting as a random walk in semi-major axis. In models for Neptune’s migration involving a gravitational upheaval, this planetesimal-driven migration is a side-effect of the dynamical friction required to damp Neptune’s orbital eccentricity. This migration is noisy, potentially causing Trans Neptunian Objects (TNOs) in mean motion resonance to be lost. With Nbody simulations, we validate a previously-derived analytic model for resonance retention and determine unknown coefficients. We identify the impact of random-walk (noisy) migration on resonance retention for resonances up to fourth order lying between 39 au and 75 au. Using a population estimate for the weak 7:3 resonance from the well-characterized Outer Solar System Origins Survey (OSSOS), we rule out two cases: (1) a planetesimal disk distributed between 13.3 and 39.9 au with ≳ 30 Earth masses in today’s size distribution and Tmig ≳ 40Myr and (2) a top-heavy size distribution with ≳2000 Pluto-sized TNOs and Tmig ≳10Myr, where Tmig is Neptune’s migration timescale. We find that low-eccentricity TNOs in the heavily populated 5:2 resonance are easily lost due to noisy migration. Improved observations of the low-eccentricity region of the 5:2 resonance and of weak mean motion resonances with Rubin Observatory’s Legacy Survey of Space and Time (LSST) will provide better population estimates, allowing for comparison with our model’s retention fractions and providing strong evidence for or against Neptune’s random interactions with planetesimals.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 85","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140993122","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

Introducing two improved methods for approximating radiative cooling in hydrodynamical simulations of accretion discs 在吸积盘流体力学模拟中引入两种近似辐射冷却的改进方法

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-05-09 DOI: 10.1093/mnras/stae1249

Alison K. Young, Maggie Celeste, Richard A. Booth, Ken Rice, Adam Koval, Ethan Carter, D. Stamatellos

{"title":"Introducing two improved methods for approximating radiative cooling in hydrodynamical simulations of accretion discs","authors":"Alison K. Young, Maggie Celeste, Richard A. Booth, Ken Rice, Adam Koval, Ethan Carter, D. Stamatellos","doi":"10.1093/mnras/stae1249","DOIUrl":"https://doi.org/10.1093/mnras/stae1249","url":null,"abstract":"\u0000 The evolution of many astrophysical systems depends strongly on the balance between heating and cooling, in particular star formation in giant molecular clouds and the evolution of young protostellar systems. Protostellar discs are susceptible to the gravitational instability, which can play a key role in their evolution and in planet formation. The strength of the instability depends on the rate at which the system loses thermal energy. To study the evolution of these systems, we require radiative cooling approximations because full radiative transfer is generally too expensive to be coupled to hydrodynamical models. Here we present two new approximate methods for computing radiative cooling that make use of the polytropic cooling approximation. This approach invokes the assumption that each parcel of gas is located within a spherical pseudo-cloud which can then be used to approximate the optical depth. The first method combines the methods introduced by Stamatellos et al. and Lombardi et al. to overcome the limitations of each method at low and high optical depths respectively. The second, the ‘Modified Lombardi’ method, is specifically tailored for self-gravitating discs. This modifies the scale height estimate from the method of Lombardi et al. using the analytical scale height for a self-gravitating disc. We show that the Modified Lombardi method provides an excellent approximation for the column density in a fragmenting disc, a regime in which the existing methods fail to recover the clumps and spiral structures. We therefore recommend this improved radiative cooling method for more realistic simulations of self-gravitating discs.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":" 39","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140997519","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

Correction to: Hyperbolic conduction: A fast, physical conduction model implemented in Smoothed Particle Hydrodynamics 更正：双曲传导：在平滑粒子流体力学中实现的快速物理传导模型

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-05-06 DOI: 10.1093/mnras/stae1107

N. A. Owens, J. Wadsley

引用次数: 0

The oldest stars with low neutron-capture element abundances and origins in ancient dwarf galaxies 中子捕获元素丰度低的最古老恒星及其在远古矮星系中的起源

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-05-06 DOI: 10.1093/mnras/stae670

Hillary Diane Andales, Ananda Santos Figueiredo, Casey Gordon Fienberg, M. Mardini, A. Frebel

{"title":"The oldest stars with low neutron-capture element abundances and origins in ancient dwarf galaxies","authors":"Hillary Diane Andales, Ananda Santos Figueiredo, Casey Gordon Fienberg, M. Mardini, A. Frebel","doi":"10.1093/mnras/stae670","DOIUrl":"https://doi.org/10.1093/mnras/stae670","url":null,"abstract":"\u0000 We present a detailed chemical abundance and kinematic analysis of six extremely metal-poor (−4.2 ≤ [Fe/H] ≤−2.9) halo stars with very low neutron-capture abundances ([Sr/H] and [Ba/H]) based on high-resolution Magellan/MIKE spectra. Three of our stars have [Sr/Ba] and [Sr/H] ratios that resemble those of metal-poor stars in ultra-faint dwarf galaxies (UFDs). Since early UFDs may be the building blocks of the Milky Way, extremely metal-poor halo stars with low, UFD-like Sr and Ba abundances may thus be ancient stars from the earliest small galactic systems that were accreted by the proto-Milky Way. We label these objects as Small Accreted Stellar System (SASS) stars, and we find an additional 61 similar ones in the literature. A kinematic analysis of our sample and literature stars reveals them to be fast-moving halo objects, all with retrograde motion, indicating an accretion origin. Because SASS stars are much brighter than typical UFD stars, identifying them offers promising ways towards detailed studies of early star formation environments. From the chemical abundances of SASS stars, it appears that the earliest accreted systems were likely enriched by a few supernovae whose light element yields varied from system to system. Neutron-capture elements were sparsely produced and/or diluted, with r-process nucleosynthesis playing a role. These insights offer a glimpse into the early formation of the Galaxy. Using neutron-capture elements as a distinguishing criterion for early formation, we have access to a unique metal-poor population that consists of the oldest stars in the universe.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"7 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141006573","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

WISDOM Project – XIX. Figures of merit for supermassive black hole mass measurements using molecular gas and/or megamaser kinematics WISDOM 项目 - XIX.利用分子气体和/或巨激光运动学测量超大质量黑洞质量的优越性数字

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-24 DOI: 10.1093/mnras/stae1106

Hengyue Zhang, Martin Bureau, Mark D Smith, M. Cappellari, T. Davis, Pandora Dominiak, J. Elford, Fu-heng Liang, I. Ruffa, Thomas G Williams

{"title":"WISDOM Project – XIX. Figures of merit for supermassive black hole mass measurements using molecular gas and/or megamaser kinematics","authors":"Hengyue Zhang, Martin Bureau, Mark D Smith, M. Cappellari, T. Davis, Pandora Dominiak, J. Elford, Fu-heng Liang, I. Ruffa, Thomas G Williams","doi":"10.1093/mnras/stae1106","DOIUrl":"https://doi.org/10.1093/mnras/stae1106","url":null,"abstract":"\u0000 The mass (MBH) of a supermassive black hole (SMBH) can be measured using spatially-resolved kinematics of the region where the SMBH dominates gravitationally. The most reliable measurements are those that resolve the smallest physical scales around the SMBHs. We consider here three metrics to compare the physical scales probed by kinematic tracers dominated by rotation: the radius of the innermost detected kinematic tracer Rmin normalised by respectively the SMBH’s Schwarzschild radius (RSchw ≡ 2GMBH/c2, where G is the gravitational constant and c the speed of light), sphere-of-influence (SOI) radius ($R_mathrm{SOI}equiv GM_mathrm{BH}/sigma _mathrm{e}^2$, where σe is the stellar velocity dispersion within the galaxy’s effective radius) and equality radius (the radius Req at which the SMBH mass equals the enclosed stellar mass, MBH = M*(Req), where M*(R) is the stellar mass enclosed within the radius R). All metrics lead to analogous simple relations between Rmin and the highest circular velocity probed Vc. Adopting these metrics to compare the SMBH mass measurements using molecular gas kinematics to those using megamaser kinematics, we demonstrate that the best molecular gas measurements resolve material that is physically closer to the SMBHs in terms of RSchw but is slightly farther in terms of RSOI and Req. However, molecular gas observations of nearby galaxies using the most extended configurations of the Atacama Large Millimeter/sub-millimeter Array can resolve the SOI comparably well and thus enable SMBH mass measurements as precise as the best megamaser measurements.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"53 20","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140660856","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

Periodic activities of Fast Radio Burst repeaters from precessing magnetars with evolving obliquity 来自斜度不断变化的前冲磁星的快速射电暴中继器的周期性活动

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-24 DOI: 10.1093/mnras/stae1092

Xin-Ming Feng, Yuanpei Yang, Qiao-Chu Li

{"title":"Periodic activities of Fast Radio Burst repeaters from precessing magnetars with evolving obliquity","authors":"Xin-Ming Feng, Yuanpei Yang, Qiao-Chu Li","doi":"10.1093/mnras/stae1092","DOIUrl":"https://doi.org/10.1093/mnras/stae1092","url":null,"abstract":"\u0000 Fast radio bursts (FRBs) are cosmological radio transients with millisecond durations and extremely high brightness temperatures. One FRB repeater, FRB 180916.J0158+65 (FRB 180916B), was confirmed to appear 16.35-day periodic activities with 5-day activity window. Another FRB repeater, FRB 121102, and two soft gamma-ray repeaters (SGRs), SGR 1935+2154 and SGR 1806-20, also show possible periodic activities. These periodicities might originate from the precession process of young magnetars due to the anisotropic pressure from the inner magnetic fields as proposed in the literature. In this work, we analyze a self-consistent model for the rotation evolution of magnetars and obtain the evolutions of magnetar precession and obliquity. We find that if the FRB repeaters and the SGRs with (possible) periodic activities originate from the magnetar precession, their ages would be constrained to be hundreds to tens of thousands of years, which is consistent with the typical ages of magnetars. Assuming that the FRB emission is beaming in the magnetosphere as proposed in the literature, we calculate the evolution of the observable probability and the duty cycle of the active window period. We find that for a given magnetar the observable probability increases with the magnetar age in the early stage and decreases with the magnetar age in the later stage, meanwhile, there are one or two active windows in one precession period if the emission is not perfectly axisymmetric with respect to the deformation axis of a magnetar, which could be tested by the future observation for repeating FRB sources.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"38 15","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140661187","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

ExoMol line lists – LVIII. High-temperature molecular line list of carbonyl sulphide (OCS) ExoMol 线表 - LVIII.羰基硫化物（OCS）的高温分子线表

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-24 DOI: 10.1093/mnras/stae1110

A. Owens, S. Yurchenko, J. Tennyson

{"title":"ExoMol line lists – LVIII. High-temperature molecular line list of carbonyl sulphide (OCS)","authors":"A. Owens, S. Yurchenko, J. Tennyson","doi":"10.1093/mnras/stae1110","DOIUrl":"https://doi.org/10.1093/mnras/stae1110","url":null,"abstract":"\u0000 A new molecular line list covering wavelengths λ > 1 μm (the 0 – 10 000 cm−1 range) for the main isotopologue of carbonyl sulphide 16O12C32S is presented. The OCS line list, named OYT8, contains almost 2.5 billion transitions between 2.4 million rotation-vibration energy levels with the total angular momentum up to J = 223. It is suitable for high-temperature environments up to T = 2000 K. Line list calculations were performed with the variational nuclear motion code trove in conjunction with a highly accurate, empirically-refined potential energy surface and a newly computed ab initio dipole moment surface of OCS. The OYT8 line list is adapted for high-resolution applications by replacing computed energy levels with empirically-derived values of OCS where available. Comparisons of the OYT8 line list with other OCS line lists and spectra yields excellent agreement for both strong and weak spectroscopic bands. The increased coverage of the OYT8 line list and the many new spectral features that are available will greatly facilitate the future observation of OCS on exoplanets. Carbonyl sulphide joins a growing number of sulphur-bearing molecules available from the ExoMol database. The OYT8 line list along with the associated temperature- and pressure-dependent molecular opacities can be downloaded from www.exomol.com and the CDS astronomical database.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"6 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140661644","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

Burst induced spin variations in the accreting magnetic white dwarf PBC J0801.2-4625 吸积磁性白矮星PBC J0801.2-4625的爆发诱导自旋变化

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-24 DOI: 10.1093/mnras/stae1103

Z. A. Irving, D. Altamirano, S. Scaringi, M. Veresvarska, C. Knigge, N. C. Segura, D. De Martino, K. Iłkiewicz

{"title":"Burst induced spin variations in the accreting magnetic white dwarf PBC J0801.2-4625","authors":"Z. A. Irving, D. Altamirano, S. Scaringi, M. Veresvarska, C. Knigge, N. C. Segura, D. De Martino, K. Iłkiewicz","doi":"10.1093/mnras/stae1103","DOIUrl":"https://doi.org/10.1093/mnras/stae1103","url":null,"abstract":"\u0000 PBC J0801.2-4625 is an intermediate polar with a primary spin frequency of 66.08 d−1 and an unknown orbital period. The long-term All Sky Automated Survey for Supernovae (ASAS-SN) light curve of this system reveals four bursts, all of which have similar peak amplitudes (∼2 mag) and durations (∼2 d). In this work, we primarily study the timing properties of this system’s February 2019 burst, which was simultaneously observed by both ASAS-SN and the Transiting Exoplanet Survey Satellite (TESS). Pre-burst, a frequency of 4.064 ± 0.002 d−1(5.906 ± 0.003 hr period), likely attributed to the binary orbit, is identified in addition to previous measurements for the white dwarf’s spin. During the burst, however, we find a spin frequency of 68.35 ± 0.28 d−1. Post-burst, the spin returns to its pre-brust value but with a factor 1.82 ± 0.05 larger amplitude. The burst profile is double-peaked, and we estimate its energy to be 3.3 × 1039 erg. We conclude that the burst appears most consistent with thermonuclear runaway (i.e., a “micronova”), and suggest that the spin variations may be an analog to burst oscillations (i.e., “micronova oscillations”). However, we also note that the above findings could be explained by a dwarf nova outburst. With the available data, we are unable to distinguish between these two scenarios.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"28 7","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140662605","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

Parametric description of intermittent probability distribution functions in solar wind and magnetohydrodynamic turbulence 太阳风和磁流体动力湍流中间歇概率分布函数的参数描述

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-24 DOI: 10.1093/mnras/stae1065

J. C. Palacios, Jean C. Perez, S. Bourouaine

{"title":"Parametric description of intermittent probability distribution functions in solar wind and magnetohydrodynamic turbulence","authors":"J. C. Palacios, Jean C. Perez, S. Bourouaine","doi":"10.1093/mnras/stae1065","DOIUrl":"https://doi.org/10.1093/mnras/stae1065","url":null,"abstract":"\u0000 In this work, we find empirical evidence that the scale-dependent statistical properties in solar wind and Magnetohydrodynamic (MHD) turbulence can be described in terms of a family of parametric probability distribution functions (PDFs) known as Normal Inverse Gaussian (NIG). Understanding these PDFs is one of the most important goals in turbulence theory, as they are inherently connected to the intermittent properties of solar wind turbulence. We investigate the properties of PDFs of Elsasser increments based on a large statistical sample from solar wind observations and high-resolution numerical simulations of MHD turbulence. In order to measure the PDFs and their corresponding properties, three experiments are presented: fast and slow solar wind for experimental data and a simulation of reduced MHD (RMHD) turbulence. Conditional statistics on a 23-year-long sample of WIND data near 1 au and high-resolution pseudo-spectral simulation of steadily driven RMHD turbulence on a 20483 mesh are used to construct scale-dependent PDFs. The empirical PDFs are fitted to NIG distributions, which depend on four free parameters. Our analysis shows that NIG distributions accurately capture the evolution of the PDFs, with scale-dependent parameters, from large scales characterized by a Gaussian distribution, turning to exponential tails within the inertial range and stretched exponentials at dissipative scales. We also show that empirically-measured NIG parameters exhibit well-defined scaling properties that are similar across the three empirical data sets, which may be indicative of universal behavior.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"27 11","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140662613","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

Impacts of Energetic Particles from T Tauri Flares on Inner Protoplanetary Discs 金牛座耀斑产生的高能粒子对内原行星盘的影响

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-24 DOI: 10.1093/mnras/stae1105

V. Brunn, C. Rab, A. Marcowith, C. Sauty, M. Padovani, C. Meskini

{"title":"Impacts of Energetic Particles from T Tauri Flares on Inner Protoplanetary Discs","authors":"V. Brunn, C. Rab, A. Marcowith, C. Sauty, M. Padovani, C. Meskini","doi":"10.1093/mnras/stae1105","DOIUrl":"https://doi.org/10.1093/mnras/stae1105","url":null,"abstract":"\u0000 T Tauri stars are known to be magnetically active stars subject to strong flares observed in X-rays. These flares are likely due to intense magnetic reconnection events during which a part of the stored magnetic energy is converted into kinetic energy of supra-thermal particles. Since T Tauri stars are surrounded by an accretion disc, these particles may influence the disc dynamics and chemistry. This work continues on a previous stationary model, which showed that energetic particles accelerated during flares can produce a strong ionisation rate at high column densities in the inner accretion disc. The present model includes non-stationary sequences of flaring events sampled by a Chandra X-ray survey of nearby young stellar objects. We calculate the averaged ionisation rate expected in a radius range from 0.08 to 0.6 au from the central star. We confirm that energetic particles produced by the flares dominate the ionisation of the disc up to column densities of $10^{25}~rm {cm^{-2}}$. We further study the main consequences of this additional source of ionisation on the viscosity, the accretion rate, the volumetric heating rate and the chemical complexity of inner protoplanetary discs.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140661474","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