A5001222540- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Astronomy and Astrophysical Research
- Astrophysical Phenomena and Observations
- Pulsars and Gravitational Waves Research
- Gamma-ray bursts and supernovae
- Astro and Planetary Science
- Galaxies: Formation, Evolution, Phenomena
- Scientific Research and Discoveries
- Adaptive optics and wavefront sensing
- Advanced Optical Sensing Technologies
- Astrophysics and Cosmic Phenomena
- Astronomical Observations and Instrumentation
- Space Exploration and Technology
- Osteoarthritis Treatment and Mechanisms
- Relativity and Gravitational Theory
- Photonic and Optical Devices
- Lung Cancer Diagnosis and Treatment
- Computational Physics and Python Applications
- Remote Sensing in Agriculture
- Cosmology and Gravitation Theories
- IL-33, ST2, and ILC Pathways
- Optical Coherence Tomography Applications
- Web Applications and Data Management
- Numerical methods for differential equations
Sun Yat-sen University
2020-2024
Xi'an Jiaotong University
2017-2024
Hubei University of Medicine
2024
Taihe Hospital
2024
Beijing Normal University
2023
RIKEN Center for Computational Science
2017-2022
The University of Tokyo
2019-2022
PLA Air Force Aviation University
2022
National Institute for Space Research
2021
Peking University
2006-2020
Searching for distinctive signatures, which characterize different formation channels of binary black holes (BBHs), is a crucial step towards the interpretation current and future gravitational wave detections. Here, we investigate demography merging BBHs in young star clusters (SCs), are nursery massive stars. We performed 4 × 103N-body simulations SCs with metallicity Z = 0.002, initial fraction 0.4, fractal conditions, to mimic clumpiness star-forming regions. Our include novel...
Introducing the dragon simulation project, we present direct N-body simulations of four massive globular clusters (GCs) with 106 stars and 5 per cent primordial binaries at a high level accuracy realism. The GC evolution is computed nbody6++gpu follows dynamical stellar individual binaries, kicks neutron black holes (BHs), effect tidal field. We investigate luminous (stellar) dark (faint remnants) components create mock observations (i.e. photometry, colour–magnitude diagrams, surface...
Accurate direct $N$-body simulations help to obtain detailed information about the dynamical evolution of star clusters. They also enable comparisons with analytical models and Fokker-Planck or Monte-Carlo methods. NBODY6 is a well-known code for clusters, NBODY6++ extended version designed large particle number by supercomputers. We present NBODY6++GPU, an optimized hybrid parallelization methods (MPI, GPU, OpenMP, AVX/SSE) accelerate simulations, in particular solve million-body problem....
Objectives Single-cell and spatial transcriptomics analysis of human knee articular cartilage tissue to present a comprehensive transcriptome landscape osteoarthritis (OA)-critical cell populations. Methods RNA sequencing spatially resolved transcriptomic technology have been applied characterise the cellular heterogeneity which were collected from 8 OA donors, 3 non-OA control total 19 samples. The novel chondrocyte population marker genes interest validated by immunohistochemistry...
The observation of quasars at very high redshift such as Poniuaena is a challenge for models super-massive black hole (SMBH) formation. This work presents study SMBH formation via known physical processes in star-burst clusters formed the onset their hosting galaxy. While early stages hyper-massive reach luminosities quasars, once massive stars die, ensuing gas accretion from still forming host galaxy compresses its stellar (BH) component to compact state overcoming heating BH--BH binaries...
Context. As a result of their formation via massive single and binary stellar evolution, the masses stellar-remnant black holes (BH) are subjects great interest in this era gravitational-wave detection from hole (BBH) neutron star merger events. Aims. In work, we present new developments related schemes current N -body evolution program NBODY7 . We demonstrate that newly implemented stellar-wind remnant-formation stellar-evolutionary sector or BSE code, such as “rapid” “delayed” supernova...
Young dense massive star clusters are a promising environment for the formation of intermediate mass black holes (IMBHs) through collisions. We present set 80 simulations carried out with Nbody6++GPU 10 initial conditions compact $\sim 7 \times 10^4 M_{\odot}$ half-mass radii $R_\mathrm{h} \lesssim 1 pc$, central densities $\rho_\mathrm{core} \gtrsim 10^5 M_\odot pc^{-3}$, and resolved stellar populations 10\% primordial binaries. Very stars (VMSs) masses up to 400 M_\odot$ grow rapidly by...
The numerical simulations of massive collisional stellar systems, such as globular clusters (GCs), are very time-consuming. Until now, only a few realistic million-body GCs with small fraction binaries (5%) have been performed by using the NBODY6++GPU code. Such models took half year computational time on GPU based super-computer. In this work, we develop new N-body code, PeTar, combining methods Barnes-Hut tree, Hermite integrator and slow-down algorithmic regularization (SDAR). code can...
Intermediate-mass black holes (IMBHs) are those between 100 and 10$^5$ solar masses ($M_{\odot}$); their formation process is debated. One possible origin the growth of less massive (BHs) via mergers with stars compact objects within globular clusters (GCs). However, previous simulations have indicated that this only produces IMBHs $<500 M_{\odot}$ because gravitational wave recoil ejects them when they merge other BHs. We perform star-by-star GC formation, finding high-density star in a...
We use the Millennium Simulation, a 10 billion particle simulation of growth cosmic structure, to construct new model galaxy clustering. adopt methodology that falls midway between traditional semi-analytic approach and halo occupation distribution (HOD) approach. In our model, we positions velocities galaxies are predicted by following orbits merging histories substructures in simulation. Rather than using star formation feedback 'recipes' specify physical properties galaxies, parametrized...
We present the first detailed comparison between million-body globular cluster simulations computed with a H\'enon-type Monte Carlo code, CMC, and direct $N$-body NBODY6++GPU. Both start from an identical model $10^6$ particles, include all of relevant physics needed to treat system in highly realistic way. With two codes "frozen" (no fine-tuning any free parameters or internal algorithms codes) we find excellent agreement overall evolution models. Furthermore, that both models, large...
Many possible scenarios for the formation of multiple stellar populations (MSP) in globular clusters (GCs) have been discussed so far, including involvement asymptotic giant branch stars, fast rotating main sequence very massive stars and mass-transferring binaries based on evolution modelling. But self-consistent, dynamical simulations young GCs are usually not considered. In this work, we perform direct $N$-body modelling such systems with total masses up to $3.2\times10^5$ M$_\odot$,...
We study the dynamics and evolution of Milky Way nuclear star cluster performing a high resolution direct one-million-body simulation. Focusing on interactions between such stellar system central supermassive black hole, we find that different components adapt their overall distribution differently. After 5 Gyr, mass holes are characterized by spatial with power-slope $-1.75$, fully consistent prediction Bahcall-Wolf pioneering work. Using vast amount data available, infer rate for tidal...
Abstract We identify members of 65 open clusters in the solar neighborhood using machine-learning algorithm StarGO based on Gaia EDR3 data. After adding 20 from previous studies we obtain 85 clusters, and study their morphology kinematics. classify substructures outside tidal radius into four categories: filamentary (f1) fractal (f2) for <100 Myr, halo (h) tail (t) >100 Myr. The kinematical f1-type are elongated; these resemble disrupted cluster Group X. Kinematic tails distinct t-type...
ABSTRACT Gaia BHs, black hole (BH) binaries discovered from data base of an astrometric telescope Gaia, pose a question to the standard binary evolution model. We have assessed whether BHs can be formed through dynamical capture in open clusters rather than isolated evolution. performed gravitational N-body simulations 100 with $10^5 \, \mathrm{M}_\odot$ total for each metallicity Z = 0.02, 0.01, and 0.005. one BH-like escaping cluster, found that formation efficiency ($\sim 10^{-5}...
The mode of star formation that results in the globular clusters and young massive is difficult to constrain through observations. We present models cluster using T ORCH framework, which uses Astrophysical MUltipurpose Software Environment (AMUSE) couple distinct multi-physics codes handle formation, stellar evolution dynamics, radiative transfer, magnetohydrodynamics. upgraded by implementing N-body code P ETAR , thereby enabling forming from 10 6 M ⊙ clouds with ≥10 5 individual stars....
Instabilities in planetary systems can result the ejection of planets from their host system, resulting free-floating (FFPs). If this occurs a star cluster, FFP may remain bound to cluster for some time and interact with other members until it is ejected. Here, we use $N$-body simulations characterise close star-planet planet-planet encounters dynamical fate population clusters containing $500-2000$ single or binary members. We find that FFPs ejected system at low velocities typically leave...
We investigate the dissolution process for dynamically evolving star clusters embedded in an external tidal field by exploring MOCCA Survey Database I, with focus on presence and evolution of a stellar-mass black hole subsystem. argue that subsystem can lead to tidally filling this be regarded as third type cluster mechanism (in addition well-known mechanisms connected strong mass loss due stellar relaxation process). This is characterized abrupt dynamical equilibrium. The powered energy...
ABSTRACT We present the implementation of updated stellar evolution recipes in codes nbody6++gpu, mocca, and mcluster. test them through numerical simulations star clusters containing 1.1 × 105 stars (with 2.0 104 primordial hard binaries) performing high-resolution direct N-body (nbody6++gpu) Monte Carlo (mocca) to an age 10 Gyr. compare models implementing either delayed or core-collapse supernovae mechanisms, a different mass ratio distribution for binaries, white dwarf (WD) natal kicks...
Identifying bifurcated blue straggler (BS) sequences in color-magnitude diagrams (CMDs) of star clusters has long been regarded as a powerful diagnostic for distinguishing different BS formation mechanisms. While such bifurcations are typically associated with core-collapsed clusters, their detection dynamically young raises new questions about origins. In this study, using high-precision proper motion data derived from Hubble Space Telescope multi-epoch observations, we confirm the...
We carry out N-body simulations to examine the effects of dynamical interactions on planetary systems in young open star clusters. explore how populations these clusters evolve, and this evolution depends initial amount substructure, virial ratio, cluster mass density, semi-major axis systems. The fraction that remains intact as a member, fBPS, is generally well-described by functional form fBPS = f0(1 + [a/a0]c)−1, where (1 − f0) stars escapes from cluster, a0 critical for survival, c...
Recently, three stellar sequences separated in age by about 1 Myr were discovered the Orion Nebula Cluster (ONC; Beccari et al. 2017). Kroupa (2018) suggest that such small dense subpopulations eject all their OB stars via decay of unstable few-body systems gas can recombine and form new stars. This explains multisequence phenomenon without introducing an extra mechanism into star formation theory. In this work, we apply recently updated primordial binary distribution model (Belloni 2017;...
ABSTRACT An accurate and efficient method dealing with the few-body dynamics is important for simulating collisional N-body systems like star clusters to follow formation evolution of compact binaries. We describe such a which combines time-transformed explicit symplectic integrator slow-down method. The former conserves Hamiltonian angular momentum long-term evolution, while latter significantly reduces computational cost weakly perturbed binary. In this work, Hamilton equations algorithm...
The hierarchical galaxy formation picture suggests that super massive black holes (MBHs) observed in galactic nuclei today have grown from coalescence of hole binaries (MBHB) after merging. Once the components a MBHB become gravitationally bound, strong three-body encounters between and stars dominate its evolution "dry" gas free environment, change MBHB's energy angular momentum (semi-major axis, eccentricity orientation). Here we present high accuracy direct N-body simulations spherical...