arXiv subjects

Xingming Chen

Publications and source records attributed to Xingming Chen.

At least 19 recordsLinked to original sources

arXiv2024

MV-MOS: Multi-View Feature Fusion for 3D Moving Object Segmentation

Effectively summarizing dense 3D point cloud data and extracting motion information of moving objects (moving object segmentation, MOS) is crucial to autonomous driving and robotics applications. How to effectively utilize motion and semantic features and avoid information loss during 3D-to-2D projection is still a key challenge. In this paper, we propose a novel multi-view MOS model (MV-MOS) by fusing motion-semantic features from different 2D representations of point clouds. To effectively exploit complementary information, the motion branches of the proposed model combines motion features from both bird's eye view (BEV) and range view (RV) representations. In addition, a semantic branch is introduced to provide supplementary semantic features of moving objects. Finally, a Mamba module is utilized to fuse the semantic features with motion features and provide effective guidance for the motion branches. We validated the effectiveness of the proposed multi-branch fusion MOS framework via comprehensive experiments, and our proposed model outperforms existing state-of-the-art models on the SemanticKITTI benchmark.

cs.CV↗

arXiv2024

YOLO-Ant: A Lightweight Detector via Depthwise Separable Convolutional and Large Kernel Design for Antenna Interference Source Detection

In the era of 5G communication, removing interference sources that affect communication is a resource-intensive task. The rapid development of computer vision has enabled unmanned aerial vehicles to perform various high-altitude detection tasks. Because the field of object detection for antenna interference sources has not been fully explored, this industry lacks dedicated learning samples and detection models for this specific task. In this article, an antenna dataset is created to address important antenna interference source detection issues and serves as the basis for subsequent research. We introduce YOLO-Ant, a lightweight CNN and transformer hybrid detector specifically designed for antenna interference source detection. Specifically, we initially formulated a lightweight design for the network depth and width, ensuring that subsequent investigations were conducted within a lightweight framework. Then, we propose a DSLK-Block module based on depthwise separable convolution and large convolution kernels to enhance the network's feature extraction ability, effectively improving small object detection. To address challenges such as complex backgrounds and large interclass differences in antenna detection, we construct DSLKVit-Block, a powerful feature extraction module that combines DSLK-Block and transformer structures. Considering both its lightweight design and accuracy, our method not only achieves optimal performance on the antenna dataset but also yields competitive results on public datasets.

cs.CV↗

arXiv1998

Disk and Coronal Instabilities in GRS 1915+105

We present time-resolved GRS 1915+105 energy and power spectra observed by RXTE, during an episode where the X-ray intensity makes an extreme dip. If the spectra are modeled in terms of disk and power law components, both have large variations. When the inner disk is disrupted, the power law dominates, exhibiting quasi-periodic oscillations with varying frequency until the inner disk returns.

astro-ph↗

arXiv1998

Double Core Evolution X. Through the Envelope Ejection Phase

The evolution of binary systems consisting of an asymptotic giant branch star of mass equal to 3 M_sun or 5 M_sun, and a main sequence star of mass equal to 0.4 M_sun or 0.6 M_sun with orbital periods > 200 days has been followed from the onset through the late stages of the common envelope phase. Using a nested grid technique, the three-dimensional hydrodynamical simulations of an asymptotic giant branch star with radii approximately 1 A.U. indicate that a significant fraction of the envelope gas is unbound (about 31% and 23% for binaries of 3 M_sun and 0.4 M_sun, and 5 M_sun and 0.6 M_sun respectively) by the ends of the simulations, and that the efficiency of the mass ejection process is about 40%. While the original volume of the giant is virtually evacuated in the late stages, most of the envelope gas remains marginally bound on the grid. At the ends of our simulations, when the orbital decay timescale exceeds about 5 years, the giant core and companion orbit one another with a period of about 1 day (2.4 days for a binary involving a more evolved giant), although this is an upper limit to the final orbital period. For a binary of 5 M_sun and 0.4 M_sun, the common envelope may not be completely ejected.

astro-ph↗

arXiv1997

Rapid Bursts From GRS 1915+105 with RXTE

The light curves of GRS 1915+105 observed with RXTE on October 15, 1996 reveal a wide range of transient activity including regular bursts with a recurrence time of about 1 minute, irregular bursts, and dips. In contrast to bursts from other sources, a secondary (and a tertiary) weaker burst immediately following the primary burst are observed. Detailed energy spectra indicate that the source softens during the main outburst and successively hardens during the secondary and tertiary bursts. This may imply that the accretion flow has a corona-disk configuration and that the relative contribution of the hot corona decreases during the primary bursts and increases during the secondary and tertiary bursts. The primary burst profile resembles the bursts produced in the time dependent evolutions of accretion disks which are thermally and viscously unstable. The secondary burst may reflect an inward shift of the inner edge of the disk which results in a greater release of gravitational binding energy.

astro-ph↗

arXiv1996

The Pattern of Correlated X-ray Timing and Spectral Behavior in GRS 1915+105

From data obtained from the PCA in the 2-11 keV and 11-30.5 keV energy range, GRS 1915+105 is seen during RXTE observations between 1996 May and October on two separate branches in a hardness intensity diagram. On the hard branch, GRS 1915+105 exhibits narrow quasi-periodic oscillations ranging from 0.5 to 6 Hz with ${Δν\over ν} \sim 0.2$. The QPOs are observed over intensities ranging from about 6,000 to 20,000 counts s$^{-1}$ in the 2 - 12.5 keV energy band, indicating a strong dependence on source intensity. Strong harmonics are seen, especially, at lower frequencies. As the QPO frequency increases, the harmonic feature weakens and disappears. On the soft branch, narrow QPOs are absent and the low frequency component of the power density spectrum is approximated by a power-law, with index $\sim -1.25$ for low count rates and $\sim -1.5$ for high count rates ($\gta 18000$ cts/s). Occasionally, a broad peaked feature in the 1-6 Hz frequency range is also observed on this branch. The source was probably in the very high state similar to those of other black hole candidates. Thermal-viscous instabilities in accretion disk models do not predict the correlation of the narrow QPO frequency and luminosity unless the fraction of luminosity from the disk decreases with the total luminosity.

astro-ph↗

arXiv1996

On the morphology of accretion flows with small non-zero specific angular momentum

The morphology of adiabatic accretion flows with small non-zero specific angular momentum has been investigated in the axisymmetric and nonviscous limit. For an initial state characterized by a Bondi flow with the specific angular momentum distributed with respect to polar angle, a travelling shock wave forms which propagates more rapidly in the equatorial plane than in the plane perpendicular to it resulting in the formation of a hot torus. In cases where the incoming flow is restricted to lie near the equatorial plane, a strong wind forms directed away from this plane with the tendency for the formation of a nonsteady shock structure. As the height of the incoming flow is increased it is found that the resultant wind weakens. The parameter regime which delineates accretion flows characterized by a travelling shock and a nearly standing shock structure is presented.

astro-ph↗

arXiv1996

Advection-dominated accretion: global transonic solutions

We obtained global transonic solutions representing optically thin advection-dominated accretion flow by solving the full set of differential equations describing such systems. We found that far from the sonic point self-similar solutions are an excellent approximation of the global flow structure if the accretion rate is well below the maximum value above which no optically thin solutions exist.

astro-ph↗

arXiv1996

The Spectral States of Black Hole X-ray Binary Sources

A framework for the interpretation of the spectral states of black hole X-ray transients based on the diversity of accretion disk models is introduced. Depending on the mass accretion rate, it is proposed that the accretion disk is described by one or a combination of the following structures: optically thick disk, advection-dominated disk, corona-disk, and non-steady state disk. In particular, it is suggested that the very high, high, low, and off states are characterized by mass accretion rates of decreasing magnitude. The very high state corresponds to mass accretion rates near the Eddington limit in which an optically thin non steady inner region is surrounded by an optically thick structure. In the high state, the inner region is optically thin and advection-dominated or optically thick. The low hard state is interpreted in terms of a disk-corona system and the off state in terms of an optically thin disk dominated by advective energy transport into the black hole. The possible observational consequences of such a paradigm are discussed.

astro-ph↗

arXiv1996

Special relativity and the pseudo-Newtonian potential

A simple re-scaling of velocities calculated from the Paczy{ń}ski \& Wiita (1980) pseudo-Newtonian potential makes them consistent with special relativity and greatly improves the agreement with the exact relativistic calculations. The improvement is relevant in calculations of the Doppler effect, spectra and radiation transfer which all involve effects of special relativity.

astro-ph↗

arXiv1996

Instabilities of Advection-Dominated Accretion Flows

Accretion disk instabilities are briefly reviewed. Some details are given to the short-wavelength thermal instabilities and the convective instabilities. Time-dependent calculations of two-dimensional advection-dominated accretion flows are presented.

astro-ph↗

arXiv1995

Thermal Instability of Advection-Dominated Disks against Local Perturbations

Thermal instability is examined for advection-dominated one-temperature accretion disks. We consider axisymmetric perturbations with short wavelength in the radial direction. The viscosity is assumed to be sufficiently small for the vertical hydrostatic balance to hold in perturbed states. The type of viscosity is given either by the $α$-viscosity or by a diffusion-type stress tensor. Optically thick disks are found to be in general more unstable than optically thin ones. When the thermal diffusion is present, the optically thin disks become stable, but the optically thick disks are still unstable. The instability of the advection-dominated disks is different from that of the geometrically thin disks without advection. In the case of no advection, the thermal mode behaves under no appreciable surface density change. In the case of advection-dominated disks, however, the thermal mode occurs with no appreciable pressure change (compared with the density change), when local perturbations are considered. The variations of angular momentum and of surface density associated with the perturbations lead to a thermal instability. The astrophysical implications of this instability are briefly discussed.

astro-ph↗

arXiv1995

Accretion discs around black holes: two dimensional, advection cooled flows

Two-dimensional accretion flows near black holes have been investigated by time-dependent hydrodynamical calculations. We assume that the flow is axisymmetric and that radiative losses of internal energy are negligible, so that the disc is geometrically thick and hot. Accretion occurs due to the overflow of the effective potential barrier near the black hole, similar to the case of the Roche lobe overflowing star in a binary system. We make no pre-assumptions on the properties of the flow, instead our models evolve self-consistently from an initially non-accreting state. The viscosity is due to the the small-scale turbulence and it is described by the $α$-viscosity prescription. We confirm earlier suggestions that viscous accretion flows are convectively unstable. We found that the instability produces transient eddies of various length-scales. The eddies contribute to the strength of the viscosity in the flow by redistributing the angular momentum. They also introduce low amplitude oscillatory variations which have a typical frequency about $100\; \msun/M$ Hz for a system of mass $M$. This may be relevant to the high frequency ($\sim 4-10$ Hz) quasi-periodic oscillations observed in the Galactic black hole candidate X-ray sources.

astro-ph↗

arXiv1995

THE EVOLUTION OF ACCRETION DISKS WITH CORONAE: A MODEL FOR THE LOW-FREQUENCY QUASI-PERIODIC OSCILLATIONS IN X-RAY BINARIES

The global nonlinear time dependent evolution of accretion disk-corona systems in X-ray binary sources has been investigated to provide an understanding of the low frequency ($\sim 0.04$~Hz) quasi-periodic oscillations (QPOs) observed recently in the Rapid Burster MXB 1730-335 and in some black hole candidates sources (Cyg X--1 and GRO~J0422+32). We consider $α$-viscosity models in which the viscous stress is proportional to the total pressure. In contrast to previous time dependent studies it is assumed that all mass accretion and angular momentum transport take place in an optically thick disk, but that a fraction of the gravitational energy that is released is dissipated in a corona. It is found that the coronal energy dissipation can effectively reduce the amplitudes of the mass flow variations generated from the thermal and viscous instabilities (in comparison to models without a corona) to a state in which the disk exhibits mild oscillatory nonsteady behavior. These oscillations are globally coherent in the unstable regions of the disk. A model for the high and low states of black hole candidate systems is also proposed. It is suggested that the low state, which is characterized by a hard X-ray spectrum, corresponds to a disk configuration in which the inner disk is in an advection dominated hot optically thin state whereas the high state corresponds to a configuration in which the inner disk is in an optically thick state surrounded by a corona. In this model, the mass accretion rate in the system is higher in the low state than in the high state. The hard X-ray spectrum of QPOs observed in the low state can be naturally explained by such a model.

astro-ph↗

arXiv1995

HOT ACCRETION DISKS WITH ADVECTION

The global structure of optically thin hot accretion disks with radial advection included has been investigated. We solve the full energy conservation equation explicitly and construct the radial structure of the disk. It is found that advection is a real cooling process and that there are two solutions co-exist for a given mass accretion rate less than a critical limit. One is fully advection cooling dominated and the other is dominated by local radiative cooling. The advection dominated accretion disks are hotter than the local cooling dominated disks; they are most probably in the two-temperature regime and effects such as electron-positron pair production and annihilation may need to be considered to study the microphysics of the hot plasma. However, the global disk structure will not be much affected by the local radiative process.

astro-ph↗

arXiv1995

COLD ACCRETION DISKS WITH CORONAE AND ADVECTION

Cold optically thick accretion disks with hot coronae and radial advection have been investigated. Within the framework of $α$-viscosity models, we assume that all the mass accretion and angular momentum transport take place in the cold disk, but that a fraction of the gravitational energy released is dissipated in the corona. Both the coronal energy dissipation and the advection heat transport have a stabilization effect on the thermal and viscous instabilities of the disk. If that more than $\sim 95$ percent of the total power is dissipated in the corona, then the locally unstable behavior of the disk is restricted to a relatively narrow spatial region and is found to lie in a small range of mass accretion rates. The global temporal variability of the disk can be very mild or may disappear, and which may be applicable to the low-frequency ($\sim 0.04$~Hz) quasi-periodic oscillations observed in black hole candidates Cyg X--1 and GRO J0422+32.

astro-ph↗

arXiv1995

Unified Description of Accretion Flows Around Black Holes

We provide a unified description of thermal equilibria of black hole accretion disks, including the newly-discovered advection-dominated solutions. We classify the solutions on the basis of optical depth and importance of advection cooling. We demonstrate that only four physically distinct topological types of equilibria exist. Two of the types correspond to optically thin and optically thick equilibria, while the other two types are distinguished by whether advection is negligible or dominant. A stable Shakura-Sunyaev disk exists only for accretion rates $\dot M$ below a certain maximum. However, there is a critical viscosity parameter $α_{\rm crit}$, which is a function of radius, such that for $α>α_{\rm crit}$ advection-dominated solutions exist for all $\dot M$. Even when $α< α_{\rm crit}$, the advection-dominated solutions are available for a wide range of $\dot M$ except for a gap around the Eddington rate. We therefore suggest that advection-dominated flows may be more common than standard thin disks in black hole systems. For certain ranges of radii and $\dot M$, no stable steady state solution is possible. In these cases, we suggest that limit cycle behavior may occur, leading to variability.

astro-ph↗

arXiv1994

Variability of Accretion Disks Surrounding Black Holes ----- the Role of Inertial-Acoustic Mode Instabilities

The global nonlinear time-dependent evolution of the inertial-acoustic mode instability in accretion disks surrounding black holes has been investigated. The viscous stress is assumed to be proportional to the gas pressure only, i.e.\,, $τ= - αp_g$. It is found that an oscillatory instability exists in the inner regions of disks ($r < 10 r_g$, where $r_g$ is the Schwarzschild radius) for sufficiently large $α$ ($\gapprox 0.2$), and for mass accretion rates less than about 0.3 times the Eddington value. The variations of the integrated bolometric luminosity from the disk, $ΔL/L$, are less than 3\%. A power spectrum analysis of these variations reveals a power spectrum which can be fit to a power law function of the frequency $P \propto f^{-γ}$, with index $γ\sim 1.4-2.3$ and a low frequency feature at about 4 Hz in one case. In addition, a narrow peak centered at a frequency corresponding to the maximum epicyclic frequency of the disk at $\sim 100-130$ Hz and its first harmonic is also seen. The low frequency modulations are remarkably similar to those observed in black hole candidate systems. The possible existence of a scattering corona in the inner region of the disk and/or to other processes contributing to the power at high frequencies in the inner region of the accretion disk may make the detection of the high frequency component difficult.

astro-ph↗