A5100391966- Astrophysical Phenomena and Observations
- Pulsars and Gravitational Waves Research
- Gamma-ray bursts and supernovae
- Astrophysics and Cosmic Phenomena
- High-pressure geophysics and materials
- Radio Astronomy Observations and Technology
- Particle physics theoretical and experimental studies
- Neutrino Physics Research
- Dark Matter and Cosmic Phenomena
- Cosmology and Gravitation Theories
- Stellar, planetary, and galactic studies
- Black Holes and Theoretical Physics
- Geophysics and Gravity Measurements
- Soil Moisture and Remote Sensing
- Crystallography and Radiation Phenomena
- Antenna Design and Optimization
- Noncommutative and Quantum Gravity Theories
- Photocathodes and Microchannel Plates
- Astronomy and Astrophysical Research
- Laser-Plasma Interactions and Diagnostics
- Ga2O3 and related materials
- Nuclear Physics and Applications
- Quantum and electron transport phenomena
- Thermodynamic properties of mixtures
- Calibration and Measurement Techniques
Chinese Academy of Sciences
2009-2025
Institute of Semiconductors
2025
Wuhan University
2017-2022
Renmin Hospital of Wuhan University
2021
National Astronomical Observatories
2008-2019
Institute of High Energy Physics
2017-2018
Max Planck Institute for Extraterrestrial Physics
2008-2014
Excellence Cluster Universe
2014
Max Planck Society
2008
University of Hong Kong
2005
Massive stars form in groups and their winds supernova explosions create superbubbles up to kpc size. Their ejecta are important for the dynamics of interstellar medium chemical evolution models. However, kinematics characteristic scales space time rather unexplored beyond ~10 ka. Through measurement radioactive 26Al with its decay constant ~10^6 years, we aim trace massive-star over million-year scales. Our goal is identify mixing scale spatio-kinematics such from pc scale. We use SPI...
The measurement of gamma-ray lines from the decay chain 56Ni provides unique information about explosion in supernovae. freshly-produced supernova powers optical light curve, as it emits gamma-rays upon its radioactive to 56Co and then 56Fe. Gamma-ray are expected become directly visible through overlying white dwarf material several weeks after explosion, they progressively penetrate envelope, diluted expands. be Doppler-shifted or broadened kinematics ejecta. With SPI spectrometer on...
Abstract In this work, we interpreted the high braking index of PSR J1640−4631 with a combination magneto-dipole radiation and dipole magnetic field decay models. By introducing mean rotation energy conversion coefficient <?CDATA $\overline{\zeta }$?> , ratio total high-energy photon to loss in whole life pulsar, combining pulsar’s timing observations reliable nuclear equation state, estimate initial spin period, ${P}_{0}\sim (17\mbox{--}44)$?> ms, corresponding moment inertia $I\sim...
We present both timing and spectral analysis of the outburst 4U 0115+63 in April -- May 2008 with INTEGRAL RXTE observations. have determined spin period neutron star at $\sim 3.61430 \pm 0.00003$ s, a up rate during $\dot{P}=(-7.24 0.03)\times10^{-6} {\rm s d^{-1}}$, angle periapsis $\omega=48.67^\circ 0.04^\circ$ its variation (apsidal motion) $\dot{\omega} = 0.048^\circ 0.003^\circ yr}^{-1}$. also confirm relation spin-up torque versus luminosity this source giant outburst. The hard X-ray...
The Be X-ray pulsar, SMC X-3 underwent a giant outburst from 2016 August to 2017 March, which was monitored with the Swift satellite. During outburst, its broadband flux increased dramatically, and unabsorbed luminosity reached an extreme value of $\sim 10^{39}$ erg/s around 24. Using Swift/XRT data, we measure observed pulse frequency neutron star compute orbital parameters binary system. After applying corrections observations, find that spin increases steadily 128.02 mHz on 10 approach...
The hard X-ray source 4U 2206+54 is a peculiar high mass binary with main-sequence donor star. Recent observations suggested that the compact object in may be neutron emission comes from accretion of stellar winds massive stars, and variability luminosity due to changes its orbit phase. To further reveal nature object, we studied INTEGRAL/IBIS two years, found most time, undergone quiescent state sometime an active state. In spectrum can fitted by power-law model $\Gamma\sim 2.1$ $\sim...
Reprocessing of primary X-ray emission in the accretion disk black hole binaries (BHXRBs) produces reflection spectrum, with characteristic Fe K$\alpha$ fluorescence line. Strong low frequency quasi-periodic oscillations (QPOs) are observed from BHXRBs, and dependence QPO properties (e.g., phase-lag) on inclination angle suggests that may be associated a geometrical effect, e.g., precession source due to frame-dragging near spining hole. Here, scenario Lense-Thirring source, we use...
A deep hard X-ray survey of the INTEGRAL satellite first detected non-thermal emission up to 90 keV in Tycho supernova (SN) remnant. Its 3 -- 100 spectrum is fitted with a thermal bremsstrahlung $kT\sim 0.81\pm 0.45$ plus power-law model $\Gamma \sim 3.01\pm 0.16$. Based on diffusive shock acceleration theory, this emission, together radio measurements, implies that remnant may not accelerate protons $>$PeV but hundreds TeV. Only heavier nuclei be accelerated cosmic ray spectral "knee". In...
Spin properties and spectral variations of a high-mass X-ray binary 4U 2206+54 are studied with long-term hard monitoring observations by INTEGRAL. A long-period pulsar Pspin ∼ 5558 s has been identified in 2206+54. The spin evolution the neutron star is detected INTEGRAL/IBIS data. From 2005 to 2011, period varies from ∼5558 ∼5588 s. average spin-down rate last 20 years derived as ∼5 × 10−7 s−1. variable source luminosities ∼1035–1036 erg s−1 range 3–100 keV. Its spectrum can be described...
P-type doping in high Al-content AlGaN alloys is a main challenge for realizing AlGaN-based deep ultraviolet optoelectronics devices. According to the first-principles calculations, Mg activation energy may be reduced so that hole concentration can obtained by introducing nanoscale (AlN)5/(GaN)1 superlattice (SL) Al0.83Ga0.17N disorder alloy. In this work, experimental evidences were achieved analyzing doped and SLs as well MgGa δ SLs. acceptor was significantly from 0.378 0.331 eV using...
Possible manifestations of accreting magnetars are discussed. It is shown that the four ultra-luminous X-ray pulsars can be understood in low magnetic field magnetar scenario. The NGC300 ULX1 pulsar may have a higher dipole than other sources. General constraint on their mass accretion rate confirmed super-Eddington nature. Lower limits beaming factor obtained. They do not seem to strong beaming. duty cycle ULX burst state also constrained by timing observations. equilibrium long run. During...
Assuming the wind-fed accretion magnetars in long period X-ray pulsars, we calculated rotational evolution of neutron stars. Our calculations considered effects magnetic field decay magnetars. The results show that can evolve to pulsars with a spin much longer than 1000 s. spin-down trend observed 4U 2206+54 like sources is expected when young binary systems are on way their equilibrium period. Detailed showed its may be affected by outflows or while spin-down. Due magnetars, will have...
Long-term hard X-ray monitoring observations of high-mass binary Vela X-1 from 2003–2011 have been carried out by the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL). I systematically analysed average spectra 3–200 keV, with main aims detecting cyclotron resonant scattering features and studying their pattern variation accreting luminosity orbital phase. The lines at ∼22–27 49–57 keV are confirmed in X-1. However, flare states higher than ∼5 × 1036 erg s−1 (3–100 keV), fundamental...
A posteriori anisotropy study of ultra-high energy cosmic rays (UHECRs) with the Pierre Auger Observatory (PAO) has shown evidence an excess cosmic-ray particles above 55 EeV within 18° direction radio galaxy Centaurus A. However, origin remains elusive. We simulate propagation different species coming from in Galactic magnetic fields and find that only nuclear charge Z ≲ 10 can avoid being deflected outside window On other hand, considering increasingly heavy composition UHECRs at highest...
We present the results of long-term hard X-ray monitoring high-mass binary 2S 0114+65 with INTEGRAL/IBIS from 2003 to 2008. is a variable source luminosities 1035–4 × 1036 erg s−1 20 100 keV due accretion rate changes in different orbital phases. In several observations when was bright, we found pulse period evolution ∼2.67 h 2.63 2008, spin-up neutron star ∼1.09 10−6 s s−1. Compared previous reported rate, accelerating. The spectral properties 18–100 band which changed phases generally...
Abstract Using archival Chandra observations with a total effective exposure of 323 ks, we derive an updated catalog point sources in the bulge globular cluster M28. The contains 502 X-ray within area ∼475 arcmin 2 , and more than 90% these are first detected this cluster. We find significant dips radial distribution profiles M28, projected distance width dip for bright ( L X ≳ 4.5 × 10 30 erg s −1 ) larger faint ≲ sources. Fitting “generalized King model” gives slightly average mass (1.30 ±...
ABSTRACT Cassiopeia A (Cas A), as the nearby young remnant of a core-collapse supernova, is best candidate for astrophysical studies in supernova explosion and its environment. We studied hard X-ray emission from Cas using 10 year data INTEGRAL observations, first detected non-thermal continuum source up to 220 keV. The 44 Ti line at 68 78 keV confirmed by our observations with mean flux ∼(2.2 ± 0.4) × −5 ph cm −2 s −1 , corresponding yield (1.3 −4 M ⊙ . 3 500 can be fit thermal...
Spin period variations and hard X-ray spectral properties of Be/X-ray pulsar GRO J1008-57 are studied with INTEGRAL observations. The pulsation periods at 93.66 s in 2004 93.73 2009 determined. Pulse profiles during outbursts energy dependent: double-peak profile soft bands 3-7 keV single-peak X-rays above 7 keV. has undergone a spin-down trend from 1993-2009 rate 4.1x10^-5 day^-1, might transfer into spin-up after 2009. spectra 3-100 fitted photon index 1.4 cutoff energies 23-29 We find...
ABSTRACT We report the orbital X-ray variability of high-mass binary (HMXB) GX 301−2. 301−2 underwent a spin-up process in 2018–2020 with period evolving from ∼685–670 s. The energy-resolved pulse profiles pulsar at 1–60 keV varied single-peaked and sinusoidal shapes to multipeaked ones across different phases. Pulse fractions over orbit had negative correlations flux. broad-band energy spectrum can be described partially covered negative–positive cut-off power-law continuum model. Near...
A LHAASO-KM2A prototype array, which is about 1% of the full one, had been in stable operation for 3 years from 2014 to 2016. This work presents a combined measurement shower muons and electromagnetic particles using its data. Benefiting wide dynamic range muon detectors surrounding detector content was studied detail showers with energies tens TeV PeV. The results are compatible prediction Monte Carlo simulation no obvious excess observed when taking into account that mass composition...
Abstract We have designed and developed the digital correlation receiver for Mingantu Spectral Radioheliograph (MUSER). The MUSER is implemented to sample, channelise, correlate a 400 MHz wide solar radio signal of 40-antenna output from intermediate-frequency array 60-antenna high-frequency array. polyphase filter channeliser used wide-band channelisation proved be efficient realise narrow-band filtering ( ${\sim}25$ MHz) in high-speed signal-processing pipeline (sampling rate ${\sim}1$...
The anomalous X-ray pulsar 4U 0142+61 was studied by the INTEGRAL observations. hard spectrum of 18 -- 500 keV for derived using near 9 years INTEGRAL/IBIS data. We obtained average with all available can be fitted a power-law an exponential high energy cutoff. This is well $\Gamma\sim 0.51\pm 0.11$ plus cutoff at $128.6\pm 17.2$ keV. flux source from 20 150 showed no significant variations (within 20$\%$) 2003 2011. spectral profiles have some variability in nine years: photon index varied...
The synchrotron radiation from secondary electrons and positrons (SEPs) generated by hadronic interactions in the shock of supernova remnant (SNR) could be a distinct evidence cosmic ray (CR) production SNR shocks. Here we provide method where observed gamma-ray flux SNRs, created pion decays, is directly used to derive SEP distribution hence spectrum. We apply three bright SNRs. In young RX J1713.7-3946, if GeV-TeV gamma-rays are origin magnetic field $B\gtrsim 0.5$mG, SEPs may produce...