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K. Xiao

Publications and source records attributed to K. Xiao.

6 recordsLinked to original sources

Atomic-scale investigation of $γ$-Ga$_2$O$_3$ deposited on MgAl$_2$O$_4$ and its relationship with $β$-Ga$_2$O$_3$

Nominally phase-pure $γ$-$Ga_2O_3$ was deposited on (100) $MgAl_2O_4$ within a narrow temperature window centered at $\sim$470 $^{\circ}$C using metal-organic chemical vapor deposition (MOCVD). The film deposited at 440 $^{\circ}$C exhibited either poor crystallization or an amorphous structure; the film grown at 500 $^{\circ}$C contained both $β$-$Ga_2O_3$ and $γ$-$Ga_2O_3$. A nominally phase-pure $β$-$Ga_2O_3$ film was obtained at 530 $^{\circ}$C. Atomic-resolution scanning transmission electron microscopy (STEM) investigations of the $γ$-$Ga_2O_3$ film grown at 470 $^{\circ}$C revealed a high density of antiphase boundaries. A planar defect model developed for $γ$-$Al_2O_3$ was extended to explain the stacking sequences of the Ga sublattice observed in the STEM images of $γ$-$Ga_2O_3$. The presence of the 180$^{\circ}$ rotational domains and 90$^{\circ}$ rotational domains of $β$-$Ga_2O_3$ inclusions within the $γ$-$Ga_2O_3$ matrix is discussed within the context of a comprehensive investigation of the epitaxial relationship between those two phases in the as-grown film at 470 $^{\circ}$C and the same film annealed at 600 $^{\circ}$C. The results led to the hypotheses that (i) incorporation of certain dopants including Si, Ge, Sn, Mg, Al, and Sc, into $β$-$Ga_2O_3$, locally stabilizes the "$γ$-phase" and (ii) the site preference(s) for these dopants promotes the formation of the "$γ$-phase" and/or $γ$-$Ga_2O_3$ solid solutions. However, in the absence of such dopants, pure $γ$-$Ga_2O_3$ remains the least stable $Ga_2O_3$ polymorph, as indicated by its very narrow growth window, lower growth temperatures relative to other $Ga_2O_3$ polymorphs, and the largest calculated difference in Helmholtz free energy per formula unit between $γ$-$Ga_2O_3$ and $β$-$Ga_2O_3$ than all other polymorphs.

cond-mat.mtrl-sci

J-PLUS: Towards an homogeneous photometric calibration using Gaia BP/RP low-resolution spectra

We present the photometric calibration of the twelve optical passbands for the Javalambre Photometric Local Universe Survey (J-PLUS) third data release (DR3), comprising 1642 pointings of two square degrees each. We selected nearly 1.5 million main sequence stars with a signal-to-noise ratio larger than ten in the twelve J-PLUS passbands and available low-resolution (R = 20-80) spectrum from the blue and red photometers (BP/RP) in Gaia DR3. We compared the synthetic photometry from BP/RP spectra with the J-PLUS instrumental magnitudes, after correcting for the magnitude and color terms between both systems, to obtain an homogeneous photometric solution for J-PLUS. To circumvent the current limitations in the absolute calibration of the BP/RP spectra, the absolute color scale was derived using the locus of 109 white dwarfs closer than 100 pc with a negligible interstellar extinction. Finally, the absolute flux scale was anchored to the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) photometry in the r band. The precision of the J-PLUS photometric calibration, estimated from duplicated objects observed in adjacent pointings and by comparison with the spectro-photometric standard star GD 153, is ~12 mmag in u, J0378, and J0395; and ~7 mmag in J0410, J0430, g, J0515, r, J0660, i, J0861, and z. The estimated accuracy in the calibration along the surveyed area is better than 1% for all the passbands. The Gaia BP/RP spectra provide a high-quality, homogeneous photometric reference in the optical range across the full-sky, in spite of their current limitations as an absolute reference. The calibration method for J-PLUS DR3 reaches an absolute precision and accuracy of 1% in the twelve optical filters within an area of 3284 square degrees.

astro-ph.SR

First-principles study of optical, elastic anisotropic and thermodynamic properties of TiN under high temperature and high pressure

The optical, elastic anisotropic and thermodynamic properties of TiN in the NaCl (B1) structure are analyzed in detail in the temperature range from 0 to 2000 K and the pressure range from 0 to 20 GPa. From the calculated dielectric constants, a first order isostructural phase transition between 29 and 30 GPa is found for TiN. The absorption spectra exhibit high values ranging from the far infrared region to the ultra-violet one. The anisotropy value of Young's modulus of TiN is smaller than that of c-BN at 0 GPa and the anisotropy of TiN clearly increases with an increase of pressure. The effects of pressure and temperature on the bulk modulus, Grüneisen parameter, Gibbs free energy, and Debye temperature are significant. The Grüneisen parameter of TiN is much larger than that of c-BN. At temperatures below 1000 K, TiN's heat capacity is much larger than that of c-BN.

cond-mat.mtrl-sci

Higher Moments of Net-Baryon Distribution as Probes of QCD Critical Point

It is crucially important to find an observable which is independent on the acceptance and late collision process, in order to search for the possible Critical Point predicted by QCD. By utilizing A Multi-Phase Transport (AMPT) model and Ultra Relativistic Quantum Molecular Dynamics (UrQMD) model, we study the centrality and evolution time dependence of higher moments of net-baryon distribution in Au + Au collisions at $\sqrt{s_{NN}}=17.3$ GeV. The results suggest that Kurtosis and Skewness are less sensitive to the acceptance effect and late collision process. Thus, they should be good observables providing the information of the early stage of heavy ion collision. In addition, our study shows that the Kurtosis times $σ^{2}$ of net-proton distribution are quite different to that of net-baryon when collisions energy is lower than $\sqrt{s_{NN}}$ = 20 GeV, the Monte Calor calculations on Kurtosis$\cdotσ^{2}$ have a deviation from the theoretical predictions.

nucl-th

IRAC Observations of CO J=4-3 High-Velocity Cloud in the 30 Doradus Complex in the Large Magellanic Cloud

We compare the CO 2-1 observations against previously taken CO 4-3 observations and analyze the spatial distribution of young stellar objects (YSO's) within the cloud using the Spitzer IRAC observations of the 30 Doradus complex. Both peaks of CO 2-1 and 4-3 emitting clouds coincide with the densest region of the filaments where multiple shells are colliding. We find that the YSO's are clustered in the southern ridge of the warm and dense molecular gas clouds traced by CO J=4-3, indicating a filamentary structure of star formation throughout the 30 Doradus. We also find that some of Class I YSO's candidates which are likely to be associated with a high-velocity component of CO 4-3 emitting clouds are present. This is a bona fide place where the triggered star formation had happened and newly formed stars may have produced such a high-velocity outflow interacting with the surrounding molecular cloud material.

astro-ph

Evolution characteristics of central black hole of magnetized accretion disc

Evolution characteristics of a Kerr black hole (BH) are investigated by considering coexistence of disc accretion with the Blandford-Znajek process (the BZ process). (i) The rate of extracting energy from the rotating BH in the BZ process and that in MC process are expressed by a unified formula, which is derived by using an improved equivalent cicuit. (ii) The mapping relation between the angular coordinate on the BH horizon and the radial coordinate on the disc is given in the context of general relativity and conservation of magnetic flux. (iii) The power and torque in the BZ process are compared with those in MC process in detail. (iv)Evolution characteristics of the BH and energy extracting efficiency are discussed by using the characteristics functions of BH evolution in the corresponding parameter space. (v) Power dissipation on the BH horizon and BH entropy increase are discussed by considering the coexistence of the above energy mechanisms.

astro-ph