9,849 research outputs found

    Limits on luminosity and mass accretion rate of a radiation pressure dominated accretion disc

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    There is a maximum for the gravity of a black hole in the vertical direction in the accretion disc. Outflows may probably be driven from the disc if the radiation flux of the disc is greater than a critical value corresponding to the maximal vertical gravity. We find that outflows are driven by the radiation force from the disc if the accretion rate is greater than the Eddington rate. The radiation of the disc is therefore limited by such outflows. The disc luminosity, L=L_Edd\propto ln mdot, at large-mdot cases. The Eddington ratio of the disc is ~3 for mdot~100, which is significantly lower than that of a conventional slim disc without outflows. This implies that the emission from some ultra-luminous X-ray sources with highly super Eddington luminosity should be Doppler beamed, or intermediate mass black holes are in these sources instead of stellar mass black holes. The spectra of the discs with outflows are saturated in the high frequency end provided mdot>2. We suggest that the saturated emission can be observed to estimate the masses of the black holes accreting at high rates, such as the narrow-line Seyfert galaxies, with the model calculations. The rate of the mass accreted by the black hole is always around the Eddington rate even if the mass accretion rate at the outer radius is very high, because most of the gas is removed into the outflows. This implies that the luminous quasars at high redshifts z>6 should have grown up through persistent accretion at a rate close to the Eddington rate.Comment: 8 pages, accepted by MNRA

    Beyond Binaries: When Artists with Disabilities Experiment with Ink, Brush, Water, and Xuan Paper

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    The disappearance of a narrow Mg II absorption system in quasar SDSS J165501.31+260517.4

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    In this letter, we present for the first time, the discovery of the disappearance of a narrow Mg II λλ2796,2803\lambda\lambda2796,2803 absorption system from the spectra of quasar SDSS J165501.31+260517.4 (ze=1.8671z_{\rm e}=1.8671). This absorber is located at zabs=1.7877z_{\rm abs} =1.7877, and has a velocity offset of 8,423 km s−18,423\rm ~km~s^{-1} with respect to the quasar. According to the velocity offset and the line variability, this narrow Mg II λλ2796,2803\lambda\lambda2796,2803 absorption system is likely intrinsic to the quasar. Since the corresponding UV continuum emission and the absorption lines of another narrow Mg II λλ2796,2803\lambda\lambda2796,2803 absorption system at zabs=1.8656z_{\rm abs}=1.8656 are very stable, we think that the disappearance of the absorption system is unlikely to be caused by the change in ionization of absorption gas. Instead, it likely arises from the motion of the absorption gas across the line of sight

    Mandarin Singing Voice Synthesis Based on Harmonic Plus Noise Model and Singing Expression Analysis

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    The purpose of this study is to investigate how humans interpret musical scores expressively, and then design machines that sing like humans. We consider six factors that have a strong influence on the expression of human singing. The factors are related to the acoustic, phonetic, and musical features of a real singing signal. Given real singing voices recorded following the MIDI scores and lyrics, our analysis module can extract the expression parameters from the real singing signals semi-automatically. The expression parameters are used to control the singing voice synthesis (SVS) system for Mandarin Chinese, which is based on the harmonic plus noise model (HNM). The results of perceptual experiments show that integrating the expression factors into the SVS system yields a notable improvement in perceptual naturalness, clearness, and expressiveness. By one-to-one mapping of the real singing signal and expression controls to the synthesizer, our SVS system can simulate the interpretation of a real singer with the timbre of a speaker.Comment: 8 pages, technical repor
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