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	1. Are crystalline silicates and amorphous silicates spatially separated in protoplanetary disks ?
	LI Moping,LI Aigen
	Astronomy 09 May 2017
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	Abstract:Crystalline silicates have been found in comets, in protoplanetary disks around young pre-main sequence stars, in debris disks around main-sequence stars, and in dust shells around evolved stars. Their infrared (IR) emission spectra indicate that they are predominantly magnesium (Mg)-rich and iron (Fe)-poor or even Fe-free. The Stardust cometary samples of crystalline silicate minerals are also predominantly Fe-poor. The Fe content of crystalline silicates not only affects the peak wavelength, width and strength of their vibrational features in the IR, but also affects their ultraviolet (UV) and visual absorptivities. Taking the young Herbig Ae star HD 142527 as a test case, we quantitatively demonstrate that, as a consequence of the latter effect, the crystallinity degree of silicate dust might have been substantially underestimated in various astrophysical regions, and the non-detection of the crystalline silicate emission features does not necessarily imply the absence of crystalline silicate dust; instead, crystalline silicates could be present but are just not heated sufficiently to emit at their characteristic IR vibrational bands.
	TO cite this article:LI Moping,LI Aigen. Are crystalline silicates and amorphous silicates spatially separated in protoplanetary disks ?[OL].[ 9 May 2017] http://en.paper.edu.cn/en_releasepaper/content/4732592


	2. The universal “heartbeat” oscillications in black hole systems accross the mass-scale
	Wu Qingwen,Bozena Czerny,Mikolaj Grzedzielski,Agnieszka Janiuk,Wei-Min Gu,Ai-jun Dong,Xiao-Feng Cao,Bei You,Zhen Yan,Mou-Yuan Sun
	Astronomy 09 October 2016
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	Abstract:The hyperluminous X-ray source (HLX-1, the peak X-ray luminosity $sim 10^{42} m erg s^{-1}$) near the spiral galaxy ESO 243-49 is possibly the best candidate for intermediate mass black hole (IMBH), which underwent recurrent outbursts with a period of $sim 400$ days. The physical reason for this quasi-periodic variability is still unclear. We explore the possibility of radiation-pressure instability in accretion disk by modeling the light curve of HLX-1, and find that it can roughly reproduce the duration, period and amplitude of the recurrent outbursts HLX-1 with an IMBH of $sim 10^5$ Msun. Our result provides a possible mechanism to explain the recurrent outbursts in HLX-1. We further find a universal correlation between the outburst duration and the bolometric luminosity for the BH sources with a very broad mass range (e.g., X-ray binaries, XRBs, HLX-1 and active galactic nuclei, AGNs), which is roughly consistent with the prediction of radiation-pressure instability of the accretion disk. These results imply that ``heartbeat" oscillations triggered by radiation-pressure instability may appears in different-scale BH systems.
	TO cite this article:Wu Qingwen,Bozena Czerny,Mikolaj Grzedzielski, et al. The universal “heartbeat” oscillications in black hole systems accross the mass-scale[OL].[ 9 October 2016] http://en.paper.edu.cn/en_releasepaper/content/4706442


	3. The Redshifted Hydrogen Balmer and Metastable $m He ~I$ Absorption System in Iron Mini-LoBAL Quasar SDSS J112526.12+002901.3: the Parsec Scale Accretion Inflow?
	Xi-Heng Shi,Peng Jiang,Hui-Yuan Wang,Shao-Hua Zhang,Tuo Ji,Wen-Juan Liu,Hong-Yan Zhou
	Astronomy 24 May 2016
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	Abstract:The accretion of interstellar medium onto the central super massive black holes is widely accepted as the source of the gigantic energy released by the active galactic nuclei. But few observational evidence has been confirmed directly demonstrating the existence of the inflows. The absorption system in the spectra of quasar SDSS J112526.12+002901.3 presents an interesting example, in which the rarely detected features hydrogen Balmer and metastable hei absorption lines are found redshifted to the quasar's rest frame along with the low-ionization metal absorption lines mgii, eii, extit{et al.}. The repeated SDSS spectroscopic observations suggest a transverse velocity smaller than the radial velocity. The motion of the absorbing medium is dominated by infall. The hei lines present a direct indicator to the strength of ionizing flux, while the Balmer lines imply a dense environment. With the help of photoionization simulations, we find the absorbing medium is exposed to the radiation with $Upprox 10^{-1.8}$, and the density is $n(mathrm{H})pprox 10^9 mathrm{cm}^{-3}$. Thus the absorbing medium is located $sim 4 mathrm{pc}$ away from the central engine. According to the similarity in the distance and physical conditions between the absorbing medium and the clumpy torus, the absorption system is strongly proposed as a candidate for the accretion inflow which originates from the inner surface of the torus.
	TO cite this article:Xi-Heng Shi,Peng Jiang,Hui-Yuan Wang, et al. The Redshifted Hydrogen Balmer and Metastable $m He ~I$ Absorption System in Iron Mini-LoBAL Quasar SDSS J112526.12+002901.3: the Parsec Scale Accretion Inflow?[OL].[24 May 2016] http://en.paper.edu.cn/en_releasepaper/content/4692939


	4. ESO 323-G077 in an X-ray low state observed with Suzaku: evidence for variable circum-nuclear absorber
	SHU Xinwen,WANG Junxian,YANG Huan
	Astronomy 17 May 2016
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	Abstract:We report on a Suzaku observation of the Seyfert 1 galaxy ESO323－G077 obtained in 2011, in which the source is at an historical extremely low X-ray state. A comparison with XMM observation obtained in 2006, Chandra observations in 2010, and other previous X-ray observations, indicates the source has diminished in 2 - 1

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