Mid-Infrared Diagnostic Diagrams and the Starburst-AGN Connection

The mid infrared regime is little affected by extinction, and it contains a plethora of spectroscopic information. The Infrared Space Observatory (ISO) has provided access to this wealth of information. Here I present new results from a study of ISO SWS spectra of about 30 AGNs, concentrating on diagnostic digrams to distinguish between star formation and AGNs as energy source in dusty galaxies (such as ULIRGs), and to discuss the Starburst AGN connection in general. Further results and all details of this study can be found in Sturm et al. (2002).

AGN: The Gamma-Ray Status after CGRO

By detecting more than 100 AGN at γ ray energies, the experiments aboard CGRO finally opened the field of extragalactic γ ray astronomy. A general picture has developed which is briefly summarized.

Can Turbulent, High-density Gas Form Stars in Molecular Clouds: A Case Study in Ophiuchus

Star formation is governed by the interplay between gravity and turbulence in most of molecular clouds.Recent theoretical works assume that dense gas,whose column density is above a critical value in the column density probability distribution function(N-PDF),where gravity starts to overcome turbulence,becomes star-forming gas and will collapse to form stars.However,these high-density gases will include some very turbulent areas in the clouds.Will these dense but turbulent gases also form stars?We test this scenario in Ophiuchus molecular cloud using N-PDF analysis and find that at least in some regions,the turbulent,dense gas is not forming stars.We identified two isolated high-density structures in Ophiuchus,which are gravitationally unbound and show no sign of star formation.Their high densities may come from turbulence.

Cumulant Structure Factors of Jellium

For the ground state of the homogeneous electron gas (jellium), it is shown how the cumulant decomposition of the 2-matrix leads to the cumulant decomposition of the structure factors Sa,p(q) for the antiparallel (a) and parallel (p) spin pairs and how it simultaneously allows one to derive the momentum distribution n(k), which is a one-body quantity [Phys. Rev. A 86, 012508 (2012)]. The small-q and large-q behavior of Sa,p(q), and their normalizations are derived and compared with the results of P. Gori-Giorgi et al. [Physica A 280, 199 (2000) and Phys. Rev. B 61, 7353 (2000)].

Green’s Functions and DOS for Some 2D Lattices

In this presentation we present the Green’s functions and density of states for the most frequently encountered 2D lattices: square, triangular, honeycomb, kagome, and Lieb lattice. Though the results are well known, we hope that its derivation performed in a uniform way provides some pedagogical value.

New insights into AGNs with low-mass black holes and high accretion rates:the case of narrow-line Seyfert 1 galaxies

Narrow-line Seyfert 1(NLS1) galaxies are believed to harbor low-mass black holes accreting at high rates,and they are therefore important targets when studying the nature of black hole growth,galaxy evolution,and accretion physics.We have rigorously studied the physical properties of a sample of NLS1 galaxies.We briefly review previous findings and present new results,including:(1) The locus of NLS1 galaxies on the MBH-σ plane,which we find to follow the relation of non-active galaxies after removing objects obviously dominated by outflows.(2) The presence of "blue outliers" which hint at extreme outflows as they would be predicted from merger models.(3) More subtle evidence for winds and outflows across the whole NLS1 population.(4) New correlations and trends which link black hole mass,Eddington ratio and physical parameters of the emission-line region.A new element is added to the eigenvector 1 space based on a principal component analysis,which aims at identifying the main drivers of AGN correlation properties.

More than softer-when-brighter: The X-ray powerlaw spectral variability in NGC 4051

The powerlaw X-ray spectra of active galactic nuclei at moderate to high accretion rates normally appear softer when they brighten,for which the underlying mechanisms are yet unclear.Utilizing XMM-Newton observations and excluding photons<2 keV to avoid contamination from the soft excess,in this work we scrutinize the powerlaw spectral variability of NCG 4051 from two new aspects.We first find that a best-fit"softer-when-brighter"relation is statistically insufficient to explain the observed spectral variabilities,and intervals deviated from the empirical relation are clearly visible in the light curve of 2-4 ke V/4-10 keV count rate ratio.The deviations are seen not only between but also within individual XMM-Newton exposures,consistent with random variations of the corona geometry or inner structure(with timescales as short as^1 ks),in addition to those behind the smooth"softer-when-brighter"trend.We further find the"softer-when-brighter"trend gradually weakens with the decreasing timescale(from^100 ks down to 0.5 ks).These findings indicate that the powerlaw spectral slope is not solely determined by its brightness.We propose a two-tier geometry,including flares/nano-flares on top of the inner disc and an embedding extended corona(heated by the flares,in analogy to solar corona)to explain the observations together with other observational clues in literature.Rapid spectral variabilities could be due to individual flares/nano-flares,while slow ones are driven by the variations in the global activity of inner disc region(akin to the variation of solar activity,but not the accretion rate)accompanied with heating/cooling and inflation/contraction of the extended corona.

Dipolar spin relaxation of divacancy qubits in silicon carbide

Divacancy spins implement qubits with outstanding characteristics and capabilities in an industrial semiconductor host On the other hand,there are still numerous open questions about the physics of these important defects,for instance,spin relaxation has not been thoroughly studied yet.Here,we carry out a theoretical study on environmental spin-induced spin relaxation processes of divacancy qubits in the 4H polytype of silicon carbide(4H-SiC).We reveal all the relevant magnetic field values where the longitudinal spin relaxation time T,drops resonantly due to the coupling to either nuclear spins or electron spins.We quantitatively analyze the dependence of the T,time on the concentration of point defect spins and the applied magnetic field and provide ananalytical expression.We demonstrate that dipolar spin relaxation plays a significant role both in as-grown and ion-implanted samples and it often limits the coherence time of divacancy qubits in 4H-SiC.

Measurement of away-side broadening with self-subtraction of flow in Au+Au collisions at √sNN=200 GeV

High transverse momentum(pT)particle production is suppressed owing to the parton(jet)energy loss in the hot dense medium created in relativistic heavy-ion collisions.Redistribution of energy at low-to-modest pT has been difficult to measure,owing to large anisotropic backgrounds.We report a data-driven method for background evaluation and subtraction,exploiting the away-side pseudorapidity gaps,to measure the jetlike correlation shape in Au+Au collisions at √sNN=200 GeV in the STAR experiment.The correlation shapes,for trigger particles pT>3GeV/c and various associated particle pT ranges within 0.5<pT<10GeV/c,are consistent with Gaussians,and their widths increase with centrality.The results indicate jet broadening in the medium created in central heavy-ion collisions.

Millimeter gap contrast as a probe for turbulence level in protoplanetary disks

Turbulent motions are believed to regulate angular momentum transport and influence dust evolution in protoplanetary disks.Measuring the strength of turbulence is challenging through gas line observations because of the requirement for high spatial and spectral resolution data,and an exquisite determination of the temperature.In this work,taking the well-known HD 163296 disk as an example,we investigated the contrast of gaps identified in high angular resolution continuum images as a probe for the level of turbulence.With self-consistent radiative transfer models,we simultaneously analyzed the radial brightness profiles along the disk major and minor axes,and the azimuthal brightness profiles of the B67 and B100 rings.By fitting all the gap contrasts measured from these profiles,we constrained the gas-to-dust scale height ratioΛto be 3.0^(+0.3)_(−0.8),1.2^(+0.1)_(−0.1),and≥6.5 for the D48,B67,and B100 regions,respectively.The varying gas-to-dust scale height ratios indicate that the degree of dust settling changes with radius.The inferred values forΛtranslate into a turbulence level of α_(turb)<3×10^(−3) in the D48 and B100 regions,which is consistent with previous upper limits set by gas line observations.However,turbulent motions in the B67 ring are strong with α_(turb)∼1.2×10^(−2).Due to the degeneracy betweenΛand the depth of dust surface density drops,the turbulence strength in the D86 gap region is not constrained.

Measurement of the integrated luminosity of the Phase 2 data of the Belle Ⅱ experiment

From April to July 2018,a data sample at the peak energy of the T(4 S) resonance was collected with the Belle Ⅱ detector at the SuperKEKB electron-positron collider.This is the first data sample of the Belle Ⅱ experiment.Using Bhabha and digamma events,we measure the integrated luminosity of the data sample to be(496.3±0.3±3.0) pb-1,where the first uncertainty is statistical and the second is systematic.This work provides a basis for future luminosity measurements at Belle Ⅱ.

费曼积分作为一类新的特殊函数

Feynman integrals(FIs)serve as fundamental components of perturbative quantum field theory.The study of FIs is important for both exploring the mysteries of quantum field theories and their phenomenological applications,particularly in particle physics.A significant amount of effort has been devoted to analytically calculating FIs,with the goal of expressing them as linear combinations of special functions.

A Note on Black Holes in Asymptotically Lifshitz Spacetime

We investigate several aspects of exact black hole solutions in asymptotically Lifshitz spacetime. Firstly,we calculate the tidal forces and find that in the near horizon region of such black hole backgrounds, the tidal forces diverge in the near extremal limit. Secondly, we evaluate the Wilson loops in both extremal and finite temperature cases. Finally, we obtain the corresponding shear viscosity and square of the sound speed and find that the ratio of shear viscosity to entropy density takes the universal value 1/4π in arbitrary dimensions while the square of the speed of sound saturates the conjectured bound 1/3 in five dimensions.

Observatory science with eXTP

In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry(eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.

从星系中星际介质（ISM）的观察到自一致模拟

2002年的“欧洲和国家联合天文学会议（JENAM）”在葡萄牙举行，会议的主题为：从星系中星际介质（ISM）的观察到自一致模拟，会议上的报告发表在2004年的《天体物理和空间科学》杂志289卷，3～4期，本书为该期的重新出版本。