Design study on the merger for BXERL-FEL

In North China, there is a preliminary proposal for ERL-FEL light source (BXERL-FEL) with its aim at "one machine, two purposes" (the XFEL and ERL work simultaneously). One of the key technologies is the merger section. In this paper, we give the physical design of the merger section for BXERL-FEL which merges three kinds of electron beam.     

The possible electromagnetic counterparts of the first high-probability NSBH merger LIGO/Virgo S190814bv

LIGO/Virgo S190814 bv is the first high-probability neutron star–black hole(NSBH) merger candidate, whose gravitational waves(GWs) triggered LIGO/Virgo detectors at21:10:39.012957 UT, 14 August 2019. It has a probability 99% of being an NSBH merger,with a low false alarm rate(FAR) of one per 1.559 e+25 years. For an NSBH merger,electromagnetic counterparts(especially short gamma-ray bursts(GRBs)) are generally expected. However, no electromagnetic counterpart has been found in the extensive follow-up observing campaign. In the present work, we propose a novel explanation for this null result. In our scenario, LIGO/Virgo S190814 bv is just a GW mirror image of the real NSBH merger which should have been detected before 14 September 2015, but at that time we had no ability to detect its GW signals. The electromagnetic counterparts associated with the real NSBH merger should be found in the archive data before 14 September 2015. In this work, we indeed find nine short GRBs that are possibly electromagnetic counterparts.     

Magnetized hypermassive neutron-star collapse: a central engine for short gamma-ray bursts

A hypermassive neutron star (HMNS) is a possible transient formed after the merger of a neutron-star binary. In the latest axisymmetric magnetohydrodynamic simulations in full general relativity, we find that a magnetized HMNS undergoes "delayed" collapse to a rotating black hole (BH) as a result of angular momentum transport via magnetic braking and the magnetorotational instability. The outcome is a BH surrounded by a massive, hot torus with a collimated magnetic field. The torus accretes onto the BH at a quasisteady accretion rate [FORMULA: SEE TEXT]; the lifetime of the torus is approximately 10 ms. The torus has a temperature [FORMULA: SEE TEXT], leading to copious ([FORMULA: SEE TEXT]) thermal radiation that could trigger a fireball. Therefore, the collapse of a HMNS is a promising scenario for generating short-duration gamma-ray bursts and an accompanying burst of gravitational waves and neutrinos.     

Effects of hyperons in binary neutron star mergers

Numerical simulations for the merger of binary neutron stars are performed in full general relativity incorporating both nucleonic and hyperonic finite-temperature equations of state (EOS) and neutrino cooling. It is found that even for the hyperonic EOS, a hypermassive neutron star is first formed after the merger for the typical total mass ≈2.7M(⊙), and subsequently collapses to a black hole (BH). It is shown that hyperons play a substantial role in the postmerger dynamics, torus formation around the BH, and emission of gravitational waves (GWs). In particular, the existence of hyperons is imprinted in GWs. Therefore, GW observations will provide a potential opportunity to explore the composition of neutron star matter.     

Magnetized neutron-star mergers and gravitational-wave signals

We investigate the influence of magnetic fields upon the dynamics of, and resulting gravitational waves from, a binary neutron-star merger in full general relativity coupled to ideal magnetohydrodynamics. We consider two merger scenarios: one where the stars have aligned poloidal magnetic fields and one without. Both mergers result in a strongly differentially rotating object. In comparison to the nonmagnetized scenario, the aligned magnetic fields delay the full merger of the stars. During and after merger we observe phenomena driven by the magnetic field, including Kelvin-Helmholtz instabilities in shear layers, winding of the field lines, and transition from poloidal to toroidal magnetic fields. These effects not only mediate the production of electromagnetic radiation, but also can have a strong influence on the gravitational waves. Thus, there are promising prospects for studying such systems with both types of waves.     

The Production of FRW Universe and Decay to Particles in Multiverse

In this study, first, it will be shown that as the Hubble parameter, “H”, increases the production cross section for closed and flat Universes increases rapidly at smaller values of “H” and becomes constant for higher values of “H”. However in the case of open Universe, the production cross section has been encountered a singularity. Before this singularity, as the H parameter increases, the cross section increases, for smaller H, (H < 2.5), exhibits a turn-over at moderate values of H, (2.5 < H < 3.5), decreases for larger amount of H After that and for a special value of H, the cross section has been encountered with a singularity. Although the cross section cannot be defined at this singularity but before and after this point, it is certainly equal to zero. After this singularity, the cross section increases rapidly, when H increases. It is shown that if the production cross section of Universe happens before this singularity, it can’t achieve to higher values of Hubble parameter after singularity. More over if the production cross section of Universe situates after the singularity, it won’t get access to values of Hubble parameter less than the singularity. After that the thermal distribution for particles inside the FRW Universes are obtained. It is found that a large amount of particles are produced near apparent horizon due to their variety in their energy and their probabilities. Finally, comparing the particle production cross sections for flat, closed and open Universes, it is concluded that as the value of k increases, the cross section decreases.     

北京大学ERL装置交汇段的研究与设计

 在交汇段设计理论的基础上,针对北京大学ERL的具体情况,对交汇段的束流传输结构进行了优化设计,通过模拟得到了满足要求的一组设计参数;研究了空间电荷效应以及相干同步辐射对束流发射度、能散及包络的影响。结果表明：空间电荷效应对发射度影响不大,但对束流包络影响较明显;相干同步辐射引起的发射度增长及能散较小,且不影响束流包络。     

Insight-HXMT observations of the first binary neutron star merger GW170817

Finding the electromagnetic(EM) counterpart of binary compact star merger, especially the binary neutron star(BNS) merger,is critically important for gravitational wave(GW) astronomy, cosmology and fundamental physics. On Aug. 17, 2017,Advanced LIGO and Fermi/GBM independently triggered the first BNS merger, GW170817, and its high energy EM counterpart,GRB 170817 A, respectively, resulting in a global observation campaign covering gamma-ray, X-ray, UV, optical, IR, radio as well as neutrinos. The High Energy X-ray telescope(HE) onboard Insight-HXMT(Hard X-ray Modulation Telescope) is the unique high-energy gamma-ray telescope that monitored the entire GW localization area and especially the optical counterpart(SSS17 a/AT2017 gfo) with very large collection area(~1000 cm~2) and microsecond time resolution in 0.2-5 MeV. In addition,Insight-HXMT quickly implemented a Target of Opportunity(ToO) observation to scan the GW localization area for potential X-ray emission from the GW source. Although Insight-HXMT did not detect any significant high energy(0.2-5 MeV) radiation from GW170817, its observation helped to confirm the unexpected weak and soft nature of GRB 170817 A. Meanwhile,Insight-HXMT/HE provides one of the most stringent constraints(~10~(-7) to 10~(-6) erg/cm~2/s) for both GRB170817 A and any other possible precursor or extended emissions in 0.2-5 MeV, which help us to better understand the properties of EM radiation from this BNS merger. Therefore the observation of Insight-HXMT constitutes an important chapter in the full context of multi-wavelength and multi-messenger observation of this historical GW event.     

Causal propagation of signals in strangeon matter

The state equation for strangeon matter is very stiff due to the non-relativistic nature of its particles and their repulsive interaction,such that pulsar masses as high as～3 M_⊙ would be expected. However, an adiabatic sound speed, c_s=(?P/?ρ)～(1/2), is usually superluminal in strangeon matter, and the dynamic response of a strangeon star(e.g., binary merger) is not tractable in numerical simulations. In this study, we examined signal propagation in strangeon matter and calculate the actual propagation speed, c_(signal).We found that the causality condition, c_(signal) c, is satisfied and the signal speed is presented as a function of stellar radius.     

A three-dimensional renormalization group bubble merger model for Rayleigh-Taylor mixing

In this paper we formulate a model for the merger of bubbles at the edge of an unstable acceleration driven (Rayleigh-Taylor) mixing layer. Steady acceleration defines a self-similar mixing process, with a time-dependent inverse cascade of structures of increasing size. The time evolution is itself a renormalization group (RNG) evolution, and so the large time asymptotics define a RNG fixed point. We solve the model introduced here at this fixed point. The model predicts the growth rate of a Rayleigh-Taylor chaotic fluid mixing layer. The model has three main components: the velocity of a single bubble in this unstable flow regime, an envelope velocity, which describes collective excitations in the mixing region, and a merger process, which drives an inverse cascade, with a steady increase of bubble size. The present model differs from an earlier two-dimensional (2-D) merger model in several important ways. Beyond the extension of the model to three dimensions, the present model contains one phenomenological parameter, the variance of the bubble radii at fixed time. The model also predicts several experimental numbers: the bubble mixing rate, alpha(b)=h(b)/Agt(2) approximately 0.05-0.06, the mean bubble radius, and the bubble height separation at the time of merger. From these we also obtain the bubble height to the radius aspect ratio. Using the experimental results of Smeeton and Youngs (AWE Report No. O 35/87, 1987) to fix a value for the radius variance, we determine alpha(b) within the range of experimental uncertainty. We also obtain the experimental values for the bubble height to width aspect ratio in agreement with experimental values. (c) 2002 American Institute of Physics.     

关于“对《理论力学教程》中两个问题的讨论”的讨论

文献[2]指出《理论力学教程》中的“一张错误的插图”,给出了所谓“正确”的插图,并修改了《理论力学教程》的公式(3.7.3),该文认为在研究刚体的平面平行运动的§3.7节不用选择转动参照系,宜采用平动参照系.本文作者认为《理论力学教程》的插图3.7.2并没有错,在§3.7节采用转动参照系是研究刚体平面平行运动转动瞬心等问题的需要;公式(3.7.3)也不必作根本上的修改,但对其中坐标分量(x′,y ′)的含义要加注释,以免造成混淆.     

Constraining nuclear equations of state using gravitational waves from hypermassive neutron stars

Latest general relativistic simulations for the merger of binary neutron stars with realistic equations of states (EOSs) show that a hypermassive neutron star of an ellipsoidal figure is formed after the merger if the total mass is smaller than a threshold value which depends on the EOSs. The effective amplitude of quasiperiodic gravitational waves from such hypermassive neutron stars is approximately 6-7 x 10(-21) at a distance of 50 Mpc, which may be large enough for detection by advanced laser interferometric gravitational wave detectors although the frequency is high, approximately 3 kHz. We point out that the detection of such signals may lead to constraining the EOSs for neutron stars.     

伴有靶核核心激发的氘核削裂反应

本文研究了在氘核削裂反应中伴随有靶核核心激发的情况。在这种情况下,假定由于核子-核子剩余相互作用,靶核的组态除了通常壳模型组态外,还混杂有核心激发的组态。同样,剩余核的组态主要是某一种核心激发的组态,但也还混杂有别种组态。在这假定下,给出了所考虑的反应过程的微分截面表示式。它表明,反应截面主要由靶核的组态混合所贡献。一般说来,组态的混合程度不大,故可预期截面数值是较小的。公式还表明,反应角分布的特征峯是由核心在激发后留下来的空穴态的轨道角动量量子数所决定的。这二点结论与这类反应的实验结果是一致的。运用这公式具体估计了六个反应事例的核谱因子,在实验误差内,理论值和从实验的估计值大致相合。     

Phasenfestlegung in den Wannier-Funktionen und einfache Herleitung des Ersatzoperators für Gitterelektronen im Magnetfeld

The motion of cristal electrons in a magnetic field can be described by the well known Hamiltonian, first given byPeierls to zeroth order inB and derived in full generality byKohn. A derivation of this most general result is given here in the most elementary and direct way, which seems possible (as the author believes). The results summed up in section 1 are derived using the gaugeA=1/2B×r which proves to be the most advatageous one for this purpose and using a special choice of phases in constructing Wannier functions from Bloch functions. This choice of phases given and discussed in section 2 seems to be of general interest for any use of Wannier-functions. In section 3 one gets the new Hamiltonian in thek-representation in a closed form by a straightforward calculation after acting with the initial Hamiltonian on certain unorthogonal modified Bloch functions, whose Fourier coefficients with respect tok are the Wannier-Luttinger functions. It consists of an one-band-Hamiltonian for each band and a band-coupling-Hamiltonian for any two bands as well as like metric operators because of the nonorthogonality of the original basis. In section 4 it is shown that the expansion of the operators in a power series ofB is always divergent but asymptotically right for smallB. In the same sense any two nonintersecting bands can be decoupled; the decoupling to first order inB and the zeroth and first order of the one-band-Hamiltonians are given and can in principle be calculated to any order. Section 5 contains some remarks about the range of validity of the asymptotic expansion in powers ofB.     

Streuung von 25 keV-Elektronen an Gasen

The differential cross section of neon, argon, krypton, and xenon for the elastic scattering and for the excitation of optical transitions has been measured. For neon and argon the elastic angular distribution can be described by the cross section calculated according toWentzel andLenz. For krypton and xenon there are considerable deviations from the Wentzel-Lenz cross section. In these cases it is better to calculate the elastic differential cross section from Slater eigenfunctions, from Thomas-Fermi-Dirac or from Hartree-Fock electron density distribution. The differential cross sections for the excitation of optical transitions, so far as measured here, obey for?<? _c the dipol approximation, i.e. for angles not to small the inverse square angular dependence is valid.? _c is higher for the heavier rare gases. The oscillator strengths for some transitions have been determined from the scattering measurements in satisfactory agreement with theoretical values.     

Global spinor fields in space-time

This paper is concerned with space-time manifolds that are space- and time-oriented, causal, and possess spinor structures. Five propositions are proven: (1) If a connected, space- and time-oriented manifold is simply con-nected, then it is non-compact; (2) If such a manifold is simply connected, it admits a spinor structure, which, moreover, is unique; (3) If the space-like section of M is compact, then there exists a global system of orthonormal tetrads on M; (4) The necessary and sufficient condition for every space-time M whose space-like section is compact to admit a spinor structure is that M have a global system of orthonormal tetrads; (5) Every space-time M which can be imbedded in R⁶ admits a spinor structure. It is further suggested that in view of the fact that the existence of a spinor structure is related to homotopy properties, space-time manifolds may be classified in terms of their homotopy groups _i (M), i=1,2, 3,4. In a concluding section, some avenues for future research are discussed.Supported by the National Science Foundation.     

The QCD pomeron in ultraperipheral heavy ion collisions: I. The double $J/\Psi$ production

The contribution of the QCD pomeron to the process is discussed. We focus on the photon-photon collision, with the quasi-real photon coming from the Weizs?cker-Williams spectrum of the nuclei. We calculate the cross section for this process considering the solution of the LLA BFKL equation at zero momentum transfer using a small t approximation for the differential cross section of the subprocess. Furthermore, the impa ct of non-leading corrections to the BFKL equation is also analyzed. In both cases the cross section is found to increase with the energy, predicting considerable values for the LHC energies. Moreover, we compare our results with the Born two-gluon approximation, which is energy independent at the photon level. Our results indicate that the experimental analyses of this process can be useful to discriminate the QCD dynamics at high energies. Received: 12 December 2002 / Published online: 7 March 2003 RID="a" ID="a" e-mail: barros@ufpel.tche.br RID="b" ID="b" e-mail: magnus@if.ufrgs.br     

Analysis of the merger between plasma vortices in a Penning trap

In the paper, the interaction between a finite-size vortex of constant density and a weak, pointlike vortex in a Penning trap is studied analytically. A suitable Fourier representation for the contour of the finite vortex is considered and a model for small perturbations, which is linear with respect to the Fourier coefficients, is deduced. The resonance condition for the surface modes and a sufficient condition for the merger of the vortices not to occur are obtained. The validity of the analytic results is checked with a contour dynamics code making use of a new methodology developed by the authors. Numerical results referred to a case of strongly-interacting vortices are also reported.Received: 18 April 2003, Published online: 12 August 2003PACS: 52.27.Jt Nonneutral plasmas - 52.35.We Plasma vorticity - 47.32.Cc Vortex dynamicsA. DAngola: Present address: Universitá della Basilicata, Dipartimento di Ingegneria e Fisica dellambiente, Contrada Macchia Romana, 85100 Potenza, Italy.     

Coupled-channel calculations of positron-atom scattering at intermediate energies

We present the cross sections for positron collisions with the alkali atoms Li, Na and K in the close-coupling approximation within the framework of a single-active-electron model. Our target basis sets are represented by Li(2s, 3s, 2p, 3p), Na(3s, 4s, 3p, 4p), and K(4s, 5s, 4p, 5p) respectively. The effects of coupling to the lowest lying Ps channels have been investigated by augmenting the target basis sets with the Ps(1s, 2s, 2p) eigenstates. The calculations have been made for impact energies below 50 eV. The interaction between the positron and the alkali target atom is represented by a model potential obtained using a single-active-electron approximation. The effect on elastic scattering and excitation due to the coupling between the direct and the Ps formation channels is found to be of great significance at low impact energies. The case of K is of particular interest. The inclusion of the Ps channels quantitatively reproduces the maximum in the total cross section at about 6 eV as reported in a recent experiment by Parikh et al. We find that the calculated total cross sections for Na and K are in good agreement with the experimental data of Parikh et al. and Kwan et al. respectively in the energy range of 2–50 eV provided allowance is made for the incomplete elastic discrimination in the experiment. The Ps formation reduces the K(4s4p) cross section at all energies below 30 eV and a reduction is also seen in the elastic cross section for energies below about 7 eV. Similar effects are observed in the case of Li. In the case of Na for impact energies between 2 and 20 eV Ps formation significantly reduces the Na(3s3p) excitation cross section, while the elastic scattering cross section increases. The calculated total Ps formation cross sections for Na and K are in good agreement with the preliminary experimental data of Kwan, Stein and co-workers.