新型高超音速静压探针的设计和实验

参考了近40年来国外有关超音速和高超音速静压探针的研究成果,设计了多种并发展了二种高超音速静压探针。它们可精确地用于持续工作流场仅为30ms的流场静压测量。实测静压与自由流静压比p_(s,m)/p_(s,∞)=1.009;马赫数比M_(∞m)/M_(∞,)=0.993。实验在加拿大多伦多大学宇航研究院的高超音速炮风洞里完成。炮风洞喷管出口气流特性是:(空气)自由流总压比_(t,∞)=25.5MPa,总温T_(t,∞)=1000K;马赫数M_∞=8.30;自由流静压p_(s,∞)=2.13kPa;雷诺数R_e=3.2×10~7。以探针直径D为基准的R_(e,D)=34,000～52,800。这种探针己被用于“管内高超音速流场发展实验研究”中了。

暗晕子结构的数值搜寻与统计性质

宇宙学数值模拟预言的暗晕及其子结构的统计性质,被广泛应用于星系形成模型、近邻宇宙学、红移巡天、宇宙大尺度结构、引力透镜和暗物质搜寻等研究领域。在精确宇宙学时代,随着天文观测能力的不断增长,人们对模型精度提出了更高的要求,因此,数值模拟及其分析工具将继续起到不可替代的巨大作用。数值模拟中物质结构的性质往往与具体的搜寻算法有关,从最初通过数值模拟发现子晕到现在的20年里,结构搜寻算法有了极大的发展,新算法不断涌现。了解不同数值搜寻算法的实现及其差异,有助于分析模拟结果的系统差和不确定性,增强研究的可重复性。通过总结现代子晕数值搜寻的基本方法,并以几种典型的搜寻算法为例,探讨了它们之间的异同,及其对相关研究的影响;回顾了子晕的基本统计性质,包括质量函数、空间分布和密度轮廓等,以及这些统计结果对搜寻算法的依赖。此外,还讨论了重子物理的影响。

Neutrino Mass Constraints from Reconstructing the Large-scale Structure:Systematic Uncertainty

We examine the possibility of applying the baryonic acoustic oscillation reconstruction method to improve the neutrino massΣm_νconstraint.Thanks to the Gaussianization of the process,we demonstrate that the reconstruction algorithm could improve the measurement accuracy by roughly a factor of two.On the other hand,the reconstruction process itself becomes a source of systematic error.While the algorithm is supposed to produce the displacement field from a density distribution,various approximations cause the reconstructed output to deviate on intermediate scales.Nevertheless,it is still possible to benefit from this Gaussianized field,given that we can carefully calibrate the“transfer function”between the reconstruction output and theoretical displacement divergence from simulations.The limitation of this approach is then set by the numerical stability of this transfer function.With an ensemble of simulations,we show that such systematic error could become comparable to statistical uncertainties for a DESI-like survey and be safely neglected for other less ambitious surveys.

Féeton(B-L gauge boson)dark matter for the 511-keV gamma-ray excess and the prediction of low-energy neutrino flux

The féeton is the gauge boson of the U(1)_(B−L) gauge theory.If the gauge coupling constant is extremely small,the féeton becomes a candidate for dark matter.We show that its decay to a pair of an electron and a positron explains the observed Galactic 511-keV gamma-ray excess in a consistent manner.This féeton dark matter decays mainly into pairs neutrino and anti-neutrino.Future low-energy experiments with improved directional capability will enable capturing these neutrino signals.The seesaw-motivated parameter space predicts a relatively short féeton lifetime that is comparable to the current cosmological constraint.

Quintom cosmology and modified gravity after DESI 2024

We reconstruct the cosmological background evolution under the scenario of dynamical dark energy through the Gaussian process approach,using the latest Dark Energy Spectroscopic Instrument(DESI)baryon acoustic oscillations(BAO)combined with other observations.Our results reveal that the reconstructed dark-energy equation-of-state(EoS)parameter w(z)exhibits the so-called quintom-B behavior,crossing-1 from phantom to quintessence regime as the universe expands.We investigate under what situation this type of evolution could be achieved from the perspectives of field theories and modified gravity.In particular,we reconstruct the corresponding actions for f(R),f(T),and f(Q)gravity,respectively.We explicitly show that,certain modified gravity can exhibit the quintom dynamics and fit the recent DESI data efficiently,and for all cases the quadratic deviation from theΛCDM scenario is mildly favored.

The mass of our Milky Way

We perform an extensive review of the numerous studies and methods used to determine the total mass of the Milky Way.We group the various studies into seven broad classes according to their modeling approaches.The classes include:i)estimating Galactic escape velocity using high velocity objects;ii)measuring the rotation curve through terminal and circular velocities;iii)modeling halo stars,globular clusters and satellite galaxies with the spherical Jeans equation and iv)with phase-space distribution functions;v)simulating and modeling the dynamics of stellar streams and their progenitors;vi)modeling the motion of the Milky Way,M31 and other distant satellites under the framework of Local Group timing argument;and vii)measurements made by linking the brightest Galactic satellites to their counterparts in simulations.For each class of methods,we introduce their theoretical and observational background,the method itself,the sample of available tracer objects,model assumptions,uncertainties,limits and the corresponding measurements that have been achieved in the past.Both the measured total masses within the radial range probed by tracer objects and the extrapolated virial masses are discussed and quoted.We also discuss the role of modern numerical simulations in terms of helping to validate model assumptions,understanding systematic uncertainties and calibrating the measurements.While measurements in the last two decades show a factor of two scatters,recent measurements using Gaia DR2 data are approaching a higher precision.We end with a detailed discussion of future developments in the field,especially as the size and quality of the observational data will increase tremendously with current and future surveys.In such cases,the systematic uncertainties will be dominant and thus will necessitate a much more rigorous testing and characterization of the various mass determination methods.

Detecting warm dark maDetecting warm dark matter by the stochastic gravitational wavestter by the stochastic gravitational waves

NANOGrav has recently reported the detection of a common-spectrum process via the time-of-arrival data of 47 millisecond pulsars[1],which could be interpreted by a stochastic gravitational wave background(SGWB)in the nanohertz frequency band(f∼10−9 Hz)with energy density parameterΩGW∼10−9.Despite the vague quadrupole correlation that obstructs the identification of gravitational waves,this report hints the possibility of some new physics at around or below 100 MeV that can generate nanohertz gravitational waves by,for instance,the first order phase transition(FOPT).

Precision Higgs physics at the CEPC

The discovery of the Higgs boson with its mass around 125 GeV by the ATLAS and CMS Collaborations marked the beginning of a new era in high energy physics.The Higgs boson will be the subject of extensive studies of the ongoing LHC program.At the same time,lepton collider based Higgs factories have been proposed as a possible next step beyond the LHC,with its main goal to precisely measure the properties of the Higgs boson and probe potential new physics associated with the Higgs boson.The Circular Electron Positron Collider(CEPC)is one of such proposed Higgs factories.The CEPC is an e^+e^- circular collider proposed by and to be hosted in China.Located in a tunnel of approximately 100 km in circumference,it will operate at a center-of-mass energy of 240 GeV as the Higgs factory.In this paper,we present the first estimates on the precision of the Higgs boson property measurements achievable at the CEPC and discuss implications of these measurements.