Applying deep learning technique to chiral magnetic wave search

The chiral magnetic wave(CMW)is a collective mode in quark-gluon plasma originated from the chiral magnetic effect(CME)and chiral separation effect.Its detection in heavy-ion collisions is challenging owing to significant background contamination.In[Y.S.Zhao et al.,Phys.Rev.C 106,L051901(2022)],we constructed a neural network that accurately identifies the CME-related signal from the final-state pion spectra.In this study,we have generalized this neural network to the case of CMW search.We show that,after an updated training,the neural network effectively recognizes the CMW-related signal.Additionally,we have assessed the performance of the neural network in comparison with other known methods for CMW search.

Gravitational Wave Radiation from Newborn Accreting Magnetars

The observed electromagnetic radiation from some long and short gamma-ray bursts,and neutron stars(NSs),and the theoretical models proposed to interpret these observations together point to a very interesting but confusing problem,namely,whether fall-back accretion could lead to dipole field decay of newborn NSs.In this paper,we investigate the gravitational wave(GW) radiation of newborn magnetars with a fall-back disk formed in both the core-collapse of massive stars and the merger of binary NSs.We make a comparison of the results obtained with and without fall-back accretion-induced dipole-field decay(FADD) involved.Depending on the fall-back parameters,initial parameters of newborn magnetars,and models used to describe FADD,FADD may indeed occur in newborn magnetars.Because of the low dipole fields caused by FADD,the newborn magnetars will be spun up to higher frequencies and have larger masses in comparison with the non-decay cases.Thus the GW radiation of newborn accreting magnetars would be remarkably enhanced.We propose that observation of GW signals from newborn magnetars using future GW detectors may help to reveal whether FADD could occur in newborn accreting magnetars.Our model is also applied to the discussion of the remnant of GW170817.From the post-merger GW searching results of Advanced LIGO and Advanced Virgo we cannot confirm the remnant is a low-dipole-field long-lived NS.Future detection of GWs from GW170817-like events using more sensitive detectors may help to clarify the FADD puzzle.

Generation of Alfvén wave energy during magnetic reconnection in Hall MHD

The effect of the reconnection rate on the generation of Alfvén wave energy is systematically investigated using Hall magnetohydrodynamics（MHD）. It is well known that a decrease in magnetic energy is proportional to the reconnection rate. It is found that an instantaneous increase in Alfvén wave energy in unit Alfvén time is the square dependence on the reconnection rate. The converted Alfvén wave energy is strongly enhanced due to the large increase in the reconnection rate in Hall MHD. For solar-terrestrial plasmas, the maximum converted Alfvén wave energy in unit Alfvén time with the Hall effect can be over 50 times higher than that without the Hall effect during magnetic reconnection.

Probing the Internal Physics of Neutron Stars through the Observed Braking Indices and Magnetic Tilt Angles of Several Young Pulsars

The braking indices of pulsars may contain important information about the internal physics of neutron stars(NSs),such as neutron superfluidity and internal magnetic fields.As a subsequent paper of Cheng et al.,we perform the same analysis as that done in the previous paper to other young pulsars with a steady braking index,n.Combining the timing data of these pulsars with the theory of magnetic field decay,and using their measured magnetic tilt angles,we can set constraints on the number of precession cycles,ξ,which represents the interactions between superfluid neutrons and other particles in the NS interior.For the pulsars considered in this paper,the results show thatξis within the range of a few×10~3 to a few×10~6.Interestingly,for the Crab and Vela pulsars,the constraints onξobtained with our method are generally consistent with that derived from modeling of the glitch rise behaviors of the two pulsars.Furthermore,we find that the internal magnetic fields of pulsar with n<3 may be dominated by the toroidal components.Our results may not only help to understand the interactions between the superfluid neutrons and other particles in the interior of NSs but also be important for the study of continuous gravitational waves from pulsars.

Basic Quantum Magnetic Interaction Based on Detailed Gauss Meter Measurements

Understanding that the magnetic phenomenon is both a particle, khumalon, that organizes itself into a wave formation to travel through a medium, this paper shows proof of this in detail. It can only be doing this because it is traveling through some medium. This paper is about observing relationships that are a result of different polarized magnetic phenomenon forced into relationships. The magnet shows it does not behave differently from other particles;when they have relationships with their “anti” particle, annihilation takes place. Two magnets will always be like a collider, but because the magnetic phenomenon is already unstable and of low energy allows us to see things otherwise difficult with particles of higher energy. Isaac Newton is truly needed in explaining this phenomenon. The magnetic phenomenon adheres to the first two laws of everything. All data can be found on figshare.com, to share.

Numerical simulations of three-dimensional magnetic swirls in a solar flux-tube

We aim to numerically study evolution of Alfv′en waves that accompany short-lasting swirl events in a solar magnetic flux-tube that can be a simple model of a magnetic pore or a sunspot. With the use of the FLASH code we numerically solve three-dimensional ideal magnetohydrodynamic equations to simulate twists which are implemented at the top of the photosphere in magnetic field lines of the flux-tube. Our numerical results exhibit swirl events and Alfv′en waves with associated clockwise and counterclockwise rotation of magnetic lines, with the largest values of vorticity at the bottom of the chromosphere, and a certain amount of energy flux.

Period ratios for standing kink and sausage modes in magnetized structures with siphon flow on the Sun

Standing oscillations with multiple periods have been found in a number of atmospheric struc- tures on the Sun. The ratio of the period of the fundamental to twice the one of its first overtone, P1/2192, is important in applications of solar magneto-seismology. We examine how field-aligned flows impact P1/2P2 of standing modes in solar magnetic cylinders. For coronal loops, the flow effects are significant for both fast kink and sausage modes. For kink modes, they reduce P1/2P2 by up to 17% relative to the static case even when the density contrast between the loop and its surroundings approaches infinity. For sausage modes, the reduction in P1/2P2 due to flow is typically ≤ 5.5% compared with the static case. However, the threshold aspect ratio, only above which can trapped sausage modes be supported, may increase dramatically with the flow magnitude. For photospheric tubes, the flow effect on P1/2P2 is not as strong. However, when applied to sausage modes, introducing field-aligned flows offers more possibilities in interpreting the multiple peri- ods that have recently been measured. We conclude that field-aligned flows should be taken into account to help better understand what causes the departure of P1/2P2 from unity.

Numerical simulations for MHD coronal seismology

Magnetohydrodynamic（MHD） processes are important for the transfer of energy over large scales in plasmas and so are essential to understanding most forms of dynamical activity in the solar atmosphere. The introduction of transverse structuring into models for the corona modifies the behavior of MHD waves through processes such as dispersion and mode coupling. Exploiting our understanding of MHD waves with the diagnostic tool of coronal seismology relies upon the development of sufficiently detailed models to account for all the features in observations. The development of realistic models appropriate for highly structured and dynamical plasmas is often beyond the domain of simple mathematical analysis and so numerical methods are employed. This paper reviews recent numerical results for seismology of the solar corona using MHD.

Simultaneous Zeeman deceleration of polyatomic free radical with lithium atoms

Chemistry in the ultracold regime enables fully quantum-controlled interactions between atoms and molecules,leading to the discovery of the hidden mechanisms in chemical reactions which are usually curtained by thermal averaging in the high temperature.Recently a couple of diatomic molecules have been cooled to ultracold regime based on laser cooling techniques,but the chemistry associated with these simple molecules is highly limited.In comparison,free radicals play a major role in many important chemical reactions,but yet to be cooled to submillikelvin temperature.Here we propose a novel method of decelerating CH_(3),the simplest polyatomic free radical,with lithium atoms simultaneously by travelling wave magnetic decelerator.This scheme paves the way towards co-trapping CH_(3)and lithium,so that sympathetical cooling can be used to preparing ultracold free radical sample.