arXiv subjects

Qiu-He Peng

Publications and source records attributed to Qiu-He Peng.

10 recordsLinked to original sources

arXiv2022

Neutrino Rocket Jet Model: An Explanation of High-velocity Pulsars and their Spin-down Evolution

The fact that the spatial velocity of pulsars is generally higher than that of their progenitor stars has bothered astronomers for nearly 50 years. It has been extensively argued that the high pulsar velocity should be acquired during a natal kick process on a timescale of 100ms - 10s in the supernova explosion, in which some asymmetrical dynamical mechanism plays a key role. However, a satisfactory picture generally is still lacking. In this study, it is argued that the neutrino rocket model can well account for the high speed as well as the long-term evolution behaviors of pulsars. The neutrinos are emitted from superfluid vortex neutrons through the neutrino cyclotron radiation mechanism. The unique characters of left-handed neutrinos and right-handed antineutrinos resulting from the nonconservation of parity in weak interactions play a major role in the spatial asymmetry. The continuous acceleration of pulsars can be naturally explained by this model, which yields a maximum velocity surpassing 1000 km s$^{-1}$. The alignment between the spinning axis and the direction of motion observed for the Crab pulsar (PSR 0531) and the Vela pulsar (PSR 0833) can be well accounted for. The observed correlation between the spin-down rate and the period of long-period pulsars with $P \gtrsim 0.5$s can also be satisfactorily explained.

astro-ph.HE↗

arXiv2020

A Magnetic-Monopole-Based Mechanism to the formation of the Hot Big Bang Modeled Universe

There are some particle physics theories that go beyond the so-called "standard cosmological model" to predict the existence of magnetic monopoles\,(MMs). The discovery of magnetic monopoles would be an incredible breakthrough in high-energy physics. The existence of MMs in the early Universe has been speculated and anticipated from Grand Unified Theory. If MMs exist, the inverse powers of the unification mass will not suppressed the baryon number violating effects of grand unified gauge theories. Therefore, MM catalyzing nucleon decay is a typical strong interaction. This phenomenon is due to the boundary conditions that must be imposed on the core of MM fermion fields. We present a possible mechanism to explain the formation of the Hot Big Bang Cosmology. The main ingredient in our model is nucleon decay catalyzed by magnetic monopoles (i.e., the Rubakov-Callan effect). It is shown that Hot Big Bang developed naturally, because the luminosity due to the Rubakov-Callan effect is much greater than the Eddington luminosity (i.e., $L_m>10^4L_{\rm{Edd}}$).

physics.gen-ph↗

arXiv2018

The Physical Essence of Pulsar Glitch

Based on the magnetic dipole radiation from the 3P2 neutron superfluid vortices (3P2NSFV) in neutron stars, we propose a model of glitch for young pulsars by oscillation between B phase and A phase of 3P2 Neutron superfluid. The main behavior of glitches of pulsars may be naturally explained by our model.

astro-ph.HE↗

arXiv2017

A unified model of supernova driven by magnetic monopoles

In this paper, we first discuss a series of important but puzzling physical mechanisms concerning the energy source, various kinds of core collapsed supernovae explosion mechanisms during central gravitational collapse in astrophysics. We also discuss the puzzle of possible association of $γ$-ray burst with gravitational wave perturbation, the heat source for the molten interior of the core of the earth and finally the puzzling problem of the cooling of white dwarfs. We then make use of the estimations for the space flux of magnetic monopoles (hereafter MMs) and nucleon decay induced by MMs (called the Rubakov-Callen(RC) effect) to obtain the luminosity due to the RC effect. In terms of the formula for this RC luminosity, we present a unified treatment for the heat source of the Earth's core, the energy source for the white dwarf interior, various kinds of core collapsed supernovae (Type II Supernova (SNII), Type Ib Supernova (SNIb), Type Ic Supernova (SNIc), Super luminous supernova (SLSN)), and the production mechanism for $γ$-ray burst. This unified model can also be used to reasonably explain the possible association of the short $γ$-ray burst detected by the Fermi $γ$-ray Burst Monitoring Satellite (GBM) with the LIGO gravitational wave event GW150914 in September 2015.

astro-ph.HE↗

arXiv2017

Strongly screening on electron capture for Nuclides $^{52, 53, 59, 60}$Fe by the Shell-Model Monte Carlo method in pre-supernova

The death of the massive stars due to supernova explosion is a key ingredient in stellar evolution, stellar population synthesis. The electron capture (EC) plays a vital role in supernovae explosions. According to the Shell-Model Monte Carlo (SMMC) method, basing onthe Random Phase Approximation (RPA) and Linear Response Theory Model (LRTM), we study the strongly screening EC rates of nuclides $^{52, 53, 59, 60}$Fe in presupernova. The results show that the screening rates can decrease about 18.66\%. We compare our results with those of Fuller et al. (FFN), Aufderheide et al. (AUFD), and Nabi et al. (NKK)in the case with and without strong electron screening(SES). For the case without SES, our calculations are in very good agreement with those of AUFD in relatively high density surroundings and the maximum error is within 0.35\% at $ρ_7=100$ (e. g., even-even nuclei $^{60}$Fe). However, for odd-A nuclei$^{59}$Fe, our rates are close to one, one, two order magnitude smaller than those of FFN, AUFD, and NKK. For the case with SES, our screening results are about three, two orders magnitude, and 7.27\% lower than those of FFN, AUFD, NKK for $^{60}$Fe, respectively, and it is lower about two, two orders magnitude, and 12.42\% than those of FFN, AUFD, NKK for odd-A nuclide $^{59}$Fe.

nucl-th↗

arXiv2017

Strongly screening electron capture rates of chromium isotopes in presupernova

Taking into account the effect of electron screening on the electron energy and electron capture threshold energy, by using the method of Shell-Model Monte Carlo and Random Phase Approximation theory, we investigate the strong electron screening capture rates of chromium isotopes according to the linear response theory screening model. The strong screening rates can decrease by about 40.43\% (e.g., for $^{60}$Cr at $T_9=3.44,Y_e=0.43$). Our conclusions may be helpful to the researches of supernova explosion and numerical simulation.

nucl-th↗

arXiv2017

Some New Possible Anticipated Signals for Existence of Magnetic Monopoles

We summarize some predictions from the model of supermassive object with magnetic monopoles which match up with recent astronomical observations quantitatively. They may be the signals for existence of magnetic monopoles in the supermassive objects, such as one at the Galactic Center.

astro-ph.HE↗

arXiv2016

A possible influence on standard model of quasars and active galactic nuclei in strong magnetic field

Recent observational evidence indicates that the center of our Milky Way harbours a super-massive object with ultra-strong radial magnetic field (Eatough et al., 2013). Here we demonstrate that the radiations observed in the vicinity of the Galactic Center (GC) (Falcke and Marko 2013) cannot be emitted by the gas of the accretion disk since the accreting plasma is prevented from approaching to the GC by the abnormally strong radial magnetic field. These fields obstruct the infalling accretion flow from the inner region of the disk and the central massive black hole in the standard model. It is expected that the observed radiations near the Galactic Center cannot be generated by the central black hole. We also demonstrate that the observed ultra-strong radial magnetic field near the Galactic Center ( Eatough et al., 2013) cannot be generated by the - turbulence dynamo mechanism of Parker since preliminary qualitative estimate in terms of this mechanism gives a magnetic field strength six orders of magnitude smaller than the observed field strength at . However, both these difficulties or the dilemma of the standard model can be overcome if the central black hole in the standard model is replaced by a supper-massive stellar object containing magnetic monopoles ( SMSOMM, Peng and Chou, 2001). The observed power peaking of the thermal radiation is essentially the same as our theoretical prediction. In addition, the discovery of the ultra-strong radial magnetic field near the Galactic Center can be naturally explained and is consistent with the prediction of our model( Peng and Chou 2001). Furthermore, the observed ultra-strong radial magnetic field in the vicinity of the Galactic Center may be considered as the astronomical evidence for the existence of magnetic monopoles as predicted by the Grand Unified Theory of particle physics.

astro-ph.GA↗

arXiv2011

The meaning inferred from the spin period distribution of normal pulsars

We make statistics about the number distribution of normal radio pulsars according to the pulsar spin period. And find the physical meaning of the traditional statistical method about this problem is very limited. According to the statistical method proposed by us, the distribution rule is exactly the exponentially decay with the spin period increasing, especially important, which can be interpreted as normal radio pulsar number decays as the radiative elements decay. It discloses that though belonging to two different extreme scales of the universe and having different inner active mechanisms, the normal radio pulsars and radiative elements accord with the same varying rule. And like the half decay period of the radiative elements we can also introduce the half decay spin period of the normal radio pulsars.

astro-ph.SR↗

arXiv2005

Elliptical Galaxies with Emission Lines from the Sloan Digital Sky Survey

We present the results of 11 elliptical galaxies with strong nebular emission lines during our study of star formation history along the Hubble sequence. After removing the dilution from the underlying old stellar populations by use of stellar population synthesis model, we derive the accurate fluxes of all emission lines for these objects, which are later classified with emission line ratios into one Seyfert 2, six LINERs and four HII galaxies. We also identify one HII galaxy (A1216+04) as a hitherto unknown Wolf-Rayet galaxy from the presence of the Wolf-Rayet broad bump at 4650 Å. We propose that the star-forming activities in elliptical galaxies are triggered by either galaxy-galaxy interaction or the merging of a small satellite/a massive star cluster, as already suggested by recent numerical simulations.

astro-ph↗