Pulsar glitches, i.e. the sudden spin-ups of pulsars, have been detected for most known pulsars.The mechanism giving rise to this kind of phenomenon is uncertain, although a large data set has been built.In the framew...Pulsar glitches, i.e. the sudden spin-ups of pulsars, have been detected for most known pulsars.The mechanism giving rise to this kind of phenomenon is uncertain, although a large data set has been built.In the framework of the starquake model, based on Baym ＆ Pines, the glitch sizes（the relative increases of spin-frequencies during glitches） △Ω/Ω depend on the released energies during glitches, with less released energies corresponding to smaller glitch sizes. On the other hand, as one of the dark matter candidates,our Galaxy might be filled with so called strange nuggets（SNs） which are relics from the early Universe.In this case collisions between pulsars and SNs are inevitable, and these collisions would lead to glitches when enough elastic energy has been accumulated during the spin-down process. The SN-triggered glitches could release less energy, because the accumulated elastic energy would be less than that in the scenario of glitches without SNs. Therefore, if a pulsar is hit frequently by SNs, it would tend to have more small glitches, whose values of ？？/？ are smaller than those in the standard starquake model（with larger amounts of released energy）. Based on the assumption that in our Galaxy the distribution of SNs is similar to that of dark matter, as well as on the glitch data in the ATNF Pulsar Catalogue and Jodrell Bank glitch table, we find that in our Galaxy the incidences of small glitches exhibit tendencies consistent with the collision rates between pulsars and SNs. Further testing of this scenario is expected by detecting more small glitches（e.g.,by the Square Kilometre Array）.展开更多
Many-body correlations in nuclei determine the behavior of Deep-Inelastic-Scattering (DIS) and Quasi-Elastic Scattering (QES) cross section ratios off heavy over light nuclei especially for <em>x</em><s...Many-body correlations in nuclei determine the behavior of Deep-Inelastic-Scattering (DIS) and Quasi-Elastic Scattering (QES) cross section ratios off heavy over light nuclei especially for <em>x</em><sub>Bjorken</sub> > 1, obtained at Jefferson Lab. They can be described in terms of quark-cluster formation in nuclei due to wave-function overlapping, manifesting itself when the momentum transfer is high so that the partonic degrees of freedom are resolved. In clusters (correlated nucleons) the quark and gluon momentum distributions are softer than in single nucleons and extend to <em style="white-space:normal;">x</em><sub style="white-space:normal;">Bjorken</sub><span style="white-space:normal;"> > 1</span>. The cluster formation probabilities are computed using a network-defining algorithm in which the initial nucleon density is either standard Woods-Saxon or is input from lower energy data while the critical radius for nucleon merging is an adjustable parameter. The exact choice of critical radius depends on the specific nucleus and it is anti-correlated to the rescaling of the <em>x</em><sub>Bjorken</sub> needed for bound nucleons. The calculations show that there is a strong dependence of the cross section ratios on the <em>x</em><sub>Bjorken</sub> in agreement with the data and that four-body correlations are needed to explain the experimental results even in the range 1 <<em> x</em><sub>Bjorken</sub> < 2. The dependence on the specific exponents of parton distributions in high-order clusters is weak.展开更多
The N-N <sup>1</sup>S<sub>0</sub> scattering length differences Δα<sub>CSB</sub> and Δα<sub>CIH</sub> of the charge symmetrybreaking and charge independence breaking...The N-N <sup>1</sup>S<sub>0</sub> scattering length differences Δα<sub>CSB</sub> and Δα<sub>CIH</sub> of the charge symmetrybreaking and charge independence breaking are calculated by a resonating group method with aquark cluster model.By adding the QED-QCD interference effect to the quark mass differenceand the electromagnetic interaction,the Δα<sub>CSH</sub> and Δα<sub>CIH</sub> can be reproduced with modelparameters constrained by the hadron isomultiplet masses.展开更多
Under the assumption that the quarks in the double hadron system have the distribu-tion of double Gaussian type, the quark wave function parameters are determined within theframework of a former cluster model in Glaub...Under the assumption that the quarks in the double hadron system have the distribu-tion of double Gaussian type, the quark wave function parameters are determined within theframework of a former cluster model in Glauber multiple scattering theory and by fitting thecalculated cross section to experimental data.展开更多
The resonance interaction of weak gravitation radiation (WGR) from agarose hydrogel with the gravitation radiation (GR) caused by celestial bodies (Sun, Jupiter, Uranus, Mercury and Moon) has been investigated by the ...The resonance interaction of weak gravitation radiation (WGR) from agarose hydrogel with the gravitation radiation (GR) caused by celestial bodies (Sun, Jupiter, Uranus, Mercury and Moon) has been investigated by the Zubow gravitation mass spectroscopy (ZGMS). The absorption of WGR by the Sun was found to change at the moment when the Sun appears in the slide plane of gravitation proton resonance (SPGPR, plane going through the Earth rotating axis and the sample place on the Earth surface). There were analyzed the signals of the gravitation Sun (GS), Mercury and Moon. GS contains signals of the corona, nucleus and sub-nucleus. Here the nature of the last one is near to the matter of “naked” protons in hydrogen bonds (HB) of the sensor with which it interacts. The proton model as analogous to the black hole has been proved ex-perimentally. The sub-nucleus was concluded to be of quarks’ nature but the nucleus of neutrons’ one. The GR velocity in the sun system has been determined experimentally additionally, the influence of gas giants (GG) on it. At the moment of Sun and GG opposition the GR velocity was 2 - 8 times higher than that one of the light. GG reduced the GR velocity in the direction of the Sun. The role of the Earth as a gravitation mir-ror has been supported. Six gravitation resonator signals from Moon gravitation shots (gravitation laser) were analyzed. The GR of planets was observed to influence the energy of water cluster ensembles.展开更多
An effective potential in a meson-meson system is discussed based on the SU（3） chiral constituent quark model, and the analytic form of the potential is explicitly given. In addition, the effective potential is empl...An effective potential in a meson-meson system is discussed based on the SU（3） chiral constituent quark model, and the analytic form of the potential is explicitly given. In addition, the effective potential is employed to study the bound state problem of ωφ, which is related to the new resonance of f0（1810） observed in BES Ⅱ very recently.展开更多
A QCD multiquark cluster system is studied in the relativistic harmonic oscillator potential model （RHOPM）, and the electromagnetic form factors of the pion, proton and deuteron in the RHOPM are predicted. The calcu...A QCD multiquark cluster system is studied in the relativistic harmonic oscillator potential model （RHOPM）, and the electromagnetic form factors of the pion, proton and deuteron in the RHOPM are predicted. The calculated theoretical results are then compared with existing experimental data, finding very good agreement between the theoretical predictions and experimental data for these three target particles. We claim that this model can be applied to study QCD hadronic properties, particularly neutron properties, and to find six-quark cluster and/or nine-quark cluster probabilities in light nuclei such as helium 3He and tritium 3H. This is a problem of particular importance and interest in quark nuclear physics.展开更多
基金supported by the National Natural Science Foundation of China (11203018)the West Light Foundation (XBBS-2014-23)+1 种基金the Science Project of Universities in Xinjiang (XJEDU2012S02)the Doctoral Science Foundation of Xinjiang University (BS120107)
文摘Pulsar glitches, i.e. the sudden spin-ups of pulsars, have been detected for most known pulsars.The mechanism giving rise to this kind of phenomenon is uncertain, although a large data set has been built.In the framework of the starquake model, based on Baym ＆ Pines, the glitch sizes（the relative increases of spin-frequencies during glitches） △Ω/Ω depend on the released energies during glitches, with less released energies corresponding to smaller glitch sizes. On the other hand, as one of the dark matter candidates,our Galaxy might be filled with so called strange nuggets（SNs） which are relics from the early Universe.In this case collisions between pulsars and SNs are inevitable, and these collisions would lead to glitches when enough elastic energy has been accumulated during the spin-down process. The SN-triggered glitches could release less energy, because the accumulated elastic energy would be less than that in the scenario of glitches without SNs. Therefore, if a pulsar is hit frequently by SNs, it would tend to have more small glitches, whose values of ？？/？ are smaller than those in the standard starquake model（with larger amounts of released energy）. Based on the assumption that in our Galaxy the distribution of SNs is similar to that of dark matter, as well as on the glitch data in the ATNF Pulsar Catalogue and Jodrell Bank glitch table, we find that in our Galaxy the incidences of small glitches exhibit tendencies consistent with the collision rates between pulsars and SNs. Further testing of this scenario is expected by detecting more small glitches（e.g.,by the Square Kilometre Array）.
文摘Many-body correlations in nuclei determine the behavior of Deep-Inelastic-Scattering (DIS) and Quasi-Elastic Scattering (QES) cross section ratios off heavy over light nuclei especially for <em>x</em><sub>Bjorken</sub> > 1, obtained at Jefferson Lab. They can be described in terms of quark-cluster formation in nuclei due to wave-function overlapping, manifesting itself when the momentum transfer is high so that the partonic degrees of freedom are resolved. In clusters (correlated nucleons) the quark and gluon momentum distributions are softer than in single nucleons and extend to <em style="white-space:normal;">x</em><sub style="white-space:normal;">Bjorken</sub><span style="white-space:normal;"> > 1</span>. The cluster formation probabilities are computed using a network-defining algorithm in which the initial nucleon density is either standard Woods-Saxon or is input from lower energy data while the critical radius for nucleon merging is an adjustable parameter. The exact choice of critical radius depends on the specific nucleus and it is anti-correlated to the rescaling of the <em>x</em><sub>Bjorken</sub> needed for bound nucleons. The calculations show that there is a strong dependence of the cross section ratios on the <em>x</em><sub>Bjorken</sub> in agreement with the data and that four-body correlations are needed to explain the experimental results even in the range 1 <<em> x</em><sub>Bjorken</sub> < 2. The dependence on the specific exponents of parton distributions in high-order clusters is weak.
基金The project supported by the NSF(19675018)SEDC of ChinaSSTC of China
文摘The N-N <sup>1</sup>S<sub>0</sub> scattering length differences Δα<sub>CSB</sub> and Δα<sub>CIH</sub> of the charge symmetrybreaking and charge independence breaking are calculated by a resonating group method with aquark cluster model.By adding the QED-QCD interference effect to the quark mass differenceand the electromagnetic interaction,the Δα<sub>CSH</sub> and Δα<sub>CIH</sub> can be reproduced with modelparameters constrained by the hadron isomultiplet masses.
文摘Under the assumption that the quarks in the double hadron system have the distribu-tion of double Gaussian type, the quark wave function parameters are determined within theframework of a former cluster model in Glauber multiple scattering theory and by fitting thecalculated cross section to experimental data.
文摘The resonance interaction of weak gravitation radiation (WGR) from agarose hydrogel with the gravitation radiation (GR) caused by celestial bodies (Sun, Jupiter, Uranus, Mercury and Moon) has been investigated by the Zubow gravitation mass spectroscopy (ZGMS). The absorption of WGR by the Sun was found to change at the moment when the Sun appears in the slide plane of gravitation proton resonance (SPGPR, plane going through the Earth rotating axis and the sample place on the Earth surface). There were analyzed the signals of the gravitation Sun (GS), Mercury and Moon. GS contains signals of the corona, nucleus and sub-nucleus. Here the nature of the last one is near to the matter of “naked” protons in hydrogen bonds (HB) of the sensor with which it interacts. The proton model as analogous to the black hole has been proved ex-perimentally. The sub-nucleus was concluded to be of quarks’ nature but the nucleus of neutrons’ one. The GR velocity in the sun system has been determined experimentally additionally, the influence of gas giants (GG) on it. At the moment of Sun and GG opposition the GR velocity was 2 - 8 times higher than that one of the light. GG reduced the GR velocity in the direction of the Sun. The role of the Earth as a gravitation mir-ror has been supported. Six gravitation resonator signals from Moon gravitation shots (gravitation laser) were analyzed. The GR of planets was observed to influence the energy of water cluster ensembles.
基金Supported by National Natrual Science Foundation (10775146, 10775148, 10975146, 11035006)Ministry of Science and Technology of China (2009CB825200)
文摘An effective potential in a meson-meson system is discussed based on the SU（3） chiral constituent quark model, and the analytic form of the potential is explicitly given. In addition, the effective potential is employed to study the bound state problem of ωφ, which is related to the new resonance of f0（1810） observed in BES Ⅱ very recently.
基金Supported by National Natural Science Foundation of China(11365002)Guangxi Natural Science Foundation for Young Researchers(2013GXNSFBB053007,2011GXNSFA018140)+2 种基金Guangxi Education Department(2013ZD049)Guangxi Grant for Excellent Researchers(2011-54)Guangxi University of Science and Technology Foundation for PhDs(11Z16)
文摘A QCD multiquark cluster system is studied in the relativistic harmonic oscillator potential model （RHOPM）, and the electromagnetic form factors of the pion, proton and deuteron in the RHOPM are predicted. The calculated theoretical results are then compared with existing experimental data, finding very good agreement between the theoretical predictions and experimental data for these three target particles. We claim that this model can be applied to study QCD hadronic properties, particularly neutron properties, and to find six-quark cluster and/or nine-quark cluster probabilities in light nuclei such as helium 3He and tritium 3H. This is a problem of particular importance and interest in quark nuclear physics.
