The Tower of the Chandrasekhar Limits and Spin Periods of Pulsars
The Tower of the Chandrasekhar Limits and Spin Periods of Pulsars
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钱德拉塞卡塔脉冲星的极限和自旋周期
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发表时间：
2015
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通讯作者：
Sylwester Kornowski
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作者：
Sylwester Kornowski
在主流宇宙学中，人们假设白色矮星在费米气体的条件下爆炸。在这里，在尺度对称理论（SST），我们表明，出现塔的阿布拉塞卡极限和恒星/白矮星的阈值质量爆炸通过中子星状态。中子星的行为类似于液晶。有所需的平面结构和细长的矩形棱镜。出现了中子星星，即中子黑洞的质量上限，等于24.81太阳质量。但是由于从星星核心向其表面的完美能量流，也出现了至少三个卡拉塞卡极限，即通过整个星星突然坍缩到中子-星星状态而爆炸为Ia型超新星的恒星质量，这导致了剧烈的全体积爆炸，因此不会产生中子-星星残余物-阈值质量为1.395，11.20和0.891太阳质量。第一个质量是众所周知的克拉塞卡极限，而第二个质量是SN 1987 A超新星的质量。能量由爱因斯坦时空成分的凝聚体携带，这些凝聚体是关于弱相互作用的黑洞，或者由高能中微子携带。质量为52.828 MeV的凝聚体产生于μ子中心，质量为424.124 MeV的凝聚体产生于重子中心，而中微子的特征能量是中性π介子质量的四分之一（33.743 MeV）。它们的数密度随着恒星的临界质量而迅速增加。这里也计算了中子星（即具有中子核和铁壳的恒星）自旋周期的下限（0.000768 s）和上限（4，228 s）。这里提出的模型非常简单，并导致观察事实。
It is assumed in the mainstream cosmology that at the Chandrasekhar limit the white dwarfs explode due to the conditions in a Fermi gas. Here, within the Scale-Symmetric Theory (SST), we showed that there appears the tower of the Chandrasekhar limits and that the stars/white-dwarfs with the threshold masses explode via a neutron-star state. Neutron stars behave as liquid crystal. There are the needed flat structures and the elongated rectangular prisms. There appears the upper limit for mass of neutron star, i.e. of the neutron black hole, equal to 24.81 solar masses. But due to perfect energy flow from core of a star toward its surface there as well appear at least three Chandrasekhar limits i.e. masses of stars which explode as Type Ia supernovae via sudden collapse of whole star to the neutron-star state which leads to violent full volumetric explosion so there is not created a neutron-star remnant – the threshold masses are 1.395, 11.20 and 0.891 solar masses. The first mass is the very well known Chandrasekhar limit whereas the second was the mass of, for example, the SN 1987A supernova. Energy is carried by the condensates of the Einstein-spacetime components that are the black holes in respect of the weak interactions or is carried by energetic neutrinos. The condensates with a mass of 52.828 MeV are produced in centres of muons, with a mass of 424.124 MeV are produced in centres of baryons, whereas the characteristic energy of neutrinos is the one fourth of the mass of neutral pion (33.743 MeV). Their number densities increase rapidly for the threshold masses of stars. Here, as well, are calculated the lower (0.000768 s) and upper (4,228 s) limits for spin periods of pulsars i.e. for stars with neutron core and iron crust. Presented here model is very simple and leads to observational facts.