论文标题
重力波时代的P-Star
P-stars in the gravitational wave era
论文作者
论文摘要
P-Star是由我们很久以前我们提出的染色体冷凝物中的夸克夸克制成的紧凑相对论恒星。 P-Star不承认临界质量，因此他们能够克服重力崩溃到黑洞。在这项工作中，我们对P-Star的理论建议进行了更大的详细信息。我们指出，我们对紧凑型相对论恒星的理论源于我们对晶格上量子染色体动力学的非扰动数值模拟支持的限制量子真空的理解。我们将我们的建议与最近观察到的大规模脉冲星，重力事件GW170817以及PSR J0030+0451质量和半径的确切确定的限制进行了比较。我们认为，核心的超新星可能会导致P-Star而不是中子恒星。在这种情况下，我们表明，P-Star的诞生可以解决超新星爆炸问题，从而导致成功的超新星爆炸，总能量达到$ 10^{53} $ ERG。我们将P-Star与重力波事件GW170817和随后的电磁随访，短伽玛射线爆发GRB170817A和Kilonova AT2017GFO进行了严格的比较。我们还提出了一项探索性研究，该研究对与质量合并的二进制P标准符$ m_1 \ simeq m_2 \ simeq 30 \;; m _ {\ odot} $。我们尝试与重力波事件GW150914进行定性比较。我们发现，大量P-Star二进制的重力波应变幅度可以通过合并的黑洞二进制物来模仿RIGHDOWN重力波发射。我们指出，大规模P-Star的明确签名将是在两个与不等质量的大规模紧凑型物体的合并后相重力波应变振幅中检测到的摇摆频率。
P-stars are compact relativistic stars made of deconfined up and down quarks in a chromomagnetic condensate proposed by us long time ago. P-stars do not admit a critical mass thereby they are able to overcome the gravitational collapse to black holes. In this work we discuss in greater details our theoretical proposal for P-stars. We point out that our theory for compact relativistic stars stems from our own understanding of the confining quantum vacuum supported by estensive non-perturbative numerical simulations of Quantum ChromoDynamics on the lattice. We compare our proposal with the constraints arising from the recent observations of massive pulsars, the gravitational event GW170817 and the precise determination of the PSR J0030+0451 mass and radius from NICER data. We argue that core-collapsed supernovae could give rise to a P-star instead of a neutron star. In this case we show that the birth of a P-star could solve the supernova explosion problem leading to successful supernova explosions with total energies up to $10^{53}$ erg. We critically compare P-stars with the gravitational wave event GW170817 and the subsequent electromagnetic follow-up, the short Gamma Ray Burst GRB170817A and the kilonova AT2017gfo. We also present an explorative study on gravitational wave emission from coalescing binary P-stars with masses $M_1 \simeq M_2 \simeq 30 \; M_{\odot}$. We attempt a qualitative comparison with the gravitational wave event GW150914. We find that the gravitational wave strain amplitude from massive P-star binaries could mimic the ringdown gravitational wave emission by coalescing black hole binaries. We point out that a clear signature for massive P-stars would be the detection of wobble frequencies in the gravitational wave strain amplitude in the post-merger phase of two coalescing massive compact objects with unequal masses.
