A bag model of matter condensed by the strong interaction

Miao, Zhi-Qiang; Xia, Cheng-Jun; Lai, Xiao-Yu; Maruyama, Toshiki; Xu, Ren-Xin; Zhou, En-Ping

doi:10.48550/arxiv.2008.06932

Cited by 4 publications

(4 citation statements)

References 78 publications

(102 reference statements)

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“…For the strangeon matter proposed in Lai & Xu (2009b), in a large parameter space the equation of state of strangeon star is compatible with the constraint by GW170817 even if the maximum mass of pulsars is higher than 2.8 M⊙ (Lai et al 2019). For the linked bag model of strangeon matter (Miao et al 2020) which can be adopted for strong condensed matter in both 2-flavoured (nucleons) and 3-flavoured (hyperons and strangeons) scenarios, it is also found that in a large parameter space the maximum mass and tidal deformability of strangeon stars are consistent with the current astrophysical constraints.…”

Section: Introductionsupporting

confidence: 56%

Merging strangeon stars II: the ejecta and light curves

Lai,

Xia,

et al. 2020

Preprint

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The state of supranuclear matter in compact star remains puzzling, and it is argued that pulsars could be strangeon stars. The consequences of merging double strangeon stars are worth exploring, especially in the new era of multimessenger astronomy. This paper gives the first qualitative description about the evolution of ejecta and find that the ejecta could end up with two components. In the hot environment of the merger, the strangeon nuggets ejected by tidal disruption and hydrodynamical squeezing would suffer from evaporation, in which process particles, such as strangeons, neutrons and protons, are emitted. Taking into account both the evaporation of strangeon nuggets and the decay of strangeons, most of the ejected strangeon nuggets would turn into neutrons and protons within 10 ms, and the dependence of evaporation rate on temperature leads to the two-component ejecta. Light curves are derived for both high and low opacity components, where the former would be ejected from the directions around the equatorial plane, and the latter would be ejected in a broad range of angular directions. Although the total ejected mass would be ∼ 10 −3 M ⊙ only, the spin-down power of the long-lived remnant would account for the whole emission of kilonova AT2017gfo associated with GW 170817. The detailed picture of merging double strangeon stars is expected to be tested by future numerical simulations.

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Section: Introductionsupporting

confidence: 56%

Merging strangeon stars II: the ejecta and light curves

Lai,

Xia,

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…For the linked bag model of strangeon matter (Miao et al 2020) which can be adopted for strong condensed matter 250-3 in both 2-flavored (nucleons) and 3-flavored (hyperons and strangeons) scenarios, it is also found that in a large parameter space the maximum mass and tidal deformability of strangeon stars are consistent with the current astrophysical constraints.…”

Section: Introductionsupporting

confidence: 58%

Merging strangeon stars II: the ejecta and light curves

Lai¹,

Xia²,

Yu³

et al. 2021

Res. Astron. Astrophys.

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The state of supranuclear matter in compact stars remains puzzling, and it is argued that pulsars could be strangeon stars. The consequences of merging double strangeon stars are worth exploring, especially in the new era of multi-messenger astronomy. To develop the “strangeon kilonova” scenario proposed in Paper I, we make a qualitative description about the evolution of ejecta and light curves for merging double strangeon stars. In the hot environment of the merger, the strangeon nuggets ejected by tidal disruption and hydrodynamical squeezing would suffer from evaporation, in which process particles, such as strangeons, neutrons and protons, are emitted. Taking into account both the evaporation of strangeon nuggets and the decay of strangeons, most of the strangeon nuggets would turn into neutrons and protons, within dozens of milliseconds after being ejected. The evaporation rates of different particles depend on temperature, and we find that the ejecta could end up with two components, with high and low opacity respectively. The high opacity component would be in the directions around the equatorial plane, and the low opacity component would be in a broad range of angular directions. The bolometric light curves show that the spin-down power of the long-lived remnant would account for the whole emission of kilonova AT2017gfo associated with GW170817, if the total ejected mass ∼ 10−3 M ⊙. The detailed picture of merging double strangeon stars is expected to be tested by future numerical simulations.

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“…To examine strangeon matter with a more detailed microscopic dynamics, recently we have developed a linked bag model (Miao et al, 2020), where the strong interaction is treated effectively via quark propagation between separated bags. With the model parameters carefully adjusted to reproduce the saturation properties of nuclear matter, the possible existence of strangeon matter and strangeon star were analyzed.…”

Section: The Way To Strange Starmentioning

confidence: 99%

A roadmap to strange star

Xu,

Lai,

Xia

2020

Preprint

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What if normal baryonic matter is compressed so tightly that atomic nuclei come into close contact? This question has been asked since 1930s. The fist answer was presented by Lev Landau whose speculation has been developed, and the concept of neutron star is then popularized. However, another answer is related to strange star, which becomes worthy of attention especially after the establishment of the standard model of particle physics in 1960s. The basic ideas of this study are introduced pedagogically. We must point out emphatically that flavour symmetry of and strong coupling between quarks would be essential in seeking true answer to the question.The final answer is expected to appear in the era of multimessenger astronomy. It is emphasized too that, besides the differences of global properties (e.g., mass-radius relation, maximum mass, tidal deformability), the strong-bound surface of strange star (rather than the gravity-bound one for conventional neutron star) could play an important role in identifying a strange star by astronomical observations.

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A bag model of matter condensed by the strong interaction

Cited by 4 publications

References 78 publications

Merging strangeon stars II: the ejecta and light curves

Merging strangeon stars II: the ejecta and light curves

Merging strangeon stars II: the ejecta and light curves

A roadmap to strange star

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