Abstract
Taking the GW190814 event as a clue, r-mode of 2.5\(M_{\odot }\) supermassive neutron star along with 1.4\(M_{\odot }\) canonical neutron star is investigated by using RNS code in the framework of rotating neutron star. Our conclusion further confirms that for the secondary star of GW190814, there exists a possibility that it is a rapid rotating supermassive neutron star in r-mode stable state. For super fast rotating neutron star with fixed spin frequency, the lower limit of its mass \(M_{min}\) can be constrained by the critical spin frequency under r-mode. As the \(M_{min}\) is EOS (equation of state) dependent, if the mass of neutron star with very high spin frequency can be observed in the future, the EOS of super-dense nuclear matter can be constrained by comparing the \(M_{min}\) of different EOSs. At last, the effect of crust-core transition densities on r-modes of neutron stars is explored and discussed.
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This manuscript has no associated data or the data will not be deposited. [Authors’comment: The processed data required to reproduce these findings cannot be shared at this time as the data also forms part of an ongoing study.]
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This work is supported by NSFC (Grant No. 11975101) and Guangdong Natural Science Foundation (Grants No. 2020A151501820 and No. 2022A1515011552).
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Communicated by Jérôme Margueron.
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Wang, J., Yang, S. & Wen, D. Constraining properties of massive neutron star through R-mode. Eur. Phys. J. A 58, 132 (2022). https://doi.org/10.1140/epja/s10050-022-00781-z
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DOI: https://doi.org/10.1140/epja/s10050-022-00781-z