What Will Be The Tidal Deformability Of Strange Planets And Strange Dwarfs? (Planetary Science)

Xu Wang and colleagues in their recent paper calculated the tidal deformability of strange quark planets and strange quark dwarfs.

According to strange quark matter hypothesis, strange quark matter, which is composed of u, d, and s quarks, could be the true ground state of baryon matter, so the observed compact stars like pulsars, neutron stars etc. may actually be strange quark stars. It has also been argued that the gravitational-wave signal from the merger of a strange planet with a strange star in the Milky Way could be detected by the LIGO detector or by the next-generation Einstein Telescope if the merger happens in local galaxies up to several Mpc. So, strange planets and strange dwarfs are hopeful candidates that could be used to test the strange quark matter hypothesis, but their tidal deformability has not been thoroughly investigated. Thus, Xu and colleagues now calculated the tidal deformability¹ of strange quark planets and strange dwarfs.

They found that the tidal deformability of strange quark objects is smaller than that of normal matter counterparts. For a typical 0.6 M compact star, the tidal deformability of a strange dwarf is about 1.4 times less than that of a normal white dwarf. The difference is even more significant between strange quark planets and normal matter planets.

Additionally, if the strange quark planet is a bare one (i.e., not covered by a normal matter curst), the tidal deformability will be extremely small, which means bare strange quark planets will hardly be distorted by tidal forces.

Finally, their study clearly proves the effectiveness of identifying strange quark objects via searching for strange quark planets through gravitational-wave observations.

Figure 1. The combined tidal deformability (a) and combined dimensionless tidal deformability (b) as a function of the mass radio q for strange quark objects with crust. In Panels (c) and (d), the combined tidal deformability and combined dimensionless tidal deformability are plot versus the chirp mass M. For comparison, the dashed curve illustrates the case of pulsar-white dwarf/normal planet systems. In all the plot, the primary compact star is assumed to have a mass of 1.4 M © Wang et al.

Note: 1) The tidal deformability describes how much a body is deformed by tidal forces, which arise when two massive bodies orbit each other.

Reference: Xu Wang, Abudushataer Kuerban, Jin-Jun Geng, Fan Xu, Xiao-Li Zhang, Bing-Jun Zuo, Wen-Li Yuan, Yong-Feng Huang, “Tidal Deformability of Strange Quark Planets and Strange Dwarfs”, Arxiv, pp. 1-10, 2021. https://arxiv.org/abs/2105.13899

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