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P-stars in the gravitational wave era

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Abstract

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.

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Notes

  1. Note that through the paper we are adopting cgs units; however, in this Section we use the natural units of high-energy physics were the Planck constant and the speed of light are set to one, \(\hslash = c = 1\). In these units the color coupling constant g is dimensionless and \(\sqrt{gH}\) has dimension of energy. To switch to cgs units it suffices to replace gH with \(\hslash c gH\). It is also useful to point out that 1.0 GeV\(^2 \, \simeq \,\) 5.13 \(\times \) 10\(^{19}\) G.

  2. Note that, since we set \(c=1\), the energy density coincides with the mass density \(\rho \).

  3. We shall follow the conventions adopted in Ref. [39].

  4. Equations (2.22) and (2.23) in cgs units can be found in Ref. [23].

  5. The range of values displayed in Eq. (2.27) is our estimate of the lattice numerical results presented in Refs. [31,32,33] extrapolated to the physical point where the mass of the pion is about 140 MeV.

  6. Note that 1 GeV\(^4 = 2.086 \times 10^{35}\) dyn/cm\(^2\) and 1 GeV\(^4\)/c\(^2\) = 2.32 \(\times 10^{14}\) gr/cm\(^3\).

  7. For a detailed review that includes an illustration of X-ray modelling techniques and associated uncertainties, see Ref. [89].

  8. This corresponds to \(c_s^\mathrm{eff} \simeq 0.2 \, c\).

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    Paolo Cea

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Cea, P. P-stars in the gravitational wave era. Eur. Phys. J. Plus 135, 891 (2020). https://doi.org/10.1140/epjp/s13360-020-00911-w

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