Supercritically charged objects and electron-positron pair creation

Abstract

We investigate the stability and $e^{+}{e}^{-}$ pair creation of supercritically charged superheavy nuclei, $ud$QM nuggets, strangelets, and strangeon nuggets based on Thomas-Fermi approximation. The model parameters are fixed by reproducing their masses and charge properties reported in earlier publications. It is found that $ud$QM nuggets, strangelets, and strangeon nuggets may be more stable than ${}^{56}$Fe at $A\gtrsim 315$, $5\times 10^4$, and $1.2\times 10^8$, respectively. For those stable against neutron emission, the most massive superheavy element has a baryon number $\sim$965, while $ud$QM nuggets, strangelets, and strangeon nuggets need to have baryon numbers larger than $39$, 433, and $2.7\times 10^5$. The $e^{+}{e}^{-}$ pair creation will inevitably start for superheavy nuclei with charge numbers $Z\ge 177$, $ud$QM nuggets with $Z\ge 163$, strangelets with $Z\ge 192$, and strangeon nuggets with $Z\ge 212$. A universal relation $Q/R_e=\left(m_e-{\bar{\mu }}_e\right)/\alpha$ is obtained at a given electron chemical potential ${\bar{\mu }}_e$, where $Q$ is the total charge and $R_e$ the radius of electron cloud. This predicts the maximum charge number by taking ${\bar{\mu }}_e=-m_e$. For supercritically charged objects with ${\bar{\mu }}_e<-m_e$, the decay rate for $e^{+}{e}^{-}$ pair production is estimated based on the JWKB approximation. It is found that most positrons are emitted at $t\lesssim 10^{-15}$ s, while a long lasting positron emission is observed for large objects with $R\gtrsim 1000$ fm. The emission and annihilation of positrons from supercritically charged objects may be partially responsible for the short $\gamma$-ray burst during the merger of binary compact stars, the 511 keV continuum emission, as well as the narrow faint emission lines in X-ray spectra from galaxies and galaxy clusters.

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Cited by in corpus (11)

• Unified Interacting Quark Matter and its Astrophysical Implications
• Quantum nucleation of up-down quark matter and astrophysical implications
• GW190814: Circumstantial Evidence for Up-Down Quark Star
• Hybrid Strangeon Stars
• Interface effects of quark matter: Light-quark nuggets and compact stars
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• Radial and Non-Radial Oscillations of Inverted Hybrid Stars
• Universal relations for anisotropic interacting quark stars
• Hybrid stars may have an inverted structure
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• Compact dwarfs made of light-quark nuggets