Abstract
A static spherically symmetric black hole usually turns out to be either a Schwarzschild black hole or a Reissner-Nordström black hole. This result was summarised by Ruffini and Wheeler as the so-called no hair conjecture which states that for a spherically symmetric black hole only the information about mass (M) and electric charge (e) of the black hole is available for an external observer. In this work, we calculate the emission rate of charged particles from an asymptotically flat charged spherically symmetric black hole endowed with a scalar hair using a semi-classical tunneling formalism. We observe that the total entropy of the black hole contains an energy-dependent part due to the scalar charge. The upper bound on the charge-mass ratio of the emitted particles is also observed to decrease with the scalar charge as well.
Highlights
The question of information loss has been addressed using the tunneling formalism
Based on the non-negativity of mutual information between consecutive Hawking emissions, we find the dependence of the charge to mass ratio of the emitted particles on the scalar charge s in each step
We studied the problem of Hawking emission of massive charged particles from a spherically symmetric charged black hole endowed with a scalar hair using the semiclassical tunneling formalism
Summary
The question of information loss has been addressed using the tunneling formalism. We employ the tunneling method to study Hawking radiation of charged particles from an asymptotically flat static spherically symmetric charged black hole, endowed with a scalar hair, dubbed as the scalar-hairy RN black hole [31]. The primary objective of the present work is to study the effect of the scalar hair on the transmission rate of charged Hawking quanta. We observe that the change in entropy of the scalar-hairy RN black hole due to the emission of charged particles contains an additional energy-dependent contribution which vanishes during emission of uncharged particles and in the absence of the scalar hair. The tunneling rate for the emission of charged particles from the scalar-hairy RN black hole matches smoothly with that of the standard RN black hole, in the absence of the scalar hair. To eliminate these singularities at r±, we introduce the generalised Painlevé transformation,
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