Accretion disk around the rotating Damour–Solodukhin wormhole

Abstract

Abstract A new rotating generalization of the Damour–Solodukhin wormhole (RDSWH), called Kerr-like wormhole, has recently been proposed and investigated by Bueno et al. for echoes in the gravitational wave signal. We show a novel feature of the RDSWH, viz., that the kinematic properties such as the ISCO or marginally stable radius $$r_{\mathrm{ms}}$$ rms , efficiency $$\epsilon $$ ϵ and the disk potential $$V_{\mathrm{eff}}$$ Veff are independent of $$\lambda $$ λ (which means they are identical to their KBH counterparts for any given spin). Differences however appear in the emissivity properties for higher values $$0.1<\lambda \le 1$$ 0.1<λ≤1 (say) and for the extreme spin $$a_{\star }=0.998$$ a⋆=0.998 . The kinematic and emissivity are generic properties as variations of the wormhole mass and the rate of accretion within the model preserve these properties. Specifically, the behavior of the luminosity peak is quite opposite to each other for the two objects, which could be useful from the viewpoint of observations. Apart from this, an estimate of the difference $$\varDelta _{\lambda }$$ Δλ in the maxima of flux of radiation F(r) shows non-zero values but is too tiny to be observable at present for $$\lambda < 10^{-3}$$ λ<10-3 permitted by the strong lensing bound. The broad conclusion is that RDSWH are experimentally indistinguishable from KBH by accretion characteristics.