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}}, efficiency epsilon and the disk potential V_{mathrm{eff}} are independent of lambda (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 (say) and for the extreme spin a_{star }=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 } 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} permitted by the strong lensing bound. The broad conclusion is that RDSWH are experimentally indistinguishable from KBH by accretion characteristics.
Highlights
1 λ2 is longer than the observational time scale, the signals emitted by a source falling into a wormhole will contain the usual quasi-normal mode (QNM) ringing signature of a black hole, in spite of the absence of a true horizon [1]
We present below three tables showing observable characteristics of the thin disk (Table 1), the minimum stable radius and the accretion efficiency (Table 2) and the difference of the maxima of flux of radiation between rotating generalization of the Damour– Solodukhin wormhole (RDSWH) and Kerr BH (Table 3)
Gravitational wave echoes of RDSWH have been recently studied by Bueno et al [3]
Summary
1 λ2 is longer than the observational time scale, the signals emitted by a source falling into a wormhole will contain the usual QNM ringing signature of a black hole, in spite of the absence of a true horizon [1]. Strong field lensing is an excellent diagnostic for studying the signatures of WHs versus BHs, see, e.g., [16] There is another important diagnostic, namely, the accretion phenomenon around compact objects that has already been a very active field of research (see, e.g., [17,18,19,20,21,22,23,24,25,26,27]). We shall study the kinematic as well as emissivity properties such as the luminosity spectra, flux of radiation, temperature profile, efficiency of a thin accretion disk around a stellar sized RDSWH using the Page–Thorne model [28,29,30,31].
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
