2019/01/31 by R. Kh. Karimov, R. N. Izmailov, K. K. Nandi · 30 citations
Engineering · Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Physics #Pulsars and Gravitational Waves Research #Superconducting Materials and Applications #Theoretical physics #Wormhole #gr-qc
paper · pdf · doi:10.1140/epjc/s10052-019-7488-7
published in The European Physical Journal C 79(11) (Springer Science+Business Media) · 9 pages, 3 tables, 13 figures
openalex publication_date 2019/11/01 · arxiv created 2020/02/04 · arxiv updated 2020/02/05 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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 rms <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>r</mml:mi><mml:mi>ms</mml:mi></mml:msub></mml:math> , efficiency ε <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mi>ϵ</mml:mi></mml:math> and the disk potential Veff <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>V</mml:mi><mml:mi>eff</mml:mi></mml:msub></mml:math> are independent of λ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mi>λ</mml:mi></mml:math> (which means they are identical to their KBH counterparts for any given spin). Differences however appear in the emissivity properties for higher values 0.1lt;λ ≤ 1 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mn>0.1</mml:mn><mml:mo><</mml:mo><mml:mi>λ</mml:mi><mml:mo>≤</mml:mo><mml:mn>1</mml:mn></mml:mrow></mml:math> (say) and for the extreme spin a⋆ =0.998 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:msub><mml:mi>a</mml:mi><mml:mo>⋆</mml:mo></mml:msub><mml:mo>=</mml:mo><mml:mn>0.998</mml:mn></mml:mrow></mml:math> . 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 λ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:msub><mml:mi>Δ</mml:mi><mml:mi>λ</mml:mi></mml:msub></mml:math> in the maxima of flux of radiation F ( r ) shows non-zero values but is too tiny to be observable at present for λ lt; 10-3 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>λ</mml:mi><mml:mo><</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mrow><mml:mo>-</mml:mo><mml:mn>3</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math> permitted by the strong lensing bound. The broad conclusion is that RDSWH are experimentally indistinguishable from KBH by accretion characteristics.