Version 1
: Received: 3 November 2020 / Approved: 4 November 2020 / Online: 4 November 2020 (14:40:23 CET)
How to cite:
Rojas Castillo, W.A.; Arenas Salazar, J.R. Conceptual Model for Cutoff Origin in Exotic Compact Objects. Preprints2020, 2020110197. https://doi.org/10.20944/preprints202011.0197.v1
Rojas Castillo, W.A.; Arenas Salazar, J.R. Conceptual Model for Cutoff Origin in Exotic Compact Objects. Preprints 2020, 2020110197. https://doi.org/10.20944/preprints202011.0197.v1
Rojas Castillo, W.A.; Arenas Salazar, J.R. Conceptual Model for Cutoff Origin in Exotic Compact Objects. Preprints2020, 2020110197. https://doi.org/10.20944/preprints202011.0197.v1
APA Style
Rojas Castillo, W.A., & Arenas Salazar, J.R. (2020). Conceptual Model for Cutoff Origin in Exotic Compact Objects. Preprints. https://doi.org/10.20944/preprints202011.0197.v1
Chicago/Turabian Style
Rojas Castillo, W.A. and Jose Robel Arenas Salazar. 2020 "Conceptual Model for Cutoff Origin in Exotic Compact Objects" Preprints. https://doi.org/10.20944/preprints202011.0197.v1
Abstract
We propose a conceptual model for the closeness parameter $\epsilon$, which characterizes exotic compact objects (ECOs). To estimate $\epsilon$, a thin spherical dust shell is considered, which gravitationally contracts from a specific position $r(t_{0})$ to near its gravitational radius $r(t_{2})=r_{s} + \epsilon$, in a finite time $t_{2}$, measured in the frame of a fiducial observer (FIDO). For an external observer, the shell’s kinematics is characterized by two clearly distinguishable phases: one of rapid contraction, where the shell is far away from the gravitational radius, $r(t_{0})\gg r_{s}$, and a second phase quasi-stationary, $r(t)\sim r_{s}$, where all of the shell’s mass is concentrated around the associated horizon, such that for a FIDO, a black hole (BH)is undistinguishable from a shell configured as a black shell (BS). \\ In the semi-classical approximation $E\ll \kappa_{0}l_{p}^{2}$ and tends to zero when the observation time of collapse $t_{2}$, measured by FIDO, tends to infinity; $\kappa_{0}$ and $l_{p}$ are surface gravity and Planck length, respectively. The quantum effects are significant when $\epsilon\ll r(t_{2})$ and $\epsilon$ tends to $\kappa_{0}l_{p}^{2}$. \\ Without knowing details on quantum gravity, parameter $\epsilon$ is calculated, which, in general, allows distinguishing the ECOs from BHs. Specifically, a BS (ECO) is undistinguishable from a BH.
Keywords
black shell; closeness parameter; cutoff; entanglement; exotic objects; compact objects
Subject
Physical Sciences, Acoustics
Copyright:
This is an open access article distributed under the Creative Commons Attribution License which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.