[Paper Review] To the search for observational evidence of wormholes

A. Pozanenko, A. A. Shatskiy|arXiv (Cornell University)|Jul 21, 2010

Earthquake Detection and Analysis2 references3 citations

TL;DR

This paper investigates whether gamma-ray bursts (GRBs) transmitted through hypothetical wormholes (WHs) could produce observable repeating, hard-spectrum bursts resembling Soft Gamma-Ray Repeaters (SGRs). Using theoretical modeling of photon flux distribution and power spectra, it finds no evidence that known SGRs are WH candidates, but identifies harder, longer-duration repeating GRBs or identical light curves from different directions as potential WH signatures.

ABSTRACT

We consider observational properties of gamma-ray bursts (GRB) transmitted by hypothetical wormholes (WH). Such burst would be observable as repeating source, analogous to Soft Gamma-Repeaters (SGR). We show that the known sources of SGR cannot be WH candidates. We also discuss observational properties of GRB which might be a signature of WH.

Motivation & Objective

• To explore whether gamma-ray bursts (GRBs) transmitted through wormholes (WHs) could produce observable astrophysical signatures.
• To model the differential power spectrum (DPS) of GRBs passing through WHs using continuous and discrete photon flux approaches.
• To compare theoretical predictions with observed properties of known SGRs and GRBs to assess WH candidacy.
• To identify potential observational markers of WH-transmitted GRBs, such as repeating bursts or identical light curves from different directions.
• To evaluate the feasibility of detecting WHs via GRB observations at cosmological distances or nearby (1–5 pc).

Proposed method

• Derives the differential power spectrum (DPS) using a continuous flux model, assuming uniform source distribution and spherically symmetric WH geometry.
• Applies the flux equation $ s = I \cdot \frac{S_0}{4\pi r^2} \cdot f(\theta) \cdot \kappa \cdot \frac{S_1}{4\pi R^2} $, where $ f(\theta) $ is the deflection function and $ \kappa $ accounts for photon losses through the WH throat.
• Uses the integral power spectrum $ \log N(>s) - \log s $ to analyze source counts with flux exceeding $ s $, linking it to the DPS via $ N(s) = \int N'(s) ds $.
• Considers the cumulative number of detected events $ N(>s) $ as a function of source distance and flux threshold, integrating over solid angle and radial volume.
• Applies the model to GRB data, particularly BATSE observations, to compare predicted spectra with observed GRB and SGR properties.
• Evaluates the likelihood of recurrent GRBs with identical light curves or overlapping error boxes as WH candidates, using statistical probability estimates.

Experimental results

Research questions

• RQ1 Can GRBs transmitted through wormholes produce observable repeating bursts with properties resembling SGRs?
• RQ2 What is the expected differential power spectrum of GRBs passing through a wormhole throat?
• RQ3 Are known SGRs consistent with being WH-transmitted GRBs, given their spectral hardness and burst duration?
• RQ4 Can identical light curves from different sky directions be evidence of WH-mediated GRBs?
• RQ5 What observational criteria (e.g., duration, spectral hardness, lack of afterglow) could identify a GRB as a WH candidate?

Key findings

• The differential power spectrum of WH-transmitted GRBs follows a $ s^{-5/2} $ dependence under uniform source distribution, consistent with Euclidean space geometry.
• Known SGRs are unlikely to be WH candidates due to their soft spectra and persistent 2–8 s pulsations, which are better explained by magnetar models.
• No confirmed candidates for WH-transmitted GRBs have been identified; the search for recurrent GRBs in BATSE data (e.g., triggers 5646–5649) yielded no statistically significant evidence.
• Harder, longer-duration repeating GRBs—distinct from SGRs—could be potential WH candidates, as they may reflect emission from the other universe.
• GRBs with no detectable host galaxies or optical afterglows (dark GRBs) may indicate WH proximity or cosmological WHs, respectively.
• If a WH connects two regions of our universe, the same GRB event could be observed twice with identical light curves, delayed by a time factor related to throat mass ratios.