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Estimates of the Dynamic Characteristics of Binary Systems for Traversable Wormholes Search

This paper investigates the observational signatures of traversable wormholes in binary systems by modeling the gravitational perturbations caused by a companion object on the other side of the throat, demonstrating that future radial velocity measurements with 1.5 km/s accuracy could detect these effects immediately, while even current 10 km/s accuracy would allow for statistically significant identification within approximately 17 years using advanced spectral and non-parametric analysis methods.

Original authors: I. A. Moiseev, O. S. Sazhina

Published 2026-04-03

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CC BY 4.0

Original authors: I. A. Moiseev, O. S. Sazhina

Original paper licensed under CC BY 4.0 (http://creativecommons.org/licenses/by/4.0/). ✨ This is an AI-generated explanation of the paper below. It is not written or endorsed by the authors. For technical accuracy, refer to the original paper. Read full disclaimer

Imagine the universe as a giant, cosmic house. Usually, we think of rooms (stars and planets) connected by hallways. But what if there were secret tunnels connecting two completely different rooms, or even two different houses entirely? In physics, these tunnels are called Wormholes.

For a long time, wormholes were just cool ideas in science fiction or complex math equations. But this paper asks a very practical question: "If a wormhole exists right next to us, how would we actually spot it?"

Here is the story of their investigation, explained simply.

The Setup: A Cosmic Game of "Whack-a-Mole"

The authors imagine a specific scenario:

Side 1 (Our Side): We have a binary system—a "dark" object (like a Black Hole or a suspected Wormhole) and a bright star orbiting it. We can see the bright star and measure how fast it's moving toward or away from us (its radial velocity).
Side 2 (The Other Side): On the other end of the wormhole tunnel, there is another massive star orbiting around.

The Analogy:
Imagine you are standing in a room (Side 1) listening to a fan (the star) spinning. Suddenly, someone on the other side of a hidden door (the wormhole) starts kicking a heavy ball around. Even though you can't see the ball or the other room, the vibrations from that kicking travel through the door and make the fan in your room wobble slightly.

The paper tries to figure out: Can we detect that tiny wobble?

The Problem: The "Static" in the Room

Detecting this wobble is incredibly hard because the universe is noisy.

The Noise: Other stars nearby, dark matter, and random gravitational tugs create a "static" or background noise. It's like trying to hear a whisper in a crowded, noisy stadium.
The Competitor: The authors first checked if the "crowd noise" (random stars bumping into each other) would drown out the "whisper" (the wormhole effect).
The Result: In the center of our galaxy, the noise is loud, but the wormhole signal is still louder. However, for the specific systems they are looking at (wide binary stars like Gaia BH1), the noise is very quiet. This makes them the perfect "listening posts."

The Solution: The "Matched Filter" (The Magic Ear)

Since the signal is so tiny, you can't just look at a graph and say, "Aha! There it is!" You need a special tool.

The authors created a digital template (a "magic ear").

How it works: They calculated exactly what the wobble should look like if a wormhole were there. It's not a smooth wave; it's a series of tiny, sharp "kicks" that happen every time the star on the other side swings closest to the tunnel.
The Trick: They take their real data and slide this "magic ear" over it. If the data matches the template, the tool screams "Signal Found!" If it doesn't match, it's just noise.

They also used two other methods:

The LS Periodogram: Like tuning a radio to find a specific frequency. If the wobble happens at a regular rhythm, this tool finds the "station."
The ALK Statistic: A non-math-heavy way to look for patterns in messy data, like spotting a rhythm in a chaotic drumbeat.

The Findings: How Long Do We Have to Wait?

The paper ran simulations to see how long we need to watch these stars to be sure.

The "Super-Telescope" Scenario: If our future telescopes are incredibly precise (measuring speed to within 1.5 km/s), we could detect the wormhole signal immediately, no matter how long we've been watching.
The "Realistic" Scenario: If we use current technology (accurate to about 10 km/s), we need to be patient. The authors calculated that we would need to accumulate data for about 17 years to be statistically sure the signal is real and not just a fluke.

Why Does This Matter?

There is a famous system called Gaia BH1. It has a black hole and a star. But astronomers are confused:

If it's a normal black hole, the star that died to create it should have been huge, which doesn't fit the current orbit.
If it's a Wormhole, the math works perfectly without needing a giant dead star.

This paper suggests that by watching Gaia BH1 (and similar systems) for the next 17 years, we might finally catch the "wobble" that proves a wormhole exists.

The Bottom Line

The universe might be full of secret tunnels. We can't see them, but we can listen for the vibrations they cause. By using clever math to filter out the cosmic noise, we might just be able to hear the "kick" of a star on the other side of the universe, proving that wormholes are real.

In short: We are building a better stethoscope to listen for the heartbeat of a wormhole, and if we listen long enough (about 17 years), we might finally hear it.

1. Problem Statement

The paper addresses the challenge of distinguishing Traversable Wormholes (WHs) from Black Holes (BHs) through observational astronomy. While both objects are compact and massive, standard General Relativity (GR) metrics often make them indistinguishable in the immediate vicinity of the event horizon.

The authors propose a novel observational strategy focusing on wide binary systems where a compact object (a WH candidate) is paired with a luminous companion star. The core hypothesis is that if the compact object is a traversable WH, a massive object located on the "other side" of the wormhole throat (Side 2) will exert a gravitational influence on the companion star (Side 1). This influence manifests as a specific, cumulative perturbation in the companion star's radial velocity (RV), distinct from the effects of a standard BH or a triple-star system.

2. Methodology

The study employs a multi-stage approach combining theoretical modeling, stochastic analysis, and statistical signal processing.

A. Theoretical Model

System Configuration: A wide binary system consisting of a compact object (WH candidate) and a companion star. The WH connects "Side 1" (observer's universe) and "Side 2" (the other side of the throat).
Perturbation Mechanism: A massive object (star) on Side 2 orbits the WH throat with non-zero eccentricity. Its time-varying gravitational field induces an acceleration on the Side 1 companion star.
Metric Assumption: For wide systems, the metric is approximated as Schwarzschild at a distance from the throat. The WH throat radius is set to the gravitational radius ( $R = 2GM/c^2$ ).
Velocity Perturbation: The authors derive an expression for the change in line-of-sight velocity ( $\Delta v$ ) caused by the gravitational impulse from Side 2. The perturbation is inversely proportional to the square of the radial coordinate of the Side 1 star ( $1/r_1^2$ ).

B. Competing Effects Analysis

To validate the detectability of the WH signal, the authors analyze competing noise sources:

Stellar Stochasticity (S-cluster): For supermassive BH candidates (e.g., Sgr A*), the stochastic gravitational force from surrounding stars is calculated. The authors find this noise is an order of magnitude lower than the expected WH perturbation but remains the dominant competing effect in galactic centers.
Wide Binary Systems: For systems like Gaia BH1, BH2, and BH3, the stellar density is low, making stochastic stellar perturbations negligible. This makes wide binaries the primary target for this search.

C. Statistical Detection Framework

The authors develop a pipeline to detect the subtle RV perturbations against observational noise:

Matched Filtering: A template ( $u(t)$ ) is constructed based on the theoretical impulse structure. The Signal-to-Noise Ratio (SNR) is calculated using a robust statistic ( $Z_{obs}$ ) derived from the integral of the filtered signal, normalized by the Median Absolute Deviation (MAD) of the noise distribution.
Spectral Analysis: The Lomb-Scargle (LS) periodogram is used to identify periodic harmonics ( $k/P$ ) in the residual RV data, corresponding to the orbital period of the perturbing object on Side 2.
Non-Parametric Analysis: The Abbe–Lafler–Kinman (ALK) statistic is employed to detect periodicity without assuming a specific functional form, sorting data by phase to find minima in variance.

3. Key Contributions

Novel Detection Signature: The paper identifies that the primary observable signature of a traversable WH in a binary system is not a single impulse, but a cumulative shortening of the orbital period of the companion star. This creates a phase lag between the predicted Keplerian velocity and the observed velocity, which accumulates over time.
Robust Statistical Methods: The authors demonstrate that combining matched filtering with spectral (LS) and non-parametric (ALK) methods significantly reduces the required data accumulation time compared to using matched filtering alone.
Differentiation from Triple Systems: The study argues that the WH-induced perturbation is distinguishable from a triple-star system. In a triple system, the third body's effect is a standard Keplerian perturbation without the specific cumulative phase shift and harmonic structure induced by the "other side" mass through the wormhole throat.
Template Construction: A specific, dimensionless template is constructed that accounts for the inverse-square dependence of the perturbation on the star's radial distance, allowing for the detection of the signal even in sparse datasets.

4. Results

The authors simulated the detection efficiency using the Gaia BH1 system as a prototype (mass $\sim 9.6 M_\odot$ , companion $\sim 0.9 M_\odot$ , period $\sim 185$ days) and synthetic systems with varying parameters.

Detection Thresholds:
- High Precision (1.5 km/s): At this level of RV accuracy (expected in the near future), the WH perturbation is detectable across all considered observation time spans using both LS and ALK methods.
- Current Precision (10 km/s): For more realistic, current observational limits, the LS periodogram becomes statistically significant after approximately 17 years of data accumulation.
Data Sparsity: The methods remain effective even with sparse data (e.g., 100 observations per year). The harmonic structure of the perturbation persists even when the sampling is non-uniform.
Signal Characteristics: The dominant contribution to the signal is the period shortening, which manifests as a growing residual in the RV curve. The matched filter statistic ( $\rho^2$ ) shows a prominent maximum near the pericenter passage.
Degeneracy Resolution: The authors address the potential degeneracy between the WH signal and errors in orbital parameter determination. They conclude that matched filtering with a local, accurate template (sensitive to discrete jumps) can distinguish the WH signal from smooth errors in orbital parameters.

5. Significance

Observational Viability: The paper provides a concrete, quantitative roadmap for searching for traversable wormholes using existing and upcoming astronomical facilities (e.g., Gaia, ELT). It moves the concept of WHs from purely theoretical speculation to an observational search program.
Resolution of Gaia BH1 Anomalies: The study offers a potential explanation for the Gaia BH1 system, where the existence of a stellar-mass BH is difficult to reconcile with the lack of a supergiant progenitor. A WH model avoids the need for a stellar evolution explanation for the compact object.
Methodological Advancement: By demonstrating that non-parametric and spectral methods can drastically shorten the required observation baseline (from decades to potentially less time depending on noise levels), the paper enhances the feasibility of detecting these exotic phenomena.
Cosmological Context: The model relies on the existence of phantom dark energy to stabilize the wormhole throat, linking the search for WHs to current cosmological constraints (e.g., DESI experiment results) regarding the equation of state of dark energy.

In conclusion, Moiseev and Sazhina establish that the gravitational influence of a massive object on the "other side" of a traversable wormhole creates a unique, cumulative perturbation in the radial velocity of a companion star. This effect is distinguishable from standard BH dynamics and triple systems, and is detectable within a human-relevant timeframe using advanced statistical analysis of RV data.