Tidal locking occurs when a celestial body, under the gravitational influence of a larger counterpart, aligns its rotational period with its orbital period, resulting in one side perpetually facing the larger body. Earth’s moon serves as a prominent example of tidal locking.

This process unfolds over extensive time spans, possibly spanning millions of years, as gravitational forces gradually align rotational and orbital periods.

To elucidate the sluggish rotation of Venus, Kane conducted calculations incorporating planetary dimensions, mass, gravity, and rotation rates. Surprisingly, his findings indicate that Venus should have achieved tidal locking within a mere 6.5 million years, a fraction of the solar system’s estimated age of 4.5 billion years.

Hence, the persisting misalignment prompts speculation regarding the influential role of Venus’s atmosphere.

Kane posits that vigorous atmospheric winds contribute to this phenomenon by inducing surface drag, thereby impeding rotation while mitigating the gravitational influence of the sun.

Paradoxically, solar energy serves as both an agent of tidal locking and a catalyst for atmospheric dynamics, impeding complete synchronization.

The intricate interplay between a planet’s atmosphere and its rotational behavior holds implications extending beyond Venus.

As astronomers explore exoplanets, potential habitats for life, Kane underscores the significance of distinguishing between Earth-like and Venus-like planets and considering atmospheric effects on rotation.

Furthermore, Kane highlights the limitations of current exoplanet detection methods, which rely on indirect observations and modeling based on solar system planets. A comprehensive understanding of near-tidally locked planets, exemplified by Venus, could enhance insights into exoplanetary systems and their potential habitability.