Two recent studies published in Nature Communications and The Astronomical Journal highlight the commonality and exclusivity of Jupiter-sized exoplanets, also known as Exo-Jupiters. 

Here are some commonalities of Exo-Jupiters: 

• Opaque clouds and hazes Larger exoplanets, including some hot Jupiters, have opaque clouds and hazes. 
• Radio emissions from exomoons Based on the commonality between Jupiter and Saturn, authors suggest that radio emissions from exomoons may be common and detectable. 
• Formation paths Two well-studied theories to explain the formation of hot Jupiters are disk migration and high-eccentricity migration. 

Here are some exclusions of Exo-Jupiters: 

• COROT-exo-3b: This object is about the size of Jupiter, but has more than 20 times the mass. 
• Saturated targets: Targets that are saturated are excluded. 
• Faintest star in a pair: The faintest star in a pair is excluded.

The two studies that highlight the commonality and exclusivity of exo-Jupiters may help astronomers better understand the formation and evolution of gas giant exoplanets. These exoplanets are between the size of Jupiter and Saturn. 

Here are some other studies related to exo-Jupiters: 

• Evidence for Two Hot-Jupiter Formation Paths: This study excludes hot Jupiters around secondary stars detected through radial velocity. 
• Disk migration and high-eccentricity migration: These are two theories that explain the formation of hot Jupiters. 
• Theory for planetary exospheres: This study highlights the interest of this derivation for case studies of exoplanets, particularly for hot Jupiters. 
• Exoplanet Exploration Program Analysis Group (ExoPAG) Study: This study excludes some type of known false positive. 
• Five Key Exoplanet Questions Answered via the Analysis of 25 Hot: This study highlights the potential impact of metal hydrides and metal oxides in regulating the thermal properties of the dayside of hot Jupiters. 
• Discriminating between hazy and clear hot-Jupiter atmospheres: This study aims to study the presence of hazes in the atmospheres of HD 209458 b and HD 189733 b.

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