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Unified Formation Channel of Hot and Warm Jupiters via Planet-Planet Scattering
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DOI：10.3847/2041-8213/ae61b0.png)
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Abstract
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Recent observations show distinct orbital architectures for hot and warm Jupiters: hot Jupiters span a wide range of stellar obliquities and tend to host distant companions without close-by companions, whereas warm Jupiters are often aligned and accompanied by both close-by and distant companions. In this Letter, we revisit planet-planet scattering and demonstrate that it provides a unified framework for both populations. Using N-body simulations with tides, we explore three regimes: hot (a(1) < 0.1 au), warm (0.1 < a(1) < 1 au), and cold (1 < a(1) < 10 au) scattering. Hot scattering predominantly produces compact hot Jupiter pairs, which are rarely observed, implying this channel is rare. Cold scattering readily produces retrograde hot Jupiters and likely constitutes a main reservoir feeding the hot Jupiter population. However, cold scattering produces few inner warm Jupiters at a similar or equal to 0.1-0.3 au. We show that warm scattering naturally fills this gap: high-inclination inner warm Jupiters produced by warm scattering are preferentially removed through further eccentricity excitation followed by tidal circularization into hot Jupiters. As a result, the surviving inner warm Jupiters are biased toward a broad range of eccentricities but modest inclinations, producing the observed eccentric-but-aligned population. This theory makes testable predictions: (i) warm Jupiters, especially at a greater than or similar to 0.3 au, should not be exclusively aligned; and (ii) warm Jupiters should often host nearby companions with nonnegligible mutual inclinations up to less than or similar to 30 degrees.
Keywords:
GAS GIANT PLANETS
ALIGNED ORBIT
CLOSE-IN
SYSTEMS
OUTCOMES
ORIGIN
CONSTRAINTS
COMPANIONS
EVOLUTION
MIGRATION
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