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Planet-Disk Interactions
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Planet-disk interactions, where an embedded massive body interacts gravitationally with the protoplanetary disk it was formed in, can play an important role in reshaping both the disk and the orbit of the planet. Spiral density waves are launched into the disk by the planet, which, if they are strong enough, can lead to the formation of a gap. Both effects are observable with current instruments. The back-reaction of perturbations induced in the disk, both wave-like and non-wavelike, is a change in orbital elements of the planet. The efficiency of orbital migration is a long-standing problem in planet formation theory. We discuss recent progress in planet-disk interactions for different planet masses and disk parameters, in particular the level of turbulence, and progress in modeling observational signatures of embedded planets.
Forward citations
Cited by 6 Pith papers
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The Distinctive Evolution and Spectral Energy Distribution of Binary Massive Black Hole Accretion
Combining three accretion disk states for binary massive black holes, the paper predicts a spectrum 'notch' and a mass-ratio evolution attractor at q~1e-3 for extreme-mass-ratio binaries.
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Dynamically Selected Mass-Radius Relationship for Low Mass Exoplanets
Planets inferred to have suffered giant collisions are more massive than pristine ones but retain comparable hydrogen envelope fractions, implying collisions occurred before disk gas dispersal.
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The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): V. Protoplanetary gas disk masses
Median protoplanetary disk gas mass falls from about 0.007 solar masses in Ophiuchus (under 1 Myr) to about 0.0007 to 0.0009 solar masses in Lupus and Upper Sco (1 to 6 Myr), with carbon monoxide depleted about tenfol...
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Capture and Escape of Planetary Mean-motion Resonances in Turbulent Discs
Active disc turbulence raises equilibrium eccentricities and overstability growth rates in mean-motion resonances, causing migrating planet pairs to escape toward tighter resonances.
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Dust Growth in Binary Systems: Inhibition of dust settling and growth in circumbinary discs
Dust grains in circumbinary discs end up five times smaller than in single-star discs, and the conditions for streaming-instability clumping are not met, arguing against in-situ planet formation there.
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A JWST, ALMA and VLA survey of the Ophiuchus-A star-forming region: Unveiling hidden dust mass and connecting infrared outflows to their radio origins
A multi-wavelength survey of 20 Ophiuchus protostars finds dust masses tens to hundreds of times larger than millimetre-only estimates, if the adopted dust-opacity model is correct.
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