The radial density of planets increases with depth due to compressibility, leading impacts on their convective dynamics. To account for these effects, including the presence a quasi-adiabatic temperature profile and entropy sources dissipation, compressibility is expressed through dissipation number, $\mathcal{D}$, proportional planet's radius gravity. In Earth's mantle, effects are moderate, b...

We propose a planet formation scenario to explain the elevated occurrence rates of transiting planets around M dwarfs compared sun-like stars discovered by Kepler. use pebble drift and accretion model simulate growth cores inside outside snow line. A smaller size interior line delays super-Earths, allowing giant in outer disk form first. When those reach isolation mass they cut off flow pebbles...

I have enjoyed reading several items on the rare-earth elements in Physics Today over past few years. David Kramer’s most recent piece focused topic (February 2021, page 20) was about neodymium-based magnets, but readers might be interested to learn of another class magnets based samarium. Among their applications are traveling wave tubes (TWTs), which form backbone world’s entire space communi...

The conditions in the protoplanetary disc are determinant for various planet formation mechanisms. We present a framework which combines self-consistent structures with calculations of growth rates planetary embryos via pebble accretion, order to study Super-Earths. first perform 2D hydrodynamical simulations inner discs, considering grain size distribution multiple chemical species and their c...