eScholarship
metadata only
Structure, Phase Stability, and Transport in Hydrogen-Bearing Magma Oceans
Sub-Neptune exoplanets are often modeled as rocky interiors surrounded by hydrogen-rich envelopes, but at the pressures and temperatures expected inside these planets, the boundary between rock and atmosphere may not remain sharp. Hydrogen can dissolve into silicate liquids and form supercritical si
Conceptio Open Archive
Analyze & explore related research in Conceptio
Connect this record directly into your research workflow or AI agent. Explore citations across open repositories, query full text, and export structured proof bundles.
This document is indexed with metadata only: full text is not available in the archive for this record. Open the official source ↗
Related documents
- Hydrogen and Helium Dissolution, Outgassing, and Loss in Evolving Sub-Neptune Magma Oceans: Examining Demographic Features and Radius Evolution#1062931
- Radiating Bondi Flows II: Giant Planet Accretion Models#1077873
- Solidification of Earth's mantle led inevitably to a basal magma ocean#1038972
- Effects of Outer Giant Planets on In Situ Formation of Inner Super-Earths#659039
- Effects of Outer Giant Planets on In Situ Formation of Inner Super-Earths#656903
Record · ID 996290
Retrieved via Conceptio: every document is proof-bundled with source, license, and retrieval metadata.
Retrieved via Conceptio: every document is proof-bundled with source, license, and retrieval metadata.
Bring this data into your agent: Connect via MCP or API · 20 free credits to start · no card required
Read the Docs → · View CLI source on GitHub · Conceptio Open Knowledge Archive
Read the Docs → · View CLI source on GitHub · Conceptio Open Knowledge Archive