arXiv (All)
open access
Turbulent viscosity in line-driven stellar winds
Radiation-driven winds from massive stars generate powerful outflows known to be intrinsically turbulent. Despite this, standard hydrodynamic models have historically restricted the application of macroscopic turbulent viscosity to rotationally supported disks, neglecting its dynamic role in the sup
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
- Examining Stellar Age Gradients of Dwarf Galaxies and Implementing Turbulence-based Star Formation in Cosmological Simulations#637456
- Computational advances and challenges in simulations of turbulence and star formation#1062803
- Globular cluster formation from inertial inflows: accreting extremely massive stars as the origin of abundance anomalies#314998
- Examination of the relationship between spectral type and stellar rotational velocity in ∼50,000 single stars#639902
- The ringing Large Magellanic Cloud: evidence for a recent dwarf-dwarf collision#1355216
Record · ID 1232991
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