# Proto-Neutron Star Winds, Magnetar Birth, and Gamma-Ray Bursts

## TL;DR

This paper reviews proto-neutron star wind theory, extends it to include magnetic fields and rotation, and argues that rapidly rotating proto-magnetars can produce relativistic winds suitable for long gamma-ray bursts.

## Contribution

It provides new analytic models for magnetically-driven proto-neutron star winds considering multi-dimensional effects and links these to gamma-ray burst production.

## Key findings

- Proto-magnetars with millisecond periods produce relativistic winds shortly after collapse.
- Magnetically-driven winds have properties conducive to gamma-ray burst generation.
- Analytic scalings connect proto-magnetar parameters to observable burst characteristics.

## Abstract

We begin by reviewing the theory of thermal, neutrino-driven proto-neutron star (PNS) winds. Including the effects of magnetic fields and rotation, we then derive the mass and energy loss from magnetically-driven PNS winds for both relativistic and non-relativistic outflows, including important multi-dimensional considerations. With these simple analytic scalings we argue that proto-magnetars born with ~ millisecond rotation periods produce relativistic winds just a few seconds after core collapse with luminosities, timescales, mass-loading, and internal shock efficiencies favorable for producing long-duration gamma-ray bursts.