论文标题
磁性形成通过原源星中的对流发电机
Magnetar formation through a convective dynamo in protoneutron stars
论文作者
论文摘要
通过磁力释放旋转能量是为多种极端爆炸性瞬变提供动力的有希望的场景。但是，它缺乏牢固的基础，因为磁性形成仍然代表了理论上的挑战。使用基于原始恒星内部模型的对流发电机的第一个三维模拟，我们证明了所需的偶性磁场可以始终如一地生成足够快速的旋转速率。磁性能力的磁能超过了动能的磁性能力饱和，高达10倍。我们的结果与银河系磁场强度的观察性约束兼容，并为gamma-ray burp and lumima burst and superlumuminous supernova Centernova Centrleca Centralsines grounsemagnetar模型提供了强有力的理论支持。
The release of spin-down energy by a magnetar is a promising scenario to power several classes of extreme explosive transients. However, it lacks a firm basis because magnetar formation still represents a theoretical challenge. Using the first three-dimensional simulations of a convective dynamo based on a protoneutron star interior model, we demonstrate that the required dipolar magnetic field can be consistently generated for sufficiently fast rotation rates. The dynamo instability saturates in the magnetostrophic regime with the magnetic energy exceeding the kinetic energy by a factor of up to 10. Our results are compatible with the observational constraints on galactic magnetar field strength and provide strong theoretical support for millisecond protomagnetar models of gamma-ray burst and superluminous supernova central engines.
