How AGN Jets Shine - Particle Acceleration | Research - Edubirdie

University:
Boston University
Course:
CAS PY 105 | Physics 1
Academic year:

2020
Views:

247

Pages:

1
Author:

Nyasia Cardenas

How AGN Jets Shine: Par cle Accelera on by Current‐driven Instabili es AGN jets are rela vis c plasma ou lows emana ng from the centers of massive galaxies. These jets shine across the electromagne c spectrum, and are among the most proliﬁc par cle accelerators in the cosmos. However, the mechanism of this accelera on has been a long ‐standing mystery. I will give a brief overview of the evolu on of par cle accelera on theory, from internal shocks to magne c reconnec on. Then I will present recent numerical simula ons, which reveal that a well‐known instability of the magne c ﬁeld in these jets (the helical kink instability) leads to the eﬃcient conversion of their magne c energy into non‐thermal plasma par cles. This mechanism might also be applicable to solar ﬂares, and outbursts from highly magne zed neutron stars.

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