期刊
ASTROPHYSICAL JOURNAL
卷 896, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab93c0
关键词
Rotation powered pulsars; Stellar wind bubbles; Interstellar synchrotron emission
资金
- DoE [DE-SC0016542]
- NSF [ACI-1657507, 10001562, 10001521]
- NASA [ATP NNX17AG21G, 80NSSC17K0757]
- Purdue Research Foundation
- U.S. Department of Energy (DOE) [DE-SC0016542] Funding Source: U.S. Department of Energy (DOE)
We construct a turbulent model of the Crab Nebula's nonthermal emission. The present model resolves a number of long-standing problems of the Kennel-Coroniti model: (i) the sigma problem, (ii) the hard spectrum of radio electrons, (iii) the high peak energy of gamma-ray flares, (iv) and the spatial evolution of the infrared (IR) emission. The Nebula contains two populations of injected particles: Component-I, accelerated at the wind termination shock via the Fermi-I mechanism; and Component-II, accelerated in reconnecting turbulence in highly magnetized (sigma >> 1) plasma in the central part of the Crab Nebula. The reconnecting turbulence in Component-II extends from radio to gamma-rays: it accelerates radio electrons with a hard spectrum, destroys the large-scale magnetic flux (and thus resolves the sigma problem), and occasionally produces gamma-ray flares (from the largest-scale reconnection events). The model reproduces the broadband spectrum of the Crab Nebula, from low-frequency synchrotron emission in radio to inverse-Compton emission at TeV energies, as well as the spatially resolved evolution of the spectral indices in the IR and optical bands.
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