Interpreting Crab Nebula’s synchrotron spectrum: two acceleration mechanisms
Abstract
We outline a model of the Crab pulsar wind nebula with two different populations of synchrotron emitting particles, arising from two different acceleration mechanisms: (i) Component-I due to Fermi-I acceleration at the equatorial portion of the termination shock, with particle spectral index pI ≈ 2.2 above the injection break corresponding to γwindσwind ~105, peaking in the ultraviolet (UV, γwind ~ 102 is the bulk Lorentz factor of the wind, σwind ~ 103 is wind magnetization); and (ii) Component-II due to acceleration at reconnection layers in the bulk of the turbulent Nebula, with particle index pII ≈ 1.6. The model requires relatively slow but highly magnetized wind. For both components, the overall cooling break is in the infrared at ~0.01 eV, so that the Component-I is in the fast cooling regime (cooling frequency below the peak frequency). In the optical band, Component-I produces emission with the cooling spectral index of αo ≈ 0.5, softening towards the edges due to radiative losses. Above the cooling break, in the optical, UV, and X-rays, Component-I mostly overwhelms Component-II. We hypothesize that acceleration at large-scale current sheets in the turbulent nebula (Component-II) extends to the synchrotron burn-off limit of ϵs ~ 100 MeV. Thus in ourmore »
- Authors:
-
[3];
- Department of Physics and Astronomy, Purdue University, 525 Northwestern Avenue, West Lafayette, IN 47907, USA
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
- School of Mathematics, University of Leeds, LS29JT Leeds, UK
- Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA
- Department of Astronomy, Columbia University, 550 W 120th St, New York, NY 10027, USA
- Publication Date:
- Research Org.:
- Purdue Univ., West Lafayette, IN (United States); Columbia Univ., New York, NY (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 1560709
- Alternate Identifier(s):
- OSTI ID: 1802961
- Grant/Contract Number:
- SC0016369; SC0016542
- Resource Type:
- Published Article
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 489 Journal Issue: 2; Journal ID: ISSN 0035-8711
- Publisher:
- Oxford University Press
- Country of Publication:
- United Kingdom
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; Astronomy & Astrophysics; pulsars: Individual: Crab; radiation mechanisms: nonthermal
Citation Formats
Lyutikov, Maxim, Temim, Tea, Komissarov, Sergey, Slane, Patrick, Sironi, Lorenzo, and Comisso, Luca. Interpreting Crab Nebula’s synchrotron spectrum: two acceleration mechanisms. United Kingdom: N. p., 2019.
Web. doi:10.1093/mnras/stz2023.
Lyutikov, Maxim, Temim, Tea, Komissarov, Sergey, Slane, Patrick, Sironi, Lorenzo, & Comisso, Luca. Interpreting Crab Nebula’s synchrotron spectrum: two acceleration mechanisms. United Kingdom. https://doi.org/10.1093/mnras/stz2023
Lyutikov, Maxim, Temim, Tea, Komissarov, Sergey, Slane, Patrick, Sironi, Lorenzo, and Comisso, Luca. Mon .
"Interpreting Crab Nebula’s synchrotron spectrum: two acceleration mechanisms". United Kingdom. https://doi.org/10.1093/mnras/stz2023.
@article{osti_1560709,
title = {Interpreting Crab Nebula’s synchrotron spectrum: two acceleration mechanisms},
author = {Lyutikov, Maxim and Temim, Tea and Komissarov, Sergey and Slane, Patrick and Sironi, Lorenzo and Comisso, Luca},
abstractNote = {We outline a model of the Crab pulsar wind nebula with two different populations of synchrotron emitting particles, arising from two different acceleration mechanisms: (i) Component-I due to Fermi-I acceleration at the equatorial portion of the termination shock, with particle spectral index pI ≈ 2.2 above the injection break corresponding to γwindσwind ~105, peaking in the ultraviolet (UV, γwind ~ 102 is the bulk Lorentz factor of the wind, σwind ~ 103 is wind magnetization); and (ii) Component-II due to acceleration at reconnection layers in the bulk of the turbulent Nebula, with particle index pII ≈ 1.6. The model requires relatively slow but highly magnetized wind. For both components, the overall cooling break is in the infrared at ~0.01 eV, so that the Component-I is in the fast cooling regime (cooling frequency below the peak frequency). In the optical band, Component-I produces emission with the cooling spectral index of αo ≈ 0.5, softening towards the edges due to radiative losses. Above the cooling break, in the optical, UV, and X-rays, Component-I mostly overwhelms Component-II. We hypothesize that acceleration at large-scale current sheets in the turbulent nebula (Component-II) extends to the synchrotron burn-off limit of ϵs ~ 100 MeV. Thus in our model acceleration in turbulent reconnection (Component-II) can produce both hard radio spectra and occasional gamma-ray flares. This model may be applicable to a broader class of high-energy astrophysical objects, like active galactic nuclei and gamma-ray burst jets, where often radio electrons form a different population from the high-energy electrons.},
doi = {10.1093/mnras/stz2023},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 489,
place = {United Kingdom},
year = {2019},
month = {8}
}
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