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Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs
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| Zeitschriftentitel: | The Astrophysical Journal |
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| Personen und Körperschaften: | , , |
| In: | The Astrophysical Journal, 851, 2017, 2, S. 129 |
| Format: | E-Article |
| Sprache: | Unbestimmt |
| veröffentlicht: |
American Astronomical Society
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| Schlagwörter: |
| author_facet |
Nerush, E. N. Serebryakov, D. A. Kostyukov, I. Yu. Nerush, E. N. Serebryakov, D. A. Kostyukov, I. Yu. |
|---|---|
| author |
Nerush, E. N. Serebryakov, D. A. Kostyukov, I. Yu. |
| spellingShingle |
Nerush, E. N. Serebryakov, D. A. Kostyukov, I. Yu. The Astrophysical Journal Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs Space and Planetary Science Astronomy and Astrophysics |
| author_sort |
nerush, e. n. |
| spelling |
Nerush, E. N. Serebryakov, D. A. Kostyukov, I. Yu. 0004-637X 1538-4357 American Astronomical Society Space and Planetary Science Astronomy and Astrophysics http://dx.doi.org/10.3847/1538-4357/aa9d1a <jats:title>Abstract</jats:title> <jats:p>We present the results of the theoretical analysis and numerical simulations of the Weibel instability in two counterstreaming hot relativistic plasma flows, for instance the flows of electron–proton plasmas with rest-mass densities <jats:inline-formula> <jats:tex-math> <?CDATA $\rho \sim {10}^{-4}\,{\rm{g}}\,{\mathrm{cm}}^{-3}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn1.gif" xlink:type="simple" /> </jats:inline-formula>, Lorentz factors <jats:inline-formula> <jats:tex-math> <?CDATA ${\rm{\Gamma }}\sim 10$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn2.gif" xlink:type="simple" /> </jats:inline-formula>, and proper temperatures <jats:inline-formula> <jats:tex-math> <?CDATA $T\sim {10}^{13}\ {\rm{K}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn3.gif" xlink:type="simple" /> </jats:inline-formula>. The instability growth rate and the filament size at the linear stage are found analytically and are in qualitative agreement with the results of three-dimensional particle-in-cell simulations. In the simulations, incoherent synchrotron emission and pair photoproduction in electromagnetic fields are taken into account. If the plasma flows are dense, fast, and hot enough, the overall energy of the synchrotron photons can be much higher than the energy of the generated electromagnetic fields. Furthermore, a sizable number of positrons can be produced due to the pair photoproduction in the generated magnetic field. We propose a rough criterion to judge copious pair production and considerable synchrotron losses. By means of this criterion, we conclude that the incoherent synchrotron emission and the pair production during the Weibel instability can have implications for the collapsar model of gamma-ray bursts.</jats:p> Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs The Astrophysical Journal |
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American Astronomical Society, 2017 |
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American Astronomical Society, 2017 |
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0004-637X 1538-4357 |
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2017 |
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American Astronomical Society |
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The Astrophysical Journal |
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| title |
Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_unstemmed |
Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_full |
Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_fullStr |
Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_full_unstemmed |
Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_short |
Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_sort |
weibel instability in hot plasma flows with the production of gamma-rays and electron–positron pairs |
| topic |
Space and Planetary Science Astronomy and Astrophysics |
| url |
http://dx.doi.org/10.3847/1538-4357/aa9d1a |
| publishDate |
2017 |
| physical |
129 |
| description |
<jats:title>Abstract</jats:title>
<jats:p>We present the results of the theoretical analysis and numerical simulations of the Weibel instability in two counterstreaming hot relativistic plasma flows, for instance the flows of electron–proton plasmas with rest-mass densities <jats:inline-formula>
<jats:tex-math>
<?CDATA $\rho \sim {10}^{-4}\,{\rm{g}}\,{\mathrm{cm}}^{-3}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn1.gif" xlink:type="simple" />
</jats:inline-formula>, Lorentz factors <jats:inline-formula>
<jats:tex-math>
<?CDATA ${\rm{\Gamma }}\sim 10$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn2.gif" xlink:type="simple" />
</jats:inline-formula>, and proper temperatures <jats:inline-formula>
<jats:tex-math>
<?CDATA $T\sim {10}^{13}\ {\rm{K}}$?>
</jats:tex-math>
<jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn3.gif" xlink:type="simple" />
</jats:inline-formula>. The instability growth rate and the filament size at the linear stage are found analytically and are in qualitative agreement with the results of three-dimensional particle-in-cell simulations. In the simulations, incoherent synchrotron emission and pair photoproduction in electromagnetic fields are taken into account. If the plasma flows are dense, fast, and hot enough, the overall energy of the synchrotron photons can be much higher than the energy of the generated electromagnetic fields. Furthermore, a sizable number of positrons can be produced due to the pair photoproduction in the generated magnetic field. We propose a rough criterion to judge copious pair production and considerable synchrotron losses. By means of this criterion, we conclude that the incoherent synchrotron emission and the pair production during the Weibel instability can have implications for the collapsar model of gamma-ray bursts.</jats:p> |
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| author | Nerush, E. N., Serebryakov, D. A., Kostyukov, I. Yu. |
| author_facet | Nerush, E. N., Serebryakov, D. A., Kostyukov, I. Yu., Nerush, E. N., Serebryakov, D. A., Kostyukov, I. Yu. |
| author_sort | nerush, e. n. |
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| description | <jats:title>Abstract</jats:title> <jats:p>We present the results of the theoretical analysis and numerical simulations of the Weibel instability in two counterstreaming hot relativistic plasma flows, for instance the flows of electron–proton plasmas with rest-mass densities <jats:inline-formula> <jats:tex-math> <?CDATA $\rho \sim {10}^{-4}\,{\rm{g}}\,{\mathrm{cm}}^{-3}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn1.gif" xlink:type="simple" /> </jats:inline-formula>, Lorentz factors <jats:inline-formula> <jats:tex-math> <?CDATA ${\rm{\Gamma }}\sim 10$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn2.gif" xlink:type="simple" /> </jats:inline-formula>, and proper temperatures <jats:inline-formula> <jats:tex-math> <?CDATA $T\sim {10}^{13}\ {\rm{K}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn3.gif" xlink:type="simple" /> </jats:inline-formula>. The instability growth rate and the filament size at the linear stage are found analytically and are in qualitative agreement with the results of three-dimensional particle-in-cell simulations. In the simulations, incoherent synchrotron emission and pair photoproduction in electromagnetic fields are taken into account. If the plasma flows are dense, fast, and hot enough, the overall energy of the synchrotron photons can be much higher than the energy of the generated electromagnetic fields. Furthermore, a sizable number of positrons can be produced due to the pair photoproduction in the generated magnetic field. We propose a rough criterion to judge copious pair production and considerable synchrotron losses. By means of this criterion, we conclude that the incoherent synchrotron emission and the pair production during the Weibel instability can have implications for the collapsar model of gamma-ray bursts.</jats:p> |
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| imprint | American Astronomical Society, 2017 |
| imprint_str_mv | American Astronomical Society, 2017 |
| institution | DE-Brt1, DE-Zwi2, DE-D161, DE-Gla1, DE-Zi4, DE-15, DE-Rs1, DE-Pl11, DE-105, DE-14, DE-Ch1, DE-L229, DE-D275, DE-Bn3 |
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| physical | 129 |
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| publisher | American Astronomical Society |
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| recordtype | ai |
| series | The Astrophysical Journal |
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| spelling | Nerush, E. N. Serebryakov, D. A. Kostyukov, I. Yu. 0004-637X 1538-4357 American Astronomical Society Space and Planetary Science Astronomy and Astrophysics http://dx.doi.org/10.3847/1538-4357/aa9d1a <jats:title>Abstract</jats:title> <jats:p>We present the results of the theoretical analysis and numerical simulations of the Weibel instability in two counterstreaming hot relativistic plasma flows, for instance the flows of electron–proton plasmas with rest-mass densities <jats:inline-formula> <jats:tex-math> <?CDATA $\rho \sim {10}^{-4}\,{\rm{g}}\,{\mathrm{cm}}^{-3}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn1.gif" xlink:type="simple" /> </jats:inline-formula>, Lorentz factors <jats:inline-formula> <jats:tex-math> <?CDATA ${\rm{\Gamma }}\sim 10$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn2.gif" xlink:type="simple" /> </jats:inline-formula>, and proper temperatures <jats:inline-formula> <jats:tex-math> <?CDATA $T\sim {10}^{13}\ {\rm{K}}$?> </jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjaa9d1aieqn3.gif" xlink:type="simple" /> </jats:inline-formula>. The instability growth rate and the filament size at the linear stage are found analytically and are in qualitative agreement with the results of three-dimensional particle-in-cell simulations. In the simulations, incoherent synchrotron emission and pair photoproduction in electromagnetic fields are taken into account. If the plasma flows are dense, fast, and hot enough, the overall energy of the synchrotron photons can be much higher than the energy of the generated electromagnetic fields. Furthermore, a sizable number of positrons can be produced due to the pair photoproduction in the generated magnetic field. We propose a rough criterion to judge copious pair production and considerable synchrotron losses. By means of this criterion, we conclude that the incoherent synchrotron emission and the pair production during the Weibel instability can have implications for the collapsar model of gamma-ray bursts.</jats:p> Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs The Astrophysical Journal |
| spellingShingle | Nerush, E. N., Serebryakov, D. A., Kostyukov, I. Yu., The Astrophysical Journal, Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs, Space and Planetary Science, Astronomy and Astrophysics |
| title | Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_full | Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_fullStr | Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_full_unstemmed | Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_short | Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| title_sort | weibel instability in hot plasma flows with the production of gamma-rays and electron–positron pairs |
| title_unstemmed | Weibel Instability in Hot Plasma Flows with the Production of Gamma-Rays and Electron–Positron Pairs |
| topic | Space and Planetary Science, Astronomy and Astrophysics |
| url | http://dx.doi.org/10.3847/1538-4357/aa9d1a |