Striped Jets in Post–Neutron Star Merger Systems
Models invoking magnetic reconnection as the particle acceleration mechanism within relativistic jets often adopt a gradual energy dissipation profile within the jet. However, such a profile has yet to be reproduced in first-principles simulations. Here we perform a suite of 3D general relativistic...
| Main Authors: | , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ace894 |
| _version_ | 1797694382084718592 |
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| author | Emma Kaufman I. M. Christie A. Lalakos A. Tchekhovskoy D. Giannios |
| author_facet | Emma Kaufman I. M. Christie A. Lalakos A. Tchekhovskoy D. Giannios |
| author_sort | Emma Kaufman |
| collection | DOAJ |
| description | Models invoking magnetic reconnection as the particle acceleration mechanism within relativistic jets often adopt a gradual energy dissipation profile within the jet. However, such a profile has yet to be reproduced in first-principles simulations. Here we perform a suite of 3D general relativistic magnetohydrodynamic simulations of post–neutron star merger disks with an initially purely toroidal magnetic field. We explore the variations in both the microphysics (e.g., nuclear recombination, neutrino emission) and system parameters (e.g, disk mass). In all of our simulations, we find the formation of magnetically striped jets. The stripes result from the reversals in the poloidal magnetic flux polarity generated in the accretion disk. The simulations display large variations in the distributions of stripe duration, τ , and power, 〈 P _Φ 〉. We find that more massive disks produce more powerful stripes, the most powerful of which reaches 〈 P _Φ 〉 ∼ 10 ^49 erg s ^−1 at τ ∼ 20 ms. The power and variability that result from the magnetic reconnection of the stripes agree with those inferred in short-duration gamma-ray bursts. We find that the dissipation profile of the cumulative energy is roughly a power law in both radial distance, z , and τ , with a slope in the range of ∼1.7–3; more massive disks display larger slopes. |
| first_indexed | 2024-03-12T02:57:04Z |
| format | Article |
| id | doaj.art-6072ce921dfa4e8ebd102c052c526c55 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T02:57:04Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-6072ce921dfa4e8ebd102c052c526c552023-09-03T15:13:20ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195414010.3847/1538-4357/ace894Striped Jets in Post–Neutron Star Merger SystemsEmma Kaufman0https://orcid.org/0000-0002-7236-284XI. M. Christie1A. Lalakos2https://orcid.org/0000-0002-6883-6520A. Tchekhovskoy3D. Giannios4Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Physics & Astronomy, Northwestern University , Evanston, IL 60208, USA ekaufman@u.northwestern.edu, ichristi231@gmail.comCenter for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Physics & Astronomy, Northwestern University , Evanston, IL 60208, USA ekaufman@u.northwestern.edu, ichristi231@gmail.comCenter for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Physics & Astronomy, Northwestern University , Evanston, IL 60208, USA ekaufman@u.northwestern.edu, ichristi231@gmail.comCenter for Interdisciplinary Exploration & Research in Astrophysics (CIERA), Physics & Astronomy, Northwestern University , Evanston, IL 60208, USA ekaufman@u.northwestern.edu, ichristi231@gmail.comDepartment of Physics and Astronomy, Purdue University , 525 Northwestern Avenue, West Lafayette, IN 47907, USAModels invoking magnetic reconnection as the particle acceleration mechanism within relativistic jets often adopt a gradual energy dissipation profile within the jet. However, such a profile has yet to be reproduced in first-principles simulations. Here we perform a suite of 3D general relativistic magnetohydrodynamic simulations of post–neutron star merger disks with an initially purely toroidal magnetic field. We explore the variations in both the microphysics (e.g., nuclear recombination, neutrino emission) and system parameters (e.g, disk mass). In all of our simulations, we find the formation of magnetically striped jets. The stripes result from the reversals in the poloidal magnetic flux polarity generated in the accretion disk. The simulations display large variations in the distributions of stripe duration, τ , and power, 〈 P _Φ 〉. We find that more massive disks produce more powerful stripes, the most powerful of which reaches 〈 P _Φ 〉 ∼ 10 ^49 erg s ^−1 at τ ∼ 20 ms. The power and variability that result from the magnetic reconnection of the stripes agree with those inferred in short-duration gamma-ray bursts. We find that the dissipation profile of the cumulative energy is roughly a power law in both radial distance, z , and τ , with a slope in the range of ∼1.7–3; more massive disks display larger slopes.https://doi.org/10.3847/1538-4357/ace894JetsGamma-ray burstsMagnetohydrodynamical simulations |
| spellingShingle | Emma Kaufman I. M. Christie A. Lalakos A. Tchekhovskoy D. Giannios Striped Jets in Post–Neutron Star Merger Systems The Astrophysical Journal Jets Gamma-ray bursts Magnetohydrodynamical simulations |
| title | Striped Jets in Post–Neutron Star Merger Systems |
| title_full | Striped Jets in Post–Neutron Star Merger Systems |
| title_fullStr | Striped Jets in Post–Neutron Star Merger Systems |
| title_full_unstemmed | Striped Jets in Post–Neutron Star Merger Systems |
| title_short | Striped Jets in Post–Neutron Star Merger Systems |
| title_sort | striped jets in post neutron star merger systems |
| topic | Jets Gamma-ray bursts Magnetohydrodynamical simulations |
| url | https://doi.org/10.3847/1538-4357/ace894 |
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