Three-dimensional GRMHD Simulations of Neutron Star Jets
Neutron stars and black holes in X-ray binaries are observed to host strong collimated jets in the hard spectral state. Numerical simulations can act as a valuable tool in understanding the mechanisms behind jet formation and its properties. Although there have been significant efforts in understand...
| Main Authors: | , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal Letters |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/2041-8213/ad151f |
| _version_ | 1797361751141908480 |
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| author | Pushpita Das Oliver Porth |
| author_facet | Pushpita Das Oliver Porth |
| author_sort | Pushpita Das |
| collection | DOAJ |
| description | Neutron stars and black holes in X-ray binaries are observed to host strong collimated jets in the hard spectral state. Numerical simulations can act as a valuable tool in understanding the mechanisms behind jet formation and its properties. Although there have been significant efforts in understanding black hole jets from general relativistic magnetohydrodynamic (GRMHD) simulations in recent years, neutron star jets still remain poorly explored. We present the results from three-dimensional GRMHD simulations of accreting neutron stars with oblique magnetospheres for the very first time. The jets in our simulations are produced due to the anchored magnetic field of the rotating star in analogy with the Blandford–Znajek process. We find that for accreting stars, the star–disk magnetic field interaction plays a significant role, and as a result, the jet power becomes directly proportional to ${{{\rm{\Phi }}}^{2}}_{\mathrm{jet}}$ , where Φ _jet is the open flux in the jet. The jet power decreases with increasing stellar magnetic inclination, and finally, for an orthogonal magnetosphere, it reduces by a factor of ≃2.95 compared to the aligned case. We also find that in the strong propeller regime, with a highly oblique magnetosphere, the disk-induced collimation of the open stellar flux preserves parts of the striped wind, resulting in a striped jet. |
| first_indexed | 2024-03-08T15:57:57Z |
| format | Article |
| id | doaj.art-cb6fa6941676488199b2d3e1ddba8d1a |
| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2024-03-08T15:57:57Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Letters |
| spelling | doaj.art-cb6fa6941676488199b2d3e1ddba8d1a2024-01-08T15:37:38ZengIOP PublishingThe Astrophysical Journal Letters2041-82052024-01-019602L1210.3847/2041-8213/ad151fThree-dimensional GRMHD Simulations of Neutron Star JetsPushpita Das0https://orcid.org/0000-0002-4764-6189Oliver Porth1https://orcid.org/0000-0002-4584-2557Anton Pannekoek Institute for Astronomy, University of Amsterdam , Science Park 904, 1098 XH, The NetherlandsAnton Pannekoek Institute for Astronomy, University of Amsterdam , Science Park 904, 1098 XH, The NetherlandsNeutron stars and black holes in X-ray binaries are observed to host strong collimated jets in the hard spectral state. Numerical simulations can act as a valuable tool in understanding the mechanisms behind jet formation and its properties. Although there have been significant efforts in understanding black hole jets from general relativistic magnetohydrodynamic (GRMHD) simulations in recent years, neutron star jets still remain poorly explored. We present the results from three-dimensional GRMHD simulations of accreting neutron stars with oblique magnetospheres for the very first time. The jets in our simulations are produced due to the anchored magnetic field of the rotating star in analogy with the Blandford–Znajek process. We find that for accreting stars, the star–disk magnetic field interaction plays a significant role, and as a result, the jet power becomes directly proportional to ${{{\rm{\Phi }}}^{2}}_{\mathrm{jet}}$ , where Φ _jet is the open flux in the jet. The jet power decreases with increasing stellar magnetic inclination, and finally, for an orthogonal magnetosphere, it reduces by a factor of ≃2.95 compared to the aligned case. We also find that in the strong propeller regime, with a highly oblique magnetosphere, the disk-induced collimation of the open stellar flux preserves parts of the striped wind, resulting in a striped jet.https://doi.org/10.3847/2041-8213/ad151fNeutron starsAccretionX-ray binary starsRelativistic jets |
| spellingShingle | Pushpita Das Oliver Porth Three-dimensional GRMHD Simulations of Neutron Star Jets The Astrophysical Journal Letters Neutron stars Accretion X-ray binary stars Relativistic jets |
| title | Three-dimensional GRMHD Simulations of Neutron Star Jets |
| title_full | Three-dimensional GRMHD Simulations of Neutron Star Jets |
| title_fullStr | Three-dimensional GRMHD Simulations of Neutron Star Jets |
| title_full_unstemmed | Three-dimensional GRMHD Simulations of Neutron Star Jets |
| title_short | Three-dimensional GRMHD Simulations of Neutron Star Jets |
| title_sort | three dimensional grmhd simulations of neutron star jets |
| topic | Neutron stars Accretion X-ray binary stars Relativistic jets |
| url | https://doi.org/10.3847/2041-8213/ad151f |
| work_keys_str_mv | AT pushpitadas threedimensionalgrmhdsimulationsofneutronstarjets AT oliverporth threedimensionalgrmhdsimulationsofneutronstarjets |