A persistent disk wind and variable jet outflow in the neutron-star low-mass X-ray binary GX 13+1
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| Main Authors: | , , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866916676800348160 |
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| author | Rogantini, Daniele Homan, Jeroen Plotkin, Richard M. Berg, Maureen van den Miller-Jones, James Neilsen, Joey Chakrabarty, Deepto Fender, Rob P. Schulz, Norbert |
| author_facet | Rogantini, Daniele Homan, Jeroen Plotkin, Richard M. Berg, Maureen van den Miller-Jones, James Neilsen, Joey Chakrabarty, Deepto Fender, Rob P. Schulz, Norbert |
| contents | In low-mass X-ray binaries (LMXBs), accretion flows are often associated with either jet outflows or disk winds. Studies of LMXBs with luminosities up to roughly 20% of the Eddington limit indicate that these outflows generally do not co-occur, suggesting that disk winds might inhibit jets. However, previous observations of LMXBs accreting near or above the Eddington limit show that jets and winds can potentially coexist. To investigate this phenomenon, we carried out a comprehensive multi-wavelength campaign (using VLA, Chandra/HETG, and NICER) on the near-Eddington neutron-star Z source LMXB GX 13+1. NICER and Chandra/HETG observations tracked GX 13+1 across the entire Z-track during high Eddington rates, detecting substantial resonance absorption features originating from the accretion disk wind in all X-ray spectra, which implies a persistent wind presence. Simultaneous VLA observations captured a variable radio jet, with radio emission notably strong during all flaring branch observations-contrary to typical behavior in Z-sources-and weaker when the source was on the normal branch. Interestingly, no clear correlation was found between the radio emission and the wind features. Analysis of VLA radio light curves and simultaneous Chandra/HETG spectra demonstrates that an ionized disk wind and jet outflow can indeed coexist in GX 13+1, suggesting that their launching mechanisms are not necessarily linked in this system. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2504_05452 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A persistent disk wind and variable jet outflow in the neutron-star low-mass X-ray binary GX 13+1 Rogantini, Daniele Homan, Jeroen Plotkin, Richard M. Berg, Maureen van den Miller-Jones, James Neilsen, Joey Chakrabarty, Deepto Fender, Rob P. Schulz, Norbert High Energy Astrophysical Phenomena In low-mass X-ray binaries (LMXBs), accretion flows are often associated with either jet outflows or disk winds. Studies of LMXBs with luminosities up to roughly 20% of the Eddington limit indicate that these outflows generally do not co-occur, suggesting that disk winds might inhibit jets. However, previous observations of LMXBs accreting near or above the Eddington limit show that jets and winds can potentially coexist. To investigate this phenomenon, we carried out a comprehensive multi-wavelength campaign (using VLA, Chandra/HETG, and NICER) on the near-Eddington neutron-star Z source LMXB GX 13+1. NICER and Chandra/HETG observations tracked GX 13+1 across the entire Z-track during high Eddington rates, detecting substantial resonance absorption features originating from the accretion disk wind in all X-ray spectra, which implies a persistent wind presence. Simultaneous VLA observations captured a variable radio jet, with radio emission notably strong during all flaring branch observations-contrary to typical behavior in Z-sources-and weaker when the source was on the normal branch. Interestingly, no clear correlation was found between the radio emission and the wind features. Analysis of VLA radio light curves and simultaneous Chandra/HETG spectra demonstrates that an ionized disk wind and jet outflow can indeed coexist in GX 13+1, suggesting that their launching mechanisms are not necessarily linked in this system. |
| title | A persistent disk wind and variable jet outflow in the neutron-star low-mass X-ray binary GX 13+1 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2504.05452 |