A Multi-wavelength Characterization of the 2023 Outburst of MAXI J1807+132: Manifestations of Disk Instability and Jet Emission
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2025
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| author | Rout, Sandeep K. Baglio, M. Cristina Hughes, Andrew Russell, David M. Bramich, D. M. Saikia, Payaswini Alabarta, Kevin Padilla, Montserrat Armas Campana, Sergio Covino, Stefano D'Avanzo, Paolo Fender, Rob Goldoni, Paolo Homan, Jeroen Lewis, Fraser Masetti, Nicola Motta, Sara Munoz-Darias, Teo Papitto, Alessandro Russell, Thomas D. Sivakoff, Gregory Eijnden, Jakob van den |
| author_facet | Rout, Sandeep K. Baglio, M. Cristina Hughes, Andrew Russell, David M. Bramich, D. M. Saikia, Payaswini Alabarta, Kevin Padilla, Montserrat Armas Campana, Sergio Covino, Stefano D'Avanzo, Paolo Fender, Rob Goldoni, Paolo Homan, Jeroen Lewis, Fraser Masetti, Nicola Motta, Sara Munoz-Darias, Teo Papitto, Alessandro Russell, Thomas D. Sivakoff, Gregory Eijnden, Jakob van den |
| contents | Several phenomenological aspects of low-luminosity neutron star transients, such as atolls, remain poorly understood. One such source, MAXI J1807+132, entered its latest outburst in July 2023. To thoroughly characterize this outburst, we conducted an extensive observational campaign spanning radio to X-ray wavelengths. Here, we present the results of this campaign, which covered the period from before the outburst to the return to quiescence. We detected a delay between the X-ray and optical rise times, which is consistent with the predictions of the disk instability model with a truncated disk. The color evolution and optical/X-ray correlations, along with infrared and radio detections, support the presence of jet synchrotron emission during the gradual decay phase following the peak. We also report for the first time in an X-ray binary a near-orthogonal rotation of the optical polarization just before a small flare, after which the jet is thought to be quenched. The main outburst is followed by several high-amplitude, rapid reflares in the optical, ultraviolet, and X-ray bands, the origin of which remains difficult to constrain. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2506_03641 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A Multi-wavelength Characterization of the 2023 Outburst of MAXI J1807+132: Manifestations of Disk Instability and Jet Emission Rout, Sandeep K. Baglio, M. Cristina Hughes, Andrew Russell, David M. Bramich, D. M. Saikia, Payaswini Alabarta, Kevin Padilla, Montserrat Armas Campana, Sergio Covino, Stefano D'Avanzo, Paolo Fender, Rob Goldoni, Paolo Homan, Jeroen Lewis, Fraser Masetti, Nicola Motta, Sara Munoz-Darias, Teo Papitto, Alessandro Russell, Thomas D. Sivakoff, Gregory Eijnden, Jakob van den High Energy Astrophysical Phenomena Several phenomenological aspects of low-luminosity neutron star transients, such as atolls, remain poorly understood. One such source, MAXI J1807+132, entered its latest outburst in July 2023. To thoroughly characterize this outburst, we conducted an extensive observational campaign spanning radio to X-ray wavelengths. Here, we present the results of this campaign, which covered the period from before the outburst to the return to quiescence. We detected a delay between the X-ray and optical rise times, which is consistent with the predictions of the disk instability model with a truncated disk. The color evolution and optical/X-ray correlations, along with infrared and radio detections, support the presence of jet synchrotron emission during the gradual decay phase following the peak. We also report for the first time in an X-ray binary a near-orthogonal rotation of the optical polarization just before a small flare, after which the jet is thought to be quenched. The main outburst is followed by several high-amplitude, rapid reflares in the optical, ultraviolet, and X-ray bands, the origin of which remains difficult to constrain. |
| title | A Multi-wavelength Characterization of the 2023 Outburst of MAXI J1807+132: Manifestations of Disk Instability and Jet Emission |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2506.03641 |