The variable radio jet of the accreting neutron star the Rapid Burster
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arXiv
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| Auteurs principaux: | , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866913443366305792 |
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| author | Eijnden, J. van den Robins, D. Sharma, R. Sánchez-Fernández, C. Russell, T. D. Degenaar, N. Miller-Jones, J. C. A. Maccarone, T. |
| author_facet | Eijnden, J. van den Robins, D. Sharma, R. Sánchez-Fernández, C. Russell, T. D. Degenaar, N. Miller-Jones, J. C. A. Maccarone, T. |
| contents | The Rapid Burster is a unique neutron star low-mass X-ray binary system, showing both thermonuclear Type-I and accretion-driven Type-II X-ray bursts. Recent studies have demonstrated how coordinated observations of X-ray and radio variability can constrain jet properties of accreting neutron stars - particularly when the X-ray variability is dominated by discrete changes. We present a simultaneous VLA, Swift, and INTEGRAL observing campaign of the Rapid Burster to investigate whether its jet responds to Type-II bursts. We observe the radio counterpart of the X-ray binary at its faintest-detected radio luminosity, while the X-ray observations reveal prolific, fast X-ray bursting. A time-resolved analysis reveals that the radio counterpart varies significantly between observing scans, displaying a fractional variability of $38 \pm 5$%. The radio faintness of the system prevents the robust identification of a causal relation between individual Type-II bursts and the evolution of the radio jet. However, based on a comparison of its low radio luminosity with archival Rapid Burster observations and other accreting neutron stars, and on a qualitative assessment of the X-ray and radio light curves, we explore the presence of a tentative connection between bursts and jet: i.e., the Type-II bursts may weaken or strengthen the jet. The former of those two scenarios would fit with magneto-rotational jet models; we discuss three lines of future research to establish this potential relation between Type-II bursts and jets more confidently. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_19827 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The variable radio jet of the accreting neutron star the Rapid Burster Eijnden, J. van den Robins, D. Sharma, R. Sánchez-Fernández, C. Russell, T. D. Degenaar, N. Miller-Jones, J. C. A. Maccarone, T. High Energy Astrophysical Phenomena The Rapid Burster is a unique neutron star low-mass X-ray binary system, showing both thermonuclear Type-I and accretion-driven Type-II X-ray bursts. Recent studies have demonstrated how coordinated observations of X-ray and radio variability can constrain jet properties of accreting neutron stars - particularly when the X-ray variability is dominated by discrete changes. We present a simultaneous VLA, Swift, and INTEGRAL observing campaign of the Rapid Burster to investigate whether its jet responds to Type-II bursts. We observe the radio counterpart of the X-ray binary at its faintest-detected radio luminosity, while the X-ray observations reveal prolific, fast X-ray bursting. A time-resolved analysis reveals that the radio counterpart varies significantly between observing scans, displaying a fractional variability of $38 \pm 5$%. The radio faintness of the system prevents the robust identification of a causal relation between individual Type-II bursts and the evolution of the radio jet. However, based on a comparison of its low radio luminosity with archival Rapid Burster observations and other accreting neutron stars, and on a qualitative assessment of the X-ray and radio light curves, we explore the presence of a tentative connection between bursts and jet: i.e., the Type-II bursts may weaken or strengthen the jet. The former of those two scenarios would fit with magneto-rotational jet models; we discuss three lines of future research to establish this potential relation between Type-II bursts and jets more confidently. |
| title | The variable radio jet of the accreting neutron star the Rapid Burster |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2405.19827 |