Radio emission from the X-ray pulsar Her X-1: a jet launched by a strong magnetic field neutron star?

Eijnden, J. van den; Degenaar, N.; Russell, Thomas; Miller-Jones, J. C. A.; Wijnands, Rudy; Miller, J. M.; King, A. L.; Rupen, M. P.

doi:10.1093/mnrasl/slx180

Cited by 15 publications

(8 citation statements)

References 40 publications

(66 reference statements)

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“…Hints of disc/jet coupling are found also in weakly accreting sources such as cataclysmic variables (Körding et al 2008), as well as in highly accreting systems such as Ultra Luminous X-ray sources (Roberts 2007;Cseh et al 2015;van den Eijnden et al 2018) and Tidal Disruption Events (TDEs, Dai et al 2018). In particular, TDEs offer the opportunity to observe in real time the on-set of jet activity at high (Bloom et al 2011) and low power (Pasham & van Velzen 2018;van Velzen et al 2016;Alexander et al 2016Alexander et al , 2017Mattila et al 2018).…”

Section: Comparison With Other Accreting Sourcesmentioning

confidence: 99%

The origin of radio emission from radio-quiet active galactic nuclei

et al. 2019

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The central nuclei of galaxies, where super-massive black holes (SMBHs) are thought to reside, can experience phases of activity when they become Active Galactic Nuclei (AGN). An AGN can eject winds, jets, and produce radiation across the entire electromagnetic spectrum. The fraction of the bolometric emission in the radio spans a factor of ∼10 5 across the different AGN classes. The weakest radio sources, radio-quiet (RQ) AGN, are typically 1,000 times fainter than the radio-loud (RL) AGN, and represent the majority of the AGN population. In RL AGN, radio emission is essentially all produced by synchrotron emission from a relativistic jet. In contrast, in RQ AGN the absence of luminous jets allows us to probe radio emission from a wide range of possible mechanisms, from the host galaxy kpc scale down to the innermost region near the SMBHs: star formation, AGN driven wind, free-free emission from photo-ionized gas, low power jet, and the innermost accretion disc coronal activity. All these mechanisms can now be probed with unprecedented precision and spatial resolution, thanks to the current and forthcoming generation of highly sensitive radio arrays.

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Section: Comparison With Other Accreting Sourcesmentioning

confidence: 99%

The origin of radio emission from radio-quiet active galactic nuclei

et al. 2019

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“…X-ray re-brightenings during outburst decays are seen in dwarf novae and occasionally in LMXBs (see for an overview Chen et al 1997), such as the NSs SAX J1808.4-3658 Sanna et al 2017;Patruno et al 2016) and IGR J17379-3747 (van den Eijnden et al 2018d) and the BHs XTE J1650-500 (Tomsick et al 2004), Swift J1910.2-0546 (Tomsick et al 2013), GRS 1739-278 (Yan & Yu 2017), and MAXI J1535-571 (Parikh et al 2018). As discussed in detail in Patruno et al (2016), these re-brightenings appear to be caused by the hydrogen-ionisation instability, which is also responsible for the main outburst (Lasota 2001).…”

Section: The Origin Of the X-ray Re-brighteningsmentioning

confidence: 99%

“…Duldig et al 1979;Nelson & Spencer 1988;Fender & Hendry 2000;Migliari & Fender 2006) and observations of individual targets (Tudose et al 2010;Migliari et al 2011). Recently, radio emission was detected from the two stronglymagnetized accreting NSs GX 1+4 (van den Eijnden et al 2018b) and Her X-1 (van den Eijnden et al 2018a). However, the exact origin of this radio emission remains undetermined as limited spectral and temporal information made a direct jet inference impossible.…”

Section: Jets From Strongly-magnetized Neutron Starsmentioning

confidence: 99%

A re-establishing jet during an X-ray re-brightening of the Be/X-ray binary Swift J0243.6+6124

Eijnden

Degenaar

Russell

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Transient Be/X-ray binary systems, wherein a compact object accretes from a Becompanion star, can show giant and periastron outbursts. During the decay of their giant outbursts, some Be/X-ray binaries also show X-ray re-brightenings, the origin of which is not understood. Recently, we presented the discovery of a jet from a neutron star Be/X-ray binary, observed during the giant outburst of Swift J0243.6+6124. Here, we present continued radio monitoring of its 2017/2018 giant outburst decay and a re-brightening of this source. During the former, we observe a radio flare with a steep radio spectrum, possibly caused by interactions between discrete ejecta colliding with the pre-existing jet or the surrounding medium. During the X-ray re-brightening, we observe the radio jet turning on and off within days. Surprisingly, this re-establishing jet is as bright in radio as at the peak of the super-Eddington giant outburst, despite more than two orders of magnitude lower X-ray luminosity. In addition, the jet is only observed when the X-ray luminosity exceeds approximately 2 × 10 36 (D/5kpc) 2 erg/s. We discuss how such an X-ray threshold for jet launching might be related to the presence of a magnetic centrifugal barrier at lower mass accretion rates. We also discuss the implications of our results for the launch of jets from strongly magnetized neutron stars, and explore future avenues to exploit the new possibility of coordinated X-ray/radio studies of neutron star Be/X-ray binaries.

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“…By observing a sample of sources over the wide frequency coverage of the ngVLA, we can additionally observe how the jet break frequency depends on the properties of the accretion flow. Observations of the BHXRBs MAXI J1836-194 and MAXI J1659-152 suggest that the jet break evolves to lower radio frequencies as X-ray spectrum softens and the accretion flow geometry changes during an outburst (Russell et al 2013(Russell et al , 2014van der Horst et al 2013). The jet-break frequency is thus expected to move through the ngVLA bands during the hard-to-soft state transition.…”

Section: Jet Propertiesmentioning

confidence: 99%

Science with an ngVLA: Accretion and Jets in Local Compact Objects

Coppejans,

Miller-Jones,

Koerding

et al. 2018

Preprint

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Despite the prevalence of jets in accreting systems and their impact on the surrounding medium, the fundamental physics of how they are launched and collimated is not fully understood. Radio observations of local compact objects, including accreting stellar mass black holes, neutron stars and white dwarfs, probe their jet emission. Coupled with multi-wavelength observations, this allows us to test the underlying accretion-outflow connection and to establish the relationship between the accretor properties and the jet power, which is necessary to accurately model jets. Compact accretors are nearby, numerous and come in a range of accretor properties, and hence are ideal probes for the underlying jet physics. Despite this there are a number of key outstanding questions regarding accretion-driven outflows in these objects that cannot be answered with current radio observations. The vastly improved sensitivity, polarization capabilities, spatial resolution and high-frequency coverage of the ngVLA will be crucial to answering these, and subsequently determining the fundamental physics behind accretion and jets at all physical scales.

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Radio emission from the X-ray pulsar Her X-1: a jet launched by a strong magnetic field neutron star?

Cited by 15 publications

References 40 publications

The origin of radio emission from radio-quiet active galactic nuclei

The origin of radio emission from radio-quiet active galactic nuclei

A re-establishing jet during an X-ray re-brightening of the Be/X-ray binary Swift J0243.6+6124

Science with an ngVLA: Accretion and Jets in Local Compact Objects

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