Radio Nebulae from Hyperaccreting X-Ray Binaries as Common-envelope Precursors and Persistent Counterparts of Fast Radio Bursts

Sridhar, Navin; Metzger, Brian

doi:10.3847/1538-4357/ac8a4a

Cited by 34 publications

(27 citation statements)

References 169 publications

(235 reference statements)

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“…The extreme RM (∼10 5 rad m −2 ; Michilli et al 2018;Hilmarsson et al 2021) of FRB 20121102A may be from the compact PRSs (Margalit & Metzger 2018;Yang et al 2022a;Sridhar & Metzger 2022). Therefore, there may be two possible RM evolution trends of FRB 20121102A afterward.…”

Section: Discussionmentioning

confidence: 99%

“…Objects FRB 20121102A (Chatterjee et al 2017) and FRB 20190520B (Niu et al 2022) are associated with compact luminous (νL ν ∼ 10 39 erg s −1 ) PRSs. The compact PRS may be from a magnetar wind nebula (Margalit & Metzger 2018;, a magnetized plasma screen (Yang et al 2022a), or ultraluminous X-ray hypernebulae (Sridhar & Metzger 2022). All of the above models consider PRSs to be associated with large RMs (∼10 4 -10 5 rad m −2 ) and that the age of the center engine is very young (e.g., 14-22 yr in Zhao & Wang 2021 and 10 yr in Sridhar & Metzger 2022).…”

Section: Compact Prssmentioning

confidence: 99%

“…Considering that the binary model of Sridhar & Metzger (2022) has evolved as a common-envelope precursor, we will not discuss this model here. Besides, there are two possible origins of luminous PRSs in massive binaries: the scaled-down pulsar wind nebulae (PWNe; Margalit & Metzger 2018; in HMGBs or the companion wind as the plasma screen (Yang et al 2022a).…”

Section: Compact Prssmentioning

confidence: 99%

“…The differences in the observed DMs and RMs of FRBs mean that there may be different origins or that they are all from magnetars but in different environments. The large (∼10 5 rad m −2 ) and decreasing RM of FRB 20121102A (Michilli et al 2018;Hilmarsson et al 2021) may be from the magnetar wind nebula (Margalit & Metzger 2018;, a pulsar near a supermassive black hole (Zhang 2018;Katz 2021a;Yang et al 2022b), or a hyperaccreting X-ray binary (Sridhar & Metzger 2022). The extreme DM of FRB 20190520B may be related to the host galaxy (Niu et al 2022) or a young supernova remnant (SNR; Katz 2022).…”

Section: Introductionmentioning

confidence: 99%

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Rotation Measure Variations and Reversals of Repeating FRBs in Massive Binary Systems

Zhao

Zhang

Wang

et al. 2023

ApJ

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Recent observations discovered that some repeating fast radio bursts (FRBs) show complicated variations and reversals of Faraday rotation measures (RMs), indicating that the sources of these FRBs are embedded in a dynamically magnetized environment. One possible scenario is that repeating FRBs are generated by pulsars in binary systems, especially containing a high-mass companion with strong stellar outflows. Here we study the RM variations caused by stellar winds and a possible stellar disk. If the magnetic field is radial in the stellar wind, RMs will not reverse except if the magnetic axis inclination angle is close to 90°. For the toroidal magnetic field in the wind, RMs will reverse at the superconjunction. For the case of the toroidal field in the disk, the RM variations may have a multimodal and multiple reversal profile because the radio signals travel through different components of the disk during periastron passage. We also apply this model to FRB 20180916B. By assuming that its 16.35 day period is from a slowly rotating or freely precessing magnetar, we find that the secular RM variation can be explained by the periastron passage of a magnetar in a massive binary system. In addition, the clumps in the stellar wind and disk can cause short timescale (<1 day) variations or reversals of RM. Therefore, long-term monitoring of RM variations can reveal the environments of repeating FRBs.

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Section: Discussionmentioning

confidence: 99%

Section: Compact Prssmentioning

confidence: 99%

Section: Compact Prssmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Rotation Measure Variations and Reversals of Repeating FRBs in Massive Binary Systems

Zhao

Zhang

Wang

et al. 2023

ApJ

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“…Much of the recent work on luminous magnetar wind nebulae has been done in the context of PRSs associated with repeating FRBs (e.g., Murase et al 2016;Beloborodov 2017;Margalit & Metzger 2018), a connection that has recently been strengthened by the detection of a low-luminosity FRB from the Galactic magnetar SGR 1935+2154 (Bochenek et al 2020;CHIME/FRB Collaboration et al 2020), though see Sridhar & Metzger (2022) for an alternative model involving a highly super-Eddington stellar-mass BH. There are a number of observational similarities between VT 1137-0337 and PRSs.…”

Section: Comparison With Frb Persistent Sourcesmentioning

confidence: 99%

A Flat-spectrum Radio Transient at 122 Mpc Consistent with an Emerging Pulsar Wind Nebula

Dong

Hallinan

2023

ApJ

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We report the discovery and follow-up observations of VT 1137–0337, an unusual radio transient found in our systematic search for extragalactic explosions in the Very Large Array Sky Survey. It is located in the brightest region of a dwarf starburst galaxy at a luminosity distance of 121.6 Mpc. Its 3 GHz luminosity is comparable to luminous radio supernovae associated with dense circumstellar interaction and relativistic outflows. However, its broadband radio spectrum—proportional to ν −0.35 over a range of ≳10× in frequency and fading at a rate of 5% yr–1—cannot be directly explained by the shock of a stellar explosion. Jets launched by various classes of accreting black holes also struggle to account for VT 1137–0337's combination of observational properties. Instead, we propose that VT 1137–0337 is a decades-old pulsar wind nebula that has recently emerged from within the free–free opacity of its surrounding supernova ejecta. If the nebula is powered by spin-down, the central neutron star should have a surface dipole field of ∼1013–1014 G and a present-day spin period of ∼10–100 ms. Alternatively, the nebula may be powered by the release of magnetic energy from a magnetar. Magnetar nebulae have been proposed to explain the persistent radio sources associated with the repeating fast radio bursts FRB 121102 and FRB 190520B. These FRB persistent sources have not previously been observed as transients but do bear a striking resemblance to VT 1137–0337 in their radio luminosity, spectral index, and host galaxy properties.

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The host galaxy of FRB 20171020A revisited

Lee-Waddell

James

Ryder

et al. 2023

Publ. Astron. Soc. Aust.

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The putative host galaxy of FRB 20171020A was first identified as ESO 601-G036 in 2018, but as no repeat bursts have been detected, direct confirmation of the host remains elusive. In light of recent developments in the field, we re-examine this host and determine a new association confidence level of 98%. At 37 Mpc, this makes ESO 601-G036 the third closest FRB host galaxy to be identified to date and the closest to host an apparently non-repeating FRB (with an estimated repetition rate limit of $<$ $0.011$ bursts per day above $10^{39}$ erg). Due to its close distance, we are able to perform detailed multi-wavelength analysis on the ESO 601-G036 system. Follow-up observations confirm ESO 601-G036 to be a typical star-forming galaxy with H i and stellar masses of $\log_{10}\!(M_{\rm{H\,{\small I}}} / M_\odot) \sim 9.2$ and $\log_{10}\!(M_\star / M_\odot) = 8.64^{+0.03}_{-0.15}$ , and a star formation rate of $\text{SFR} = 0.09 \pm 0.01\,{\rm M}_\odot\,\text{yr}^{-1}$ . We detect, for the first time, a diffuse gaseous tail ( $\log_{10}\!(M_{\rm{H\,{\small I}}} / M_\odot) \sim 8.3$ ) extending to the south-west that suggests recent interactions, likely with the confirmed nearby companion ESO 601-G037. ESO 601-G037 is a stellar shred located to the south of ESO 601-G036 that has an arc-like morphology, is about an order of magnitude less massive, and has a lower gas metallicity that is indicative of a younger stellar population. The properties of the ESO 601-G036 system indicate an ongoing minor merger event, which is affecting the overall gaseous component of the system and the stars within ESO 601-G037. Such activity is consistent with current FRB progenitor models involving magnetars and the signs of recent interactions in other nearby FRB host galaxies.

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Radio Nebulae from Hyperaccreting X-Ray Binaries as Common-envelope Precursors and Persistent Counterparts of Fast Radio Bursts

Cited by 34 publications

References 169 publications

Rotation Measure Variations and Reversals of Repeating FRBs in Massive Binary Systems

Rotation Measure Variations and Reversals of Repeating FRBs in Massive Binary Systems

A Flat-spectrum Radio Transient at 122 Mpc Consistent with an Emerging Pulsar Wind Nebula

The host galaxy of FRB 20171020A revisited

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