Discovery of Three Candidate Magnetar-powered Fast X-ray Transients from Chandra Archival Data

Lin, Dacheng; Irwin, Jimmy A.; Berger, Edo; Nguyen, Ronny

doi:10.48550/arxiv.2201.06754

Cited by 2 publications

(2 citation statements)

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“…This rotational energy reservoir has been used to explain many different features of various electromagnetic transients. Such as the X-ray plateaus of gamma-ray bursts (e.g., Rowlinson et al 2010;Dall'Osso et al 2011;Rowlinson et al 2013;Lasky et al 2017;Strang & Melatos 2019;Sarin et al 2020b;Strang et al 2021), some fast X-ray transients (Xue et al 2019;Yang et al 2019;Ai & Zhang 2021;Lin et al 2022), or bright kilonovae (e.g., Fong et al 2021). However, in many cases, the same observations could be interpreted with the afterglow produced by a structured relativistic jet (Beniamini et al 2020;, or attributed to systematics and not require a neutron star central engine (Zhu et al 2021;O'Connor et al 2021).…”

Section: Introductionmentioning

confidence: 99%

On the diversity of magnetar-driven kilonovae

Sarin

Omand

Margalit

et al. 2022

Monthly Notices of the Royal Astronomical Society

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A non-negligible fraction of binary neutron star mergers are expected to form long-lived neutron star remnants, dramatically altering the multimessenger signatures of a merger. Here, we extend existing models for magnetar-driven kilonovae and explore the diversity of kilonovae and kilonova afterglows. Focusing on the role of the (uncertain) magnetic field strength, we study the resulting electromagnetic signatures as a function of the external dipolar and internal toroidal fields. These two parameters govern, respectively, the competition between magnetic-dipole spin-down and gravitational-wave spin-down (due to magnetic-field deformation) of the rapidly rotating remnant. We find that even in the parameter space where gravitational-wave emission is dominant, a kilonova with a magnetar central engine will be significantly brighter than one without an engine, as this parameter space is where more of the spin-down luminosity is thermalized. In contrast, a system with minimal gravitational-wave emission will produce a kilonova that may be difficult to distinguish from ordinary kilonovae unless early epoch observations are available. However, as the bulk of the energy in this parameter space goes into accelerating the ejecta, such a system will produce a brighter kilonova afterglow that will peak in shorter times. To effectively hide the presence of the magnetar from the kilonova and kilonova afterglow, the rotational energy inputted into the ejecta must be ≲10−3to 10−2Erot. We discuss the different diagnostics available to identify magnetar-driven kilonovae in serendipitous observations and draw parallels to other potential magnetar-driven explosions, such as superluminous supernovae and broad-line supernovae Ic.

show abstract

Section: Introductionmentioning

confidence: 99%

On the diversity of magnetar-driven kilonovae

Sarin

Omand

Margalit

et al. 2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…This rotational energy reservoir has been used to explain many different features of various electromagnetic transients. Such as the X-ray plateaus of gamma-ray bursts (e.g., Rowlinson et al 2010;Dall'Osso et al 2011;Rowlinson et al 2013;Lasky et al 2017;Sarin et al 2020b), some fast X-ray transients (Xue et al 2019;Yang et al 2019;Ai & Zhang 2021;Lin et al 2022), or bright kilonovae (e.g., Fong et al 2021). However, in many cases, the same observations could be interpreted with the afterglow produced by a structured relativistic jet (Beniamini et al 2020;, or attributed to systematics and not require a neutron star central engine (Zhu et al 2021;O'Connor et al 2021).…”

Section: Introductionmentioning

confidence: 99%

On the diversity of magnetar-driven kilonovae

Sarin,

Omand,

Margalit

et al. 2022

Preprint

View full text Add to dashboard Cite

A non-negligible fraction of binary neutron star mergers are expected to form long-lived neutron star remnants, dramatically altering the multi-messenger signatures of a merger. Here, we extend existing models for magnetar-driven kilonovae and explore the diversity of kilonovae and kilonova afterglows. Focusing on the role of the (uncertain) magnetic field strength, we study the resulting electromagnetic signatures as a function of the external dipolar and internal toroidal fields. These two parameters govern, respectively, the competition between magneticdipole spindown and gravitational-wave spindown (due to magnetic-field deformation) of the rapidly-rotating remnant. We find that even in the parameter space where gravitationalwave emission is dominant, a kilonova with a magnetar central engine will be significantly brighter than one without an engine, as this parameter space is where more of the spin-down luminosity is thermalised. In contrast, a system with minimal gravitational-wave emission will produce a kilonova that may be difficult to distinguish from ordinary kilonovae unless earlyepoch observations are available. However, as the bulk of the energy in this parameter space goes into accelerating the ejecta, such a system will produce a brighter kilonova afterglow that will peak on shorter times. To effectively hide the presence of the magnetar from the kilonova and kilonova afterglow, the rotational energy inputted into the ejecta must be 10 −3 − 10 −2 𝐸 rot . We discuss the different diagnostics available to identify magnetar-driven kilonovae in serendipitous observations and draw parallels to other potential magnetar-driven explosions, such as superluminous supernovae and broad-line supernovae Ic.

show abstract

Discovery of Three Candidate Magnetar-powered Fast X-ray Transients from Chandra Archival Data

Cited by 2 publications

References 43 publications

On the diversity of magnetar-driven kilonovae

On the diversity of magnetar-driven kilonovae

On the diversity of magnetar-driven kilonovae

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