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Photospheric Radius Expansion and a Double-peaked Type-I X-Ray Burst from GRS 1741.9-2853

Photospheric Radius Expansion and a Double-peaked Type-I X-Ray Burst from GRS 1741.9-2853
Photospheric Radius Expansion and a Double-peaked Type-I X-Ray Burst from GRS 1741.9-2853
We present an analysis of two type-I X-ray bursts observed by NuSTAR originating from the very faint transient neutron star (NS) low-mass X-ray binary GRS 1741.9–2853 during a period of outburst in 2020 May. We show that the persistent emission can be modeled as an absorbed, Comptonized blackbody in addition to Fe Kα emission, which can be attributed to relativistic disk reflection. We measure a persistent bolometric, unabsorbed luminosity of ${L}_{\mathrm{bol}}={7.03}_{-0.05}^{+0.04}\times {10}^{36}\,\mathrm{erg}\,{{\rm{s}}}^{-1}$, assuming a distance of 7 kpc, corresponding to an Eddington ratio of 4.5%. This persistent luminosity combined with light-curve analysis leads us to infer that the bursts were the result of pure He burning rather than mixed H/He burning. Time-resolved spectroscopy reveals that the bolometric flux of the first burst exhibits a double-peaked structure, placing the source within a small population of accreting NSs that exhibit multiple-peaked type-I X-ray bursts. We find that the second, brighter burst shows evidence for photospheric radius expansion (PRE) and that at its peak, this PRE event had an unabsorbed bolometric flux of ${F}_{\mathrm{peak}}={2.94}_{-0.26}^{+0.28}\times {10}^{-8}\,\mathrm{erg}\,{\mathrm{cm}}^{-2}\,{{\rm{s}}}^{-1}$. This yields a new distance estimate of d = 9.0 ± 0.5 kpc, assuming that this corresponds to the Eddington limit for pure He burning on the surface of a canonical NS. Additionally, we performed a detailed timing analysis that failed to find evidence for quasi-periodic oscillations or burst oscillations, and we place an upper limit of 16% on the rms variability around 589 Hz, the frequency at which oscillations have previously been reported.
0004-637X
Pike, Sean N.
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Harrison, Fiona A.
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Tomsick, John A.
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Bachetti, Matteo
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Buisson, Douglas J.K.
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Garcia, Javier A.
0783c08d-c7e1-48fd-a280-0e36c30b0208
Jiang, Jiachen
95329273-2124-446e-9e16-b7df729367c9
Ludlam, R.M.
53c3b7dc-c23b-4bf3-84a4-288cbf1bfe52
Madsen, Kristin K.
841133ab-8245-4a2e-b645-e07a1c921f83
Pike, Sean N.
a3e8fd64-fc70-4f89-8948-30319ec9c12e
Harrison, Fiona A.
4e106d1d-5f0e-4a2d-aefd-5e99ada7a5b4
Tomsick, John A.
96b2e8cc-70c1-424a-8380-2551a5077ff5
Bachetti, Matteo
6a6bb4d1-0e16-4284-a923-16115c6d3c9d
Buisson, Douglas J.K.
f96b1210-d056-4948-9e4a-deeb669e6d1a
Garcia, Javier A.
0783c08d-c7e1-48fd-a280-0e36c30b0208
Jiang, Jiachen
95329273-2124-446e-9e16-b7df729367c9
Ludlam, R.M.
53c3b7dc-c23b-4bf3-84a4-288cbf1bfe52
Madsen, Kristin K.
841133ab-8245-4a2e-b645-e07a1c921f83

Pike, Sean N., Harrison, Fiona A., Tomsick, John A., Bachetti, Matteo, Buisson, Douglas J.K., Garcia, Javier A., Jiang, Jiachen, Ludlam, R.M. and Madsen, Kristin K. (2021) Photospheric Radius Expansion and a Double-peaked Type-I X-Ray Burst from GRS 1741.9-2853. Astrophysical Journal, 918 (1), [9]. (doi:10.3847/1538-4357/ac0ef9).

Record type: Article

Abstract

We present an analysis of two type-I X-ray bursts observed by NuSTAR originating from the very faint transient neutron star (NS) low-mass X-ray binary GRS 1741.9–2853 during a period of outburst in 2020 May. We show that the persistent emission can be modeled as an absorbed, Comptonized blackbody in addition to Fe Kα emission, which can be attributed to relativistic disk reflection. We measure a persistent bolometric, unabsorbed luminosity of ${L}_{\mathrm{bol}}={7.03}_{-0.05}^{+0.04}\times {10}^{36}\,\mathrm{erg}\,{{\rm{s}}}^{-1}$, assuming a distance of 7 kpc, corresponding to an Eddington ratio of 4.5%. This persistent luminosity combined with light-curve analysis leads us to infer that the bursts were the result of pure He burning rather than mixed H/He burning. Time-resolved spectroscopy reveals that the bolometric flux of the first burst exhibits a double-peaked structure, placing the source within a small population of accreting NSs that exhibit multiple-peaked type-I X-ray bursts. We find that the second, brighter burst shows evidence for photospheric radius expansion (PRE) and that at its peak, this PRE event had an unabsorbed bolometric flux of ${F}_{\mathrm{peak}}={2.94}_{-0.26}^{+0.28}\times {10}^{-8}\,\mathrm{erg}\,{\mathrm{cm}}^{-2}\,{{\rm{s}}}^{-1}$. This yields a new distance estimate of d = 9.0 ± 0.5 kpc, assuming that this corresponds to the Eddington limit for pure He burning on the surface of a canonical NS. Additionally, we performed a detailed timing analysis that failed to find evidence for quasi-periodic oscillations or burst oscillations, and we place an upper limit of 16% on the rms variability around 589 Hz, the frequency at which oscillations have previously been reported.

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Photospheric Radius Expansion and a Double-peaked Type-I X-Ray Burst from GRS 1741.9-2853 - Accepted Manuscript
Restricted to Repository staff only until 30 August 2022.
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Accepted/In Press date: 24 June 2021
Published date: 30 August 2021
Additional Information: arxiv is am.

Identifiers

Local EPrints ID: 451964
URI: http://eprints.soton.ac.uk/id/eprint/451964
ISSN: 0004-637X
PURE UUID: 25f59321-dde9-4dfb-b6ee-eb8912d799f5

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Date deposited: 04 Nov 2021 17:34
Last modified: 11 Nov 2021 17:30

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Contributors

Author: Sean N. Pike
Author: Fiona A. Harrison
Author: John A. Tomsick
Author: Matteo Bachetti
Author: Douglas J.K. Buisson
Author: Javier A. Garcia
Author: Jiachen Jiang
Author: R.M. Ludlam
Author: Kristin K. Madsen

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