Anti-glitches in the Ultraluminous Accreting Pulsar NGC 300 ULX-1 Observed with NICER

Ray, Paul S.; Guillot, Sebastien; Ho, Wynn C. G.; Kerr, M.; Enoto, T.; Gendreau, Keith C.; Arzoumanian, Zaven; Altamirano, D.; Bogdanov, Slavko; Campion, R. P.; Chakrabarty, Deepto; Deneva, J. S.; Jaisawal, Gaurava K.; Kozon, Robert P.; Malacaria, C.; Strohmayer, Tod E.; Wolff, M. T.

doi:10.3847/1538-4357/ab24d8

Cited by 40 publications

(35 citation statements)

References 60 publications

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“…Pulsation periods and the associated uncertainties were also calculated by fitting the pulse times of arrival (TOA) with a timing model. We followed the methodology described by Ray et al (2011), that has been applied to other HMXB pulsars (Ray et al 2019b;Vasilopoulos et al 2019Vasilopoulos et al , 2020. We subdivided the data into 10-20 intervals and generated TOAs by comparing the pulse profile of each interval with a template profile.…”

Section: Timing Analysismentioning

confidence: 99%

Revisiting the spectral and timing properties of 4U 1909+07 with NuSTAR and Astrosat

Jaisawal

Naik

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the results obtained from the analysis of high mass X-ray binary pulsar 4U 1909+07 using NuSTAR and Astrosat observations in 2015 and 2017 July, respectively. X-ray pulsations at ≈604 s are clearly detected in our study. Based on the long term spin-frequency evolution, the source is found to spun up in the last 17 years. We observed a strongly energy-dependent pulse profile that evolved from a complex broad structure in soft X-rays into a profile with a narrow emission peak followed by a plateau in energy ranges above 20 keV. This behaviour ensured a positive correlation between the energy and pulse fraction. The pulse profile morphology and its energy-evolution are almost similar during both the observations, suggesting a persistent emission geometry of the pulsar over time. The broadband energy spectrum of the pulsar is approximated by an absorbed high energy exponential cutoff power law model with iron emission lines. In contrast to the previous report, we found no statistical evidence for the presence of cyclotron absorption features in the X-ray spectra. We performed phase-resolved spectroscopy by using data from the NuSTAR observation. Our results showed a clear signature of absorbing material at certain pulse-phases of the pulsar. These findings are discussed in terms of stellar wind distribution and its effect on the beam geometry of this wind-fed accreting neutron star. We also reviewed the subsonic quasi-spherical accretion theory and its implication on the magnetic field of 4U 1909+07 depending on the global spin-up rate.

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Section: Timing Analysismentioning

confidence: 99%

Revisiting the spectral and timing properties of 4U 1909+07 with NuSTAR and Astrosat

Jaisawal

Naik

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…As its behavior cannot be accounted by the standard glitch theory, different models assuming an internal [182][183][184] or external [185] origin have been proposed. More recently, new anti-glitches have been reported in the accreting pulsar NGC 300 ULX-1 [186]. Despite the present uncertainties, a precise detection of a glitch in a pulsar with known mass in a binary system would substantially increase our understanding of NS interiors.…”

Section: Glitch Activitymentioning

confidence: 97%

Phase transitions in neutron stars and their links to gravitational waves

Orsaria

Malfatti

Mariani

et al. 2019

J. Phys. G: Nucl. Part. Phys.

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The recent direct observation of gravitational wave event GW 170817 and its GRB170817A signal has opened up a new window to study neutron stars and heralds a new era of Astronomy referred to as the Multimessenger Astronomy. Both gravitational and electromagnetic waves from a single astrophysical source have been detected for the first time. This combined detection offers an unprecedented opportunity to place constraints on the neutron star matter equation of state. The existence of a possible hadron-quark phase transition in the central regions of neutron stars is associated with the appearance of g-modes, which are extremely important as they could signal the presence of a pure quark matter core in the centers of neutron stars. Observations of g-modes with frequencies between 1 kHz and 1.5 kHz could be interpreted as evidence of a sharp hadron-quark phase transition in the cores of neutron stars. In this article, we shall review the description of the dense matter composing neutron stars, the determination of the equation of state of such matter, and the constraints imposed by astrophysical observations of these fascinating compact objects. arXiv:1907.04654v1 [astro-ph.HE]

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“…The observed spin period showed the fast evolution with the period derivative of 10 −7 −10 −5 s s −1 . Another feature of this source is that its secular period evolution rate is quite stable, as well as its luminosity after MJD 57740 [14,38,42,37].…”

Section: Observations Of the Rotational Behaviors For Different Sourcesmentioning

confidence: 98%

“…We have included the different observations for each source, while the only observed parameters with notable differences are included, and in the calculations, we avoid using Ṗ computed based on just comparing two spin period or long timescale average measurements (marked with * ). Since the observation information and parameters are not complete, many other measured data [34,35,14,36,37,38,39] are not listed.…”

Section: Observations Of the Rotational Behaviors For Different Sourcesmentioning

confidence: 99%

Studying magnetic fields of ultraluminous X-ray pulsars using different accretion torques

Chen¹,

Wang²,

Tong³

2021

Preprint

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The magnetic field of ultraluminous X-ray (ULX) pulsars is the key parameter to understand the nature and accretion physics. However, the typical magnetic field values in these ULX pulsars are still under debate. We used six different torque models to study the magnetic fields of ULX pulsars, to see how derived magnetic fields change with different models, and to determine which models are more suitable for ULX pulsars. We took the currently available period, period derivative, and flux data of 7 confirmed ULX pulsars, M82 X-2, ULX NGC 7793 P13, ULX NGC 5907, NGC 300 ULX1, NGC 1313 X-2, M51 ULX-7, Swift J0243.6+6124, plus one potential ULX pulsars, SMC X-3. The magnetic fields of these ULX pulsars were constrained from two physical conditions: the spin-up process and near equilibrium. We checked possible dependence of the magnetic field estimations on the different torque models. The calculations suggest the accretion torque models by Ghosh & Lamb [1], Wang [2], Kluźniak & Rappaport [3] and Campbell [4] are more likely to support magnetar models for ULX pulsars, while Lovelace, Romanova & Bisnovatyi-Kogan [5]'s model generally predicts the magnetic field in normal neutron stars. Implications of our results combined with other independent methods are also discussed, which will help us to understand the nature and rotational behavior of these ULX pulsars.

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Anti-glitches in the Ultraluminous Accreting Pulsar NGC 300 ULX-1 Observed with NICER

Cited by 40 publications

References 60 publications

Revisiting the spectral and timing properties of 4U 1909+07 with NuSTAR and Astrosat

Revisiting the spectral and timing properties of 4U 1909+07 with NuSTAR and Astrosat

Phase transitions in neutron stars and their links to gravitational waves

Studying magnetic fields of ultraluminous X-ray pulsars using different accretion torques

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