We have studied the unusual time variability of an ultraluminous X-ray sourcein M 101, 4XMM J140314.2$+$541806 (henceforth, J1403), using Chandra andXMM-Newton data. Over the last two decades, J1403 has shown short-durationoutbursts with an X-ray luminosity $sim1-3 imes 10^{39}$ erg s$^{-1}$, andlonger intervals at luminosities $sim0.5-1 imes 10^{38}$ erg s$^{-1}$. Thebimodal behaviour and fast outburst evolution (sometimes only a few days) aremore consistent with an accretor/propeller scenario for a neutron star thanwith the canonical outburst cycles of stellar-mass black holes. If thisscenario is correct, the luminosities in the accretor and propeller statessuggest a fast spin ($P approx$ 5 ms) and a low surface magnetic field ($Bsim 10^{10}$ G), despite our identification of J1403 as a high-mass X-raybinary. The most striking property of J1403 is the presence of strong$sim$600-s quasi periodic oscillations (QPOs), mostly around frequencies of$approx 1.3-1.8$ mHz, found at several epochs during the ultraluminous regime.We illustrate the properties of such QPOs, in particular their frequency andamplitude changes between and within observations, with a variety of techniques(Fast Fourier Transforms, Lomb-Scargle periodograms, weighted waveletZ-transform analysis). The QPO frequency range $<$10 mHz is an almostunexplored regime in X-ray binaries and ultraluminous X-ray sources. We compareour findings with the (few) examples of very low frequency variability found inother accreting sources, and discuss possible explanations (Lense-Thirringprecession of the inner flow or outflow; radiation pressure limit-cycleinstability; marginally stable He burning on the neutron star surface).

Quasi periodic whispers from a transient ULX in M 101: signatures of a fast-spinning neutron star?

Paolo Esposito;
2022

Abstract

We have studied the unusual time variability of an ultraluminous X-ray sourcein M 101, 4XMM J140314.2$+$541806 (henceforth, J1403), using Chandra andXMM-Newton data. Over the last two decades, J1403 has shown short-durationoutbursts with an X-ray luminosity $sim1-3 imes 10^{39}$ erg s$^{-1}$, andlonger intervals at luminosities $sim0.5-1 imes 10^{38}$ erg s$^{-1}$. Thebimodal behaviour and fast outburst evolution (sometimes only a few days) aremore consistent with an accretor/propeller scenario for a neutron star thanwith the canonical outburst cycles of stellar-mass black holes. If thisscenario is correct, the luminosities in the accretor and propeller statessuggest a fast spin ($P approx$ 5 ms) and a low surface magnetic field ($Bsim 10^{10}$ G), despite our identification of J1403 as a high-mass X-raybinary. The most striking property of J1403 is the presence of strong$sim$600-s quasi periodic oscillations (QPOs), mostly around frequencies of$approx 1.3-1.8$ mHz, found at several epochs during the ultraluminous regime.We illustrate the properties of such QPOs, in particular their frequency andamplitude changes between and within observations, with a variety of techniques(Fast Fourier Transforms, Lomb-Scargle periodograms, weighted waveletZ-transform analysis). The QPO frequency range $<$10 mHz is an almostunexplored regime in X-ray binaries and ultraluminous X-ray sources. We compareour findings with the (few) examples of very low frequency variability found inother accreting sources, and discuss possible explanations (Lense-Thirringprecession of the inner flow or outflow; radiation pressure limit-cycleinstability; marginally stable He burning on the neutron star surface).
accretion, accretion discs – stars: neutron – X-rays: binaries – X-rays: individual: 4XMM J140314.2 + 541806
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/20.500.12076/11116
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