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 $<$10 mHz is an almostunexplored regime in X-ray binaries and ultraluminous X-ray sources. We compareour findings with the (few) examples of very low frequency variability found inother accreting sources, and discuss possible explanations (Lense-Thirringprecession of the inner flow or outflow; radiation pressure limit-cycleinstability; marginally stable He burning on the neutron star surface).
Quasi periodic whispers from a transient ULX in M 101: signatures of a fast-spinning neutron star?
Paolo Esposito;
2022-01-01
Abstract
We have studied the unusual time variability of an ultraluminous X-ray sourcein M 101, 4XMM J140314.2$+$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).I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
