A systematic analysis of the phase lags associated with the type-C quasi-periodic oscillation in GRS 1915+105

Zhang, L.; Méndez, Mariano; Altamirano, D.; Qu, J. L.; Chen, Li; Καρπούζας, Κωνσταντίνος; Belloni, T.; Bu, Q. C.; Huang, Y.; Ma, Xiang; Tao, Lian; Wang, Yanan

doi:10.1093/mnras/staa797

Cited by 47 publications

(140 citation statements)

References 59 publications

Supporting

Mentioning

119

Contrasting

Order By: Relevance

“…When the QPO frequency descends below 2 Hz; that is, during the linear decay phase, the lag at the QPO frequency averages to zero lag, but the upper harmonic frequency shows hard lags. This behavior is consistent with earlier studies during the outburst phase (Reig et al 2000;Qu et al 2010;Pahari et al 2013;Zhang et al 2020), where the phase lag has a log-linear relationship with the QPO frequency and changes sign approximately at 2 Hz.…”

Section: The Exponential and Linear Decay Phasessupporting

confidence: 92%

“…Interestingly, similar behavior is seen in the transition from exponential and linear decay phases that display a transitional QPO frequency of 2 Hz. In addition, it has been found that the average QPO phase lag is positive above and negative below 2 Hz (Reig et al 2000;Lin et al 2000;Qu et al 2010;Pahari et al 2013;Zhang et al 2020), and a similar trend can be observed between the exponential and linear outburst decay phases. This effect has been attributed to a pivoting lag-energy spectrum with the lag increasing with energy for progressively lower QPO frequencies and decreasing for progressively higher QPO frequencies (Pahari et al 2013;Zhang et al 2020).…”

Section: Comparison With the Previous Low X-ray Flux Statessupporting

confidence: 52%

See 1 more Smart Citation

ALMA/NICER observations of GRS 1915+105 indicate a return to a hard state

Koljonen

Hovatta

2021

A&A

View full text Add to dashboard Cite

Context. GRS 1915+105 is a transient black hole X-ray binary consistently emitting 10–100% of the Eddington luminosity in the X-ray band over the last three decades until mid-2018 when the source luminosity suddenly decreased by an order of magnitude. This phase was followed by a change to a state with even lower average X-ray fluxes never seen before during the outburst but presenting renewed flaring activity at different wavelengths, albeit with mean fluxes still in decline. Aims. GRS 1915+105 has the longest orbital period known among low-mass X-ray binaries, the largest accretion disk size, and therefore the largest mass supply for accretion. The high inclination of the disk allows the study of geometrical effects of the accretion flow such as changes in the height-to-radius ratio or the effect of accretion disk winds on the intrinsic emission that is expected during the outburst decay. In addition, the transient jet is expected to change to a compact, self-absorbed, steady jet. Methods. We conducted two full polarization Atacama Large Millimeter Array observations to study the jet properties during the outburst decay by analyzing the spectral, polarization, and intra-epoch variability for both observation epochs. In addition, we analyzed almost daily Neutron Star Interior Composition Explorer pointing observations, modeling X-ray power spectral densities, spectral energy distributions, and light curves with a physically motivated model to follow the changing accretion disk properties throughout the outburst decay and relating them to the jet emission. Results. We show that the X-ray and millimeter (mm) spectral, timing, and polarization properties are consistent with those of a typical decaying X-ray binary outburst and that GRS 1915+105 has descended into the low-luminosity hard X-ray state. The jet emission in the mm is consistent with a compact, steady jet with ∼1% linear polarization, and the magnetic field is likely aligned with the jet position angle. Relating the mm emission to the X-ray emission reveals that the source has changed from a higher radio/X-ray correlation index to a lower one; Lradio ∝ LX0.6.

show abstract

Section: The Exponential and Linear Decay Phasessupporting

confidence: 92%

Section: Comparison With the Previous Low X-ray Flux Statessupporting

confidence: 52%

ALMA/NICER observations of GRS 1915+105 indicate a return to a hard state

Koljonen

Hovatta

2021

A&A

View full text Add to dashboard Cite

show abstract

“…for QPOs; Lee & Miller 1998;Lee, Misra & Taam 2001;Kumar & Misra 2014). Karpouzas et al (2020) explain this for the kHz QPOs in neutron-star LMXBs, and Zhang et al (2020) for the type C QPOs in the BH candidate GRS 1915+105, but the same mechanism could apply for the broad-band component that we discuss here. A similar argument was discussed by Méndez, van der Klis & Ford (2001) for the dependence of the rms amplitude of the khz QPOs in the neutron-star LMXBs 4U 1728-34, 4U 1608-52, and Aql X-1.…”

Section: Anticorrelation Between the Fractional Rms Amplitude And Thementioning

confidence: 55%

X-ray spectral and timing evolution of MAXI J1727–203 with NICER

Alabarta

Altamirano

Méndez

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We present a detailed X-ray spectral and variability study of the full 2018 outburst of MAXI J1727–203 using NICER observations. The outburst lasted approximately four months. Spectral modelling in the 0.3–10 keV band shows the presence of both a soft thermal and a hard Comptonised component. The analysis of these components shows that MAXI J1727–203 evolved through the soft, intermediate and hard spectral states during the outburst. We find that the soft (disc) component was detected throughout almost the entire outburst, with temperatures ranging from ∼0.4 keV, at the moment of maximum luminosity, to ∼0.1 keV near the end of the outburst. The power spectrum in the hard and intermediate states shows broadband noise up to 20 Hz, with no evidence of quasi-periodic oscillations. We also study the rms spectra of the broadband noise at 0.3 − 10 keV of this source. We find that the fractional rms increases with energy in most of the outburst except during the hard state, where the fractional rms remains approximately constant with energy. We also find that, below 3 keV, the fractional rms follows the same trend generally observed at energies >3 keV, a behaviour known from previous studies of black holes and neutron stars. The spectral and timing evolution of MAXI J1727–203, as parametrised by the hardness-intensity, hardness-rms, and rms-intensity diagrams, suggest that the system hosts a black hole, although we could not rule out a neutron star.

show abstract

“…The phase lags at the type-C QPO frequencies have been systematically investigated in Van den Eijnden et al (2017) and Zhang et al (2020), but a similar feature has not been reported. Perhaps this is because those observations were mostly of type-C QPOs in the hard state, while we find that such hard lags are specific to type-C QPOs observed during the relatively short-lived transition and are not seen as clearly in the hard state.…”

Section: Appendix a Lag-frequency Spectra Of Individual Epochsmentioning

confidence: 96%

Disk, Corona, Jet Connection in the Intermediate State of MAXI J1820+070 Revealed by NICER Spectral-timing Analysis

Wang

Mastroserio

Kara

et al. 2021

ApJL

101

View full text Add to dashboard Cite

We analyze five epochs of Neutron star Interior Composition Explorer (NICER) data of the black hole X-ray binary MAXI J1820+070 during the bright hard-to-soft state transition in its 2018 outburst with both reflection spectroscopy and Fourier-resolved timing analysis. We confirm the previous discovery of reverberation lags in the hard state, and find that the frequency range where the (soft) reverberation lag dominates decreases with the reverberation lag amplitude increasing during the transition, suggesting an increasing X-ray emitting region, possibly due to an expanding corona. By jointly fitting the lag-energy spectra in a number of broad frequency ranges with the reverberation model reltrans, we find the increase in reverberation lag is best described by an increase in the X-ray coronal height. This result, along with the finding that the corona contracts in the hard state, suggests a close relationship between spatial extent of the X-ray corona and the radio jet. We find the corona expansion (as probed by reverberation) precedes a radio flare by ∼5 days, which may suggest that the hard-to-soft transition is marked by the corona expanding vertically and launching a jet knot that propagates along the jet stream at relativistic velocities.Unified Astronomy Thesaurus concepts: Low-mass x-ray binary stars (939); Stellar mass black holes (1611); High energy astrophysics (739); Black hole physics (159); X-ray transient sources (1852)

show abstract

A systematic analysis of the phase lags associated with the type-C quasi-periodic oscillation in GRS 1915+105

Cited by 47 publications

References 59 publications

ALMA/NICER observations of GRS 1915+105 indicate a return to a hard state

ALMA/NICER observations of GRS 1915+105 indicate a return to a hard state

X-ray spectral and timing evolution of MAXI J1727–203 with NICER

Disk, Corona, Jet Connection in the Intermediate State of MAXI J1820+070 Revealed by NICER Spectral-timing Analysis

Contact Info

Product

Resources

About