Milli-Hertz Gravitational-wave Background Produced by Quasiperiodic Eruptions

Xian, Chen; Qiu, Yu; Li, Shuo; Liu, F. K.

doi:10.3847/1538-4357/ac63bf

Cited by 28 publications

(20 citation statements)

References 48 publications

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“…Most other QPE models invoke the interaction between a stellar-like body and the SMBH (or SMBH plus accretion flow) identifying the QPE quasi-periodicity with the orbital period of the stellar companion. The proposed models can be roughly separated into two classes in which QPEs are either due to collisions between the stellar companion and the accretion flow in a nearly circular orbit (Xian et al 2021), or to episodic mass transfer events at each pericenter passage in a mildly or highly eccentric orbit (King 2020;Chen et al 2022;King 2022;Wang et al 2022;Zhao et al 2022;Krolik & Linial 2022;Lu & Quataert 2022). Below we discuss, with no ambition of completeness, some of the most relevant aspects of the two classes of proposed models in comparison with the rich phenomenology of GSN 069.…”

Section: Constraints On the Qpe Emission Mechanismmentioning

confidence: 99%

“…Several theoretical models have been considered to explain the QPE phenomenon. Proposed scenarios include (i) modified disc instability models (Sniegowska et al 2020;Raj & Nixon 2021;Pan et al 2022;Kaur et al 2022); (ii) gravitational lensing in a nearly equal-mass supermassive black hole (SMBH) binary (Ingram et al 2021); (iii) mass transfer from one or more orbiting bodies in a variety of different configurations as discussed by King (2020King ( , 2022, Chen et al (2022), Metzger et al (2022), Zhao et al (2022), Wang et al (2022), Krolik & Linial (2022), and Lu & Quataert (2022);or (iv) collisions between an orbiting secondary body and the accretion disc that is formed following the initial TDE (Suková et al 2021;Xian et al 2021). Most proposed models focus on QPEs ignoring the long-term evolution of the quiescent level emission which is particularly well monitored in GSN 069.…”

Section: Introductionmentioning

confidence: 99%

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Repeating tidal disruptions in GSN 069: Long-term evolution and constraints on quasi-periodic eruptions’ models

Miniutti¹,

Giustini²,

Arcodia³

et al. 2023

A&A

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Context. GSN 069 is the first galactic nucleus where quasi-periodic eruptions (QPEs) have been identified in December 2018. These are high-amplitude, soft X-ray bursts recurring every ∼ 9 hr, lasting ∼ 1 hr, and during which the X-ray count rate increases by up to two orders of magnitude with respect to an otherwise stable quiescent level. The X-ray spectral properties and the long-term evolution of GSN 069 in the first few years since its first X-ray detection in 2010 are consistent with a long-lived tidal disruption event (TDE). Aims. We aim to derive the properties of QPEs and of the long-term X-ray evolution in GSN 069 over the past 12 yr. Methods. We analyse timing and spectral X-ray data from 11 XMM-Newton, one Chandra, and 34 Swift observations of GSN 069 on timescales ranging from minutes to years. Results. QPEs in GSN 069 are a transient phenomenon with a lifetime of 1.05 yr. The QPE intensity and recurrence time oscillate and allow for alternating strong-weak QPEs and long-short recurrence times to be defined. In observations with QPEs, the quiescent level exhibits a quasi-periodic oscillation with a period equal to the average separation between consecutive QPEs. The QPE spectral evolution is consistent with thermal emission from a very compact region that heats up quickly and subsequently cools down via X-ray emission while expanding by a factor of ∼ 3 in radius. The long-term evolution of the quiescent level is characterised by two repeating TDEs ∼ 9 yr apart. We detect a precursor X-ray flare prior to the second TDE that may be associated with the circularisation phase during disc formation. A similar precursor flare is tentatively detected just before the first TDE. Conclusions. We provide a comprehensive summary of observational results that can be used to inform further theoretical and numerical studies on the origin of QPEs in GSN 069 and we discuss our results in terms of currently proposed QPE models. Future X-ray observations of GSN 069 promise that the QPE origin and the relation between QPEs and repeating TDEs in this galactic nucleus will be constrained, with consequences for the other sources where QPEs have been identified.

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Section: Constraints On the Qpe Emission Mechanismmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Repeating tidal disruptions in GSN 069: Long-term evolution and constraints on quasi-periodic eruptions’ models

Miniutti¹,

Giustini²,

Arcodia³

et al. 2023

A&A

View full text Add to dashboard Cite

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“…, where Δf is the increment of frequency during the observational period (Barack & Cutler 2004;Bonetti & Sesana 2020;Chen et al 2022). The total effective strain h eff can be calculated by…”

Section: Discussionmentioning

confidence: 99%

“…EMRIs are important targets for future space-borne detectors (e.g., Amaro-Seoane et al 2007;Han & Fan 2018;Chen & Han 2018;Chen et al 2022) such as LISA, TianQin, and Taiji (e.g., Luo et al 2016;Robson et al 2019). In a recent work, Chen et al (2022) estimated the effective strain for these QPEs sources, and they found that the GW from these several QPE sources cannot be detected by the above proposed space-born GW detectors. Here, we simply estimate the possible detection distance for the EMRIs as expected in QPE sources.…”

Section: Possibility Of Space-borne Gw Detectionmentioning

confidence: 99%

“…The MBH-WD EMRI in our model has a highly eccentric orbit so that the GW radiation is spread into a wide range of harmonic frequencies (e.g., Peters & Mathews 1963;Finn & Thorne 2000;Barack & Cutler 2004). The characteristic strain h c,n of the nth harmonic component, which corresponds to the frequency n/T (T is the orbital period, Finn & Thorne 2000; Barack & Cutler 2004;Bonetti & Sesana 2020;Chen et al 2022)…”

Section: Possibility Of Space-borne Gw Detectionmentioning

confidence: 99%

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A Model for the Possible Connection Between a Tidal Disruption Event and Quasi-periodic Eruption in GSN 069

Wang¹,

Yin²,

Ma³

et al. 2022

ApJ

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Quasi-periodic eruptions (QPEs) are found in the center of five galaxies, where a tidal disruption event (TDE)-like event has been reported in GSN 069, which occurred a couple of years before the QPEs. We explain the connection of these phenomena based on a model of a highly eccentric white dwarf (WD) 104−6 M ⊙ massive black hole (MBH) binary formed by the Hill mechanism. In this system, the tidally induced internal oscillation of a WD can heat the WD envelope thereby inducing tidal nova and inflating the WD envelope, which can be captured by the MBH and form a TDE. The tidal stripping of the surviving WD in the eccentric orbit can produce QPEs. We also apply this model to the other four QPE sources. Based on the estimated fallback rate, we find that the remaining time after the QPE-observed time for these QPEs is only around 1–2 yr based on our simple model estimation, after which the WD will be fully disrupted. We also show that the accretion rate can be much higher than the Eddington accretion rate in the final stage of these QPE sources. The peak frequency of the spectral energy distribution of the disk stays in the soft X-ray band (∼0.1–1 keV), which is consistent with observational results.

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The complex time and energy evolution of quasi-periodic eruptions in eRO-QPE1

Arcodia

Miniutti

Ponti

et al. 2022

A&A

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Quasi-periodic eruptions (QPEs) are recurrent X-ray bursts found so far in the nuclei of low-mass galaxies. Their trigger mechanism is still unknown, but recent models involving one or two stellar-mass companions around the central massive (≈ 10 5 − 10 6 M ) black hole have gathered significant attention. While these have been compared only qualitatively with observations, the phenomenology of QPEs is developing at a fast pace, with the potential to reveal new insights. Here we report two new observational results found in eRO-QPE1, the brightest QPE source discovered so far: i) the eruptions in eRO-QPE1 occur sometimes as single isolated bursts, and at others as chaotic mixtures of multiple overlapping bursts with very different amplitudes; ii) we confirm that QPEs peak at later times and are broader at lower energies, with respect to higher energies while, for the first time, we find that QPEs also start earlier at lower energies. Furthermore, eruptions appear to undergo an anti-clockwise hysteresis cycle in a plane of hardness ratio versus total count rate. Behavior i) was not found before in any other QPE source and implies that if a common trigger mechanism is in place for all QPEs, it must be able to produce both types of timing properties, regular and complex. Result ii) implies that the X-ray emitting component does not have an achromatic evolution even during the start of QPEs, and that the rise is harder than the decay at a given total count rate. This specific energy dependence could be qualitatively compatible with inward radial propagation during the rise within a compact accretion flow, the presence of which is suggested by the stable quiescence spectrum observed in general for QPE sources.right panel of Fig. 2). It is loosely based on that proposed in Norris et al. (2005) for gamma-ray bursts, and defined as:which is evaluated at zero for times smaller than the asymptote at t peak − t as , where t as = √ τ 1 τ 2 . Whereas A is the amplitude at the peak and λ = e t λ a normalization to join rise and decay, Article number, page 2 of 11 R. Arcodia et al.: Evolution of quasi-periodic eruptions in eRO-QPE1

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Milli-Hertz Gravitational-wave Background Produced by Quasiperiodic Eruptions

Cited by 28 publications

References 48 publications

Repeating tidal disruptions in GSN 069: Long-term evolution and constraints on quasi-periodic eruptions’ models

Repeating tidal disruptions in GSN 069: Long-term evolution and constraints on quasi-periodic eruptions’ models

A Model for the Possible Connection Between a Tidal Disruption Event and Quasi-periodic Eruption in GSN 069

The complex time and energy evolution of quasi-periodic eruptions in eRO-QPE1

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