Radio emission from the unbound debris of tidal disruption events

Yalinewich, Almog; Steinberg, Elad; Piran, Tsvi; Krolik, Julian H.

doi:10.1093/mnras/stz1567

Cited by 37 publications

(45 citation statements)

References 44 publications

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“…Compared to the primary ejecta unbound as an immediate consequence of the disruption (Guillochon et al 2016;Krolik et al 2016;Yalinewich et al 2019), this secondary ejecta has a fraction ≈ f u of the mass, higher velocity ( §4.4), and a larger opening angle ( §4.1). The ejecta drives a bow shock while running into the surrounding medium, and relativistic electrons accelerated in this shock can produce synchrotron radiation (Krolik et al 2016;Yalinewich et al 2019). At later times, the shock driven by the ejecta may mimic a supernova remnant (Guillochon et al 2016).…”

Section: Energeticsmentioning

confidence: 99%

“…The denser medium around AGNs could mean that TDEs are more radio-bright in AGNs than in vacuum. The prompt emission due to the secondary ejecta could be more luminous than the primary ejecta because the fastest material has higher velocity and a wider interaction area (Krolik et al 2016;Yalinewich et al 2019). All these may explain why the radio transient Cygnus A-2 (Perley et al 2017), if interpreted as a thermal TDE happening in an AGN (de Vries et al 2019), is brighter in radio than typical thermal TDEs in vacuum.…”

Section: Energeticsmentioning

confidence: 99%

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Tidal Disruption Events in Active Galactic Nuclei

Chan

Piran

Krolik

et al. 2019

ApJ

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A fraction of tidal disruption events (TDEs) occur in active galactic nuclei (AGNs) whose black holes possess accretion disks; these TDEs can be confused with common AGN flares. The disruption itself is unaffected by the disk, but the evolution of the bound debris stream is modified by its collision with the disk when it returns to pericenter. The outcome of the collision is largely determined by the ratio of the stream mass current to the azimuthal mass current of the disk rotating underneath the stream footprint, which in turn depends on the mass and luminosity of the AGN. To characterize TDEs in AGNs, we simulated a suite of stream-disk collisions with various mass current ratios. The collision excites shocks in the disk, leading to inflow and energy dissipation orders of magnitude above Eddington; however, much of the radiation is trapped in the inflow and advected into the black hole, so the actual bolometric luminosity may be closer to Eddington. The emergent spectrum may not be thermal, TDE-like, or AGN-like. The rapid inflow causes the disk interior to the impact point to be depleted within a fraction of the mass return time. If the stream is heavy enough to penetrate the disk, part of the outgoing material eventually hits the disk again, dissipating its kinetic energy in the second collision; another part becomes unbound, emitting synchrotron radiation as it shocks with surrounding gas.

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Section: Energeticsmentioning

confidence: 99%

Section: Energeticsmentioning

confidence: 99%

Tidal Disruption Events in Active Galactic Nuclei

Chan

Piran

Krolik

et al. 2019

ApJ

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“…The TDE Arp 299-B AT1 was initially detected as a near-infrared transient; radio verylong baseline interferometry (VLBI) resolved a relativistic TDE-driven jet (Mattila et al 2018). More recently, the thermal TDEs ASASSN-14li (Alexander et al 2016;Krolik et al 2016;van Velzen et al 2016;Yalinewich et al 2019) and XMMSL1 J0750-85 (Alexander et al 2017) were found to have radio emission that indicated sub-/nonrelativistic outflows, indicating that these are the first thermal TDEs with detected radio emission. These objects revealed the possibility that all TDEs are accompanied by radio emission, with earlier nondetections (Bower 2011;Bower et al 2013;van Velzen et al 2013;Arcavi et al 2014;Chornock et al 2014) a result of their lower radio luminosities: both ASASSN-14li and XMMSL1 J0750-85 were relatively nearby at z0.02, whereas the median TDE redshift is approximately z∼0.1 (Komossa 2015)-though see Blagorodnova et al (2017) and Saxton et al (2019) for upper limits on the radio luminosities of TDEs that are more than an order of magnitude below that of ASASSN-14li in hosts that are similarly nearby.…”

Section: Introductionmentioning

confidence: 99%

Caltech–NRAO Stripe 82 Survey (CNSS). III. The First Radio-discovered Tidal Disruption Event, CNSS J0019+00

Anderson

Mooley

Hallinan

et al. 2020

ApJ

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We present the discovery of a nuclear transient with the Caltech-NRAO Stripe 82 Survey (CNSS), a dedicated radio transient survey carried out with the Karl G.Jansky Very Large Array (VLA). This transient, CNSS J001947.3+003527, exhibited a turn-on over a timescale of 1 yr, increasing in flux density at 3 GHz from <0.14 mJy in 2014 February to 4.4±0.1 mJy in 2015 March, reaching a peak luminosity of-5 10 erg s Hz 28 1 1 around 2015 October. The association of CNSS J0019+00 with the nucleus (Gaia and our very-long baseline interferometry positions are consistent to within 1 pc) of a nearby S0 Seyfert galaxy at 77 Mpc, together with the radio spectral evolution, implies that this transient is most likely a tidal disruption event (TDE). Our equipartition analysis indicates the presence of a ∼15,000 km s −1 outflow, having energy ∼10 49 erg. We derive the radial density profile for the circumnuclear material in the host galaxy to be proportional to R −2.5. All of these properties suggest resemblance with radio-detected thermal TDEs like ASASSN-14li and XMMSL1 J0740-85. No significant X-ray or optical emission is detected from CNSS J0019+00, although this may simply be due to the thermal emission being weak during our late-time follow-up observations. From the CNSS survey we have obtained the first unbiased measurement of the rate of radio TDEs, R(>500μJy) of about 2×10 −3 deg −2 , or equivalently a volumetric rate of about 10 Gpc −3 yr −1. This rate implies that all-sky radio surveys such as the VLA Sky Survey and those planned with ASKAP, will find many tens of radio TDEs over the next few years.

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“…Another interesting application of moving mesh codes has been done by Yalinewich et al (2019), who simulate the evolution of the unbound debris and the associated radio emission.…”

Section: Moving Mesh Codesmentioning

confidence: 99%

Simulations of Tidal Disruption Events

et al. 2020

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Numerical simulations have historically played a major role in understanding the hydrodynamics of the tidal disruption process. Given the complexity of the geometry of the system, the challenges posed by the problem have indeed stimulated much work on the numerical side. Smoothed Particles Hydrodynamics methods, for example, have seen their very first applications in the context of tidal disruption and still play a major role to this day. Likewise, initial attempts at simulating the evolution of the disrupted star with the so-called affine method have been historically very useful. In this Chapter, we provide an overview of the numerical techniques used in the field and of their limitations, and summarize the work that has been done to simulate numerically the tidal disruption process.

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Radio emission from the unbound debris of tidal disruption events

Cited by 37 publications

References 44 publications

Tidal Disruption Events in Active Galactic Nuclei

Tidal Disruption Events in Active Galactic Nuclei

Caltech–NRAO Stripe 82 Survey (CNSS). III. The First Radio-discovered Tidal Disruption Event, CNSS J0019+00

Simulations of Tidal Disruption Events

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