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We report the discovery of a Tidal Disruption Event (TDE) candidate occurring in the Active Galactic Nucleus SDSS J022700.77-042020.6. A sudden increase in flux of J0227-0420 during the second half of 2009 is clearly shown in the long-term optical, UV, and NIR light curves. A plateau phase, following an initial decline, is seen in the NUV and optical u, g, r, i light curves. Moreover, we find possible evidence that the plateau phase in the NUV band may lag behind the optical ones by approximately 70-80 days with also a much shorter duration, i.e. $\sim$7-15 days against $\sim$40-50 days. The long-term NUV/optical (after the plateau phase), NIR and MIR light curves can be well characterized with a form of $L(t)\propto t^{-\beta}$, consistent with the expectation of a TDE. The plateaus can be explained if the stellar streams collide with the pre-existing AGN disk at different radii. Though the overall fallback rate decreases, the material in the outer disk gradually drifts inward and increases the local accretion rate at the inner region, producing the optical and UV plateaus. The possible lag between the optical and NUV plateaus can then be attributed to viscosity delay. The index $\beta$ of the NIR $J, H, K_s$ bands ($\sim1.4-3.3$) is steeper than that of the UV/optical ($\sim0.7-1.3$) and MIR bands ($\sim0.9-1.8$), which may suggest that a certain fraction of the dust in the inner region of the dusty torus may be sublimated during the TDE phase. Our results indicate that, due to collisions between stellar debris and pre-existing disk, the light curves of TDEs occurring in AGN may show distinctive features, which may shed new light on the accretion process., Comment: 15 pages, 7 figures, submitted to ApJ after minor revision

We present and analyze the optical/UV and X-ray observations of a nearby tidal disruption event (TDE) candidate AT2019azh, spanning from $\sim$ 30 d before to $\sim$ 400 d after its early optical peak. The X-rays show a late brightening by a factor of $\sim$ 30-100 around 200 days after discovery, while the UV/opticals continuously decayed. The early X-rays show two flaring episodes of variation, temporally uncorrelated with the early UV/opticals. We found a clear sign of X-ray hardness evolution, i.e., the source is harder at early times, and becomes softer as it brightens later. The drastically different temporal behaviors in X-rays and UV/opticals suggest that the two bands are physically distinct emission components, and probably arise from different locations. These properties argue against the reprocessing of X-rays by any outflow as the origin of the UV/optical peak. The full data are best explained by a two-process scenario, in which the UV/optical peak is produced by the debris stream-stream collisions during the circularization phase; some shocked gas with low angular momentum forms an early, low-mass 'precursor' accretion disk which emits the early X-rays. The major body of the disk is formed after the circularization finishes, whose enhanced accretion rate produces the late X-ray brightening. AT2019azh is a strong case of TDE whose emission signatures of stream-stream collision and delayed accretion are both identified., Comment: 20 pages, 11 figures, 6 tables. Accepted for publication on ApJ

Recently two fast X-ray transients (XT1 and XT2) have been reported from the search in the Chandra Deep Field (CDF) data. Each transient shows an initial plateau lasting around hundreds to thousands seconds followed by a rapid decay in the light curve. In particular, CDF-S XT2 is found to be associated with a galaxy at redshift z= 0.738 and was explained as a counterpart of a binary neutron-star merger event. In this paper, motivated by the short duration and decay slopes of the two transients, we consider an alternative interpretation in which both events are accretion-driven flares from tidal disruption of white dwarfs by intermediate-mass black holes. We derive a theoretical model of the accretion rate history, and find that it fits the observed X-ray light curves well. The extremely super-Eddington peak luminosity of XT2 can be explained by the beaming effect of the system, likely in the form of a jet., Comment: 8 pages, 3 figures, 1 table. Accepted for publication in APJL

A multi-messenger, black hole (BH) - neutron star (NS) merger event still remains to be detected. The tidal (dynamical) ejecta from such an event, thought to produce a kinonova, is concentrated in the equatorial plane and occupies only part of the whole azimuthal angle. In addition, recent simulations suggest that the outflow or wind from the post-merger remnant disk, presumably anisotropic, can be a major ejecta component responsible for a kilonova. For any ejecta whose photosphere shape deviates from the spherical symmetry, the electron scattering at the photosphere causes a net polarization in the kilonova light. Recent observational and theoretical polarization studies have been focused to the NS-NS merger kilonova AT2017gfo. We extend those work to the case of a BH-NS merger kilonova. We show that the degree of polarization at the first $\sim 1$ hr can be up to $\sim$ 3\% if a small amount ($10^{-4} M_{\odot}$) of free neutrons have survived in the fastest component of the dynamical ejecta, whose beta-decay causes a precursor in the kilonova light. The polarization degree can be $\sim$ 0.6\% if free neutrons survived in the fastest component of the disk wind. Future polarization detection of a kilonova will constrain the morphology and composition of the dominant ejecta component, therefore help to identify the nature of the merger., Comment: 10 pages, 5 figures. Accepted for publication in ApJ

Two X-ray sources were recently discovered by Irwin et al. in compact companions to elliptical galaxies to show ultra-luminous flares with fast rise (~ minute) and decay (~ hour), and with a peak luminosity ~10^{40-41} erg/s. Together with two other sources found earlier, they constitute a new type of fast transients which cannot be attributed to neutron stars but might be due to intermediate-mass black holes (IMBHs; 10^{2-4} M_sun). The flaring behavior is recurrent for at least two sources. If the flare represents a short period of accretion onto an IMBH during the periastron passage of a donor star on an eccentric (i.e., repeating) or parabolic (non-repeating) orbit, we argue that the flare's rise time corresponds to the duration during which the donor's tidally stripped mass joins a residual disk at the pericenter. This duration is in turn equal to three other time scales: the duration of stripping, the sound crossing time of the donor, and the circular orbit time at the pericenter radius. Only a white dwarf can have a sound crossing time as short as one minute. Therefore, the donor must be a white dwarf and it was stripped of ~10^{-10} M_sun upon each passage at several to tens of Schwarzschild radii from the IMBH. The flux decay corresponds to the viscous drainage of the supplied mass toward the hole. Aided with long-term X-ray monitoring, this type of fast transients would be an ideal target for next-generation gravitational wave detectors., Comment: 7 pages, 2 figures, 1 appendix. ApJL accepted. UXB sample reduced to 4 sources

According to the traditional scenario for core-collapse supernovae, the core of the collapsing star forms a neutron star and its gravitational energy release sends out a shockwave into the stellar envelope. However, in a significant number of numerical simulations, the shock stalls and the star cannot be exploded successfully, especially for a massive, compact star. We consider an alternative scenario that with mass fallback, the collapsing star forms a black hole in the center, surrounded by a dense, hot accretion disk, which blows out an intense outflow (wind). The kinetic energy of the wind may result in a successful stellar explosion. With an improved version of the formulism in Kohri et al. (2005) who studied neutron star accretion of minor fallback, we study this disk wind-driven explosion by calculating the accretion history for a suite of pre-SN stellar models with different initial surface rotational velocities, masses and metallicities, and by comparing the disk wind energy with the binding energy of the infalling stellar envelope. We show that the most promising models to be exploded successfully by this new channel are those relatively compact pre-SN stars with relatively low metallicities and not too low specific angular momenta. The total energies of the explosions are $\sim 10^{51-52}$ergs, and a more massive progenitor may produce a more energetic explosion., Comment: 11 pages, 8 figures, 3 tables, the Astrophysical Journal accepted

There has been suggestive evidence of intermediate-mass black holes (IMBHs; 10^{3-5} M_sun) existing in some globular clusters (GCs) and dwarf galaxies, but IMBHs as a population remain elusive. As a main-sequence star passes too close by an IMBH it might be tidally captured and disrupted. We study the long-term accretion and observational consequence of such tidal disruption events. The disruption radius is hundreds to thousands of the BH's Schwarzschild radius, so the circularization of the falling-back debris stream is very inefficient due to weak general relativity effects. Due to this and a high mass fallback rate, the bound debris initially goes through a ~10 yr long super-Eddington accretion phase. The photospheric emission of the outflow ejected during this phase dominates the observable radiation and peaks in the UV/optical bands with a luminosity of 10^42 erg/s. After the accretion rate drops below the Eddington rate, the bolometric luminosity follows the conventional t^{-5/3} power-law decay, and X-rays from the inner accretion disk start to be seen. Modeling the newly reported IMBH tidal disruption event candidate 3XMM J2150-0551, we find a general consistency between the data and predictions. The search for these luminous, long-term events in GCs and nearby dwarf galaxies could unveil the IMBH population., Comment: 8 pages, 11 figures, published in the Astrophysical Journal

The angular distribution of GRB jets is not yet clear. The observed luminosity of GRB 170817A is the lowest among all known short GRBs, which is best explained by the fact that our line of sight is outside of the jet opening angle, $\theta_{obs}$ $>$ $\theta_j$, where $\theta_{obs}$ is the angle between our line of sight and jet axis. Inferred by gravitational wave observations, as well as radio and X-ray afterglow modeling of GRB 170817A, it is likely that $\theta_{obs}$ $\sim$ 20$^{\circ}$ -- 28$^{\circ}$. In this work, we quantitatively consider two scenarios of angular energy distribution of GRB ejecta: top-hat jet, and structured jet with a power law index $s$. For top-hat jet model, we get a large $\theta_j$ (e.g., $\theta_{j}$$>$$10^{\circ}$), a rather high local (i.e., z$<$0.01) short GRB rate $\sim$8--15$\times10^3$ $Gpc^{-3}$$yr^{-1}$ (estimated 90$\sim$1850 $ Gpc^{-3}$$yr^{-1}$ in Fong et al. 2015) and an extremely high $E_{peak,0}$(on-axis,rest-frame)$>$7.5$\times10^4$keV($\sim$500keV for typical short GRB). For structured jet model, we use $\theta_{obs}$ to give limits on $s$ and $\theta_{j}$ for a typical on-axis luminosity short GRB (e.g., $10^{49}$ erg s$^{-1}$$\sim$$10^{51}$ erg s$^{-1}$), and a low on-axis luminosity case (e.g., $10^{49}$ erg s$^{-1}$) gives more reasonable values of $s$. A structured jet model is more feasible for GRB 170817A than a top-hat jet model, due to the rather high local short GRB rate and the extremely high on-axis $E_{peak,0}$ almost rules out the top-hat jet model. GRB 170817A is likely a low on-axis luminosity GRB ($10^{49}$ erg s$^{-1}$) with a structured jet., Comment: 10 Pages, 3 Figures, 1 Table, RAA, in press