Fig. 1: Evolution of the spectral  luminosity at 10 keV of Sw 1644+57/GRB 110328A together with GRB 090417B  (red) and other 137 long GRBs (gray) in their rest frames (from Shao et  al. 2011)

(image by FAN Yi Zhong)

Sw 1644+57/GRB  110328A was discovered by the Swift satellite at 2011 March 28 12:57:45  UT. It is coincident with an optical source at redshift . The isotropic  energy of total X-ray and gamma-ray is and the luminosity of the flaring  X-ray afterglow is , both comparable to regular Gamma-Ray Bursts (GRBs)  and establishing its initial name, GRB 110328A. However, the source was  detectable and variable in Burst Alert Telescope (BAT) more than 40  hours after the initial trigger (BAT re-triggered for quite a few  times), with peak brightness in the order of 200 mCrab. Moreover the  flaring X-ray plateau held up to  days. These features are rather  peculiar and have not been reported in any GRBs before, rendering Sw  1644+57 one of the most exciting astrophysical discoveries made in 2011  (see also http://www.nasa.gov/topics/universe/features/star-disintegration.html).

Dr. SHAO Lang   and Zhang Fu Wen , together with Prof. FAN Yi-Zhong and WEI  Da Ming  carried out a timely research on this remarkable cosmological X-ray  outburst. They found out that the early-time (<0.1 day since the  trigger) X-ray emission of Sw 1644+57 resembles some gamma-ray bursts,  say, GRB 090417B. But the late-time flaring X-ray plateau lasting  days  makes it unique (see Fig.1). They examined the possibilities that the  outburst is a super-long GRB powered either by the fallback accretion  onto a nascent black hole or by a millisecond pulsar, and found out that  these two scenarios can address some but not all of the main  observational features. They then focused on the model of tidal  disruption of a (giant) star by a super-massive black hole, in which the  mass of the tidal-disrupted star was estimated to be  a few solar  masses and a simple/straightforward argument for a magnetic origin of  the relativistic outflow had been presented. They then focused on the  model of tidal disruption of a (giant) star by a super-massive black  hole, in which the mass of the tidal-disrupted star was estimated to be  > a few solar masses and a simple/straightforward argument for a  magnetic origin of the relativistic outflow had been presented.  The  central super-massive black hole likely has a mass ~1E6 solar masses  while GRB 090417B-like events plausibly have a typical mass ~ a few -  tens solar masses. The similarity between the early (t<0.1 day) X-ray  emission of Sw 1644+57 and that of GRB 090417B strongly suggests that  very different central engines can produce rather similar X-ray  outbursts in a selected time interval, possibly via the same kind of  initial energy-extraction and late-time-energy-dissipation processes.  The work by SHAO Lang, ZHANG Fu Wen, FAN Yi Zhong (corresponding author)  and WEI  Da Ming, accepted by The Astrophysical Journal Letters (ApJL.)  in 3 weeks, has been published online  (http://iopscience.iop.org/2041-8205/734/2/L33).