(2017 gravitational wave detection from a neutron star merger)
GW170817 was a GW detection by LIGO and Virgo
for which a corresponding gamma-ray burst (GRB) was detected
(a short burst, or SGRB, occurring 1.7 seconds later, GRB 170817A),
and for which the source was found through checking
for transients within the region of the celestial sphere
(e.g., with the Víctor M. Blanco Telescope DECam)
that was indicated through triangulation from the three detectors.
As such, it the first case of a
new type of multi-messenger astronomy,
observation via EMR as well as other media.
Virgo's detection was weak (i.e., a low signal-to-noise ratio) and
the fact that detector sensitivity depends upon the direction
of the source was a factor in reducing the region of the sky
The source was in the galaxy, NGC 4993.
The event has been interpreted as a neutron star merger due to the
pattern of gravitational waves (the signal detected lasts longer because
the lower mass of neutron stars results in a slower orbital decay).
It is observationally a transient somewhat like a supernova (SN),
but showing less EMR-power and a different subsequent
evolution, falling under the class of kilonova (a SN-like
transient but with less power). The event has been the subject of
much study, being the first such observation in which the underlying
event is so certain. Among the revelations:
The r-process is expected since the shock of impact sends neutrons
flying free, and is detected through the EMR produced by hot elements,
heated for a while by
radioactivity (e.g., beta decay), all consistent
with the products of r-process nucleosynthesis. Among the effects
is high opacity soon after the merger, due to the presence of
elements heavier than iron.
Early EMR observation was to a degree indistinct,
which is attributed to the effects of relativistic speed of ejected material.
Interpretation suggests the two neutron stars first merged
into a hypermassive neutron star (HMNS), and about a second later, collapsed into a black hole.
Given the scenario most likely to form a binary neutron star, the decay of its
orbit would take a very long time, and estimates are that this
system's orbit decayed over 11 gigayears leading up to the merger.
(gravitational waves,event,gamma rays,neutron stars,transient)
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Referenced by pages:
gamma-ray burst (GRB)
gravitational wave (GW)
GW detection (GW)
hypermassive neutron star (HMNS)
neutron star merger
Swope Supernova Survey (SSS)