![]() ![]() This paper is the first attempt at estimating the source of X-ray afterglows using this kind of model. For a magnetar-strength field, this process happens on a scale from seconds to days – exactly the duration of most X-ray plateaux. This gap in observations isn’t surprising because the magnetic field of the star converts the rotational energy into electromagnetic energy. All known magnetars have a very slow rotation frequency similarly, all observed neutron stars with millisecond spins have weak magnetic fields. For each short gamma-ray burst, the results suggested that the remnant neutron star is a millisecond magnetar: a neutron star with an extraordinarily powerful magnetic field. ![]() In our study, we borrowed the basic physics from previous short gamma-ray burst models to predict the luminosity and duration of the X-ray plateau. So, if the remnant of a short gamma-ray burst is a neutron star, it must have a similar energy outflow as a supernova remnant. While remnants from short gamma-ray bursts and supernovae have many differences, the energy driving from a rotating neutron star has the same underlying physics. The model we used was inspired by remnants from young supernova. ![]()
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