The Structure and Signals of Neutron Stars, from Birth to Death

Session

Afternoon session - Parallel A

26 Mar 2014, 15:15

Conveners

Afternoon session - Parallel A

• Jorge Horvath (IAG-USP)

78. The effects of a neutron star translational and rotational motion in observable timing and evolution of radiopulsars

Anton Biryukov

26/03/2014, 15:15

The instant observed period of an isolated radiopulsar is accepted to be identical to the physical period of a neutron star rotation except for the cases of obvious strong precession. However, in the strict sense, the time interval between two successive pulses received by an observer is nothing else than the interval between successive passes of the observer through rotating pulsar beam....

40. The glitch activity of the Crab pulsar

Cristobal Espinoza (P)

26/03/2014, 15:35

The rotation of the Crab pulsar has been regularly monitored at Jodrell Bank Observatory and other observatories for 44 years. Like most pulsars, its regular spindown is occasionally interrupted by sudden spin-up events known as glitches. Glitches are thought to be the response of a dense internal neutron superfluid to the pulsar's spindown. Here we report on a detailed study of the...

3. Nuclear equation of state from observations of short gamma-ray burst remnants

Dr Paul Lasky (School of Physics, melbourne University)

26/03/2014, 15:55

The favoured progenitor model for short gamma-ray bursts (SGRBs) is the merger of two neutron stars that triggers an explosion with a burst of collimated gamma-rays. Following the initial prompt emission, some SGRBs exhibit a plateau phase in their X-ray light curves that indicates additional energy injection from a central engine, believed to be a rapidly rotating, highly magnetised neutron...

103. GRB 130831A: The Birth and Death of a Magnetar at z=0.5

Dr M. De Pasquale (Mullard Space Science Laboratory - University College London)

26/03/2014, 16:15

We present observations of GRB 130831A obtained by Swift, Chandra, and multiple ground-based observatories. This burst shows a remarkable drop in the X-ray light curve at about 10^5 s after the trigger, with a decay slope of \alpha_X \simeq 5. Such behaviour cannot be explained in the standard Forward Shock (FS) model, whereas it can be explained if the high energy emission is powered by a...