Conveners
Slowly rotating pulsars: Tuesday block 1
- Alice Borghese (INAF/Astronomical Observatory of Rome)
- Francesco Coti Zelati
Slowly rotating pulsars: Tuesday block 2
- Alice Borghese (INAF/Astronomical Observatory of Rome)
- Francesco Coti Zelati
Description
Over the past few years, sky surveys using a variety of radio instruments have led to the discovery of pulsating sources with much longer periods than those measured for the bulk of radio pulsars, placing them in an unexplored area of the spin period - spin period derivative diagram for pulsars. While some of these sources have been identified as slowly rotating neutron stars, the nature of other sources remains debated. This session aims to bring together observers and theoreticians to present and discuss the latest observational discoveries, the state-of-the-art modeling, evolutionary scenarios of these peculiar objects, and future prospects for this increasingly interesting field in pulsar research.
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Kaustubh Rajwade (University of Oxford)09/07/2024, 15:00Slowly rotating pulsarsInvited talk in a parallel session
Ultra-long period (ULP) radio transients are one of the most recent mysteries in compact object astrophysics. Theories suggest that these could be slowly spinning neutron stars or white dwarfs. However, the confirmation of either (or both) would be a giant leap toward understanding the evolution of compact objects and the physics of coherent radio emission. This has led to large-scale...
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Alex Cooper (University of Oxford)09/07/2024, 15:25Slowly rotating pulsarsInvited talk in a parallel session
The nature of recently discovered ultra-long period radio transients is uncertain. If these sources are neutron stars, their long periods strongly challenge rotation-powered emission models. In this talk, I will present a new model of radio emission from ultra-long period magnetars, in which crustal stresses power magnetospheric twists, which dissipate to produce coherent radio emission. I...
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Zorawar Wadiasingh (University of Maryland College Park / NASA GSFC)09/07/2024, 15:50Slowly rotating pulsarsInvited talk in a parallel session
In this talk I will make the case that ultra-long period radio pulsars are magnetically powered neutron stars, or magnetars in the broadest sense of the term. Although they appear very different observationally from X-ray magnetars, I will argue they host strong magnetar-like fields. This will encompass arguments from many directions, including source densities, energetics, the physics of how...
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Dr Ali Arda Gençali (Sabancı University)09/07/2024, 16:15Slowly rotating pulsarsTalk in a parallel session
Recently discovered long-period pulsars (LPPs), namely PSR J0901–4046 (76 s), GLEAM-X J162759.5–523504.3 (1091 s), and GPM J1839–10 (1318 s), have rotational periods much longer than those of radio pulsars and other isolated neutron star populations. LPPs exhibit transient pulsed-radio epochs with unusual and variable pulse shapes, similar to the radio behaviors of rotating radio transients...
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Michela Rigoselli (INAF)09/07/2024, 17:00Slowly rotating pulsarsTalk in a parallel session
The X-ray spectra of isolated neutron stars (INSs) typically include a thermal component, that comes from the cooling surface, and a non-thermal component, produced by highly-relativistic particles accelerated in the stellar magnetosphere. Hot spots from returning currents can also be detected.
Middle-aged pulsars exhibit a mixture of these components, but other flavours of INSs, that show...
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Banibrata Mukhopadhyay (Indian Institute of Science)09/07/2024, 17:15Slowly rotating pulsarsTalk in a parallel session
The radio pulsar PSR J0901-4046 exhibits very slow rotation with a spin period
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76 s, which is unusually low for a neutron star. Typically the spin period of
radio pulsars ranges 1.4 ms to 23.5 s, when they are divided into various
sub-classes, e.g. transient, millisecond pulsar, magnetar. The question
arises, is PSR J0901-4046 really a neutron star? In fact, the spin period
76 s more... -
Alice Borghese (INAF/Astronomical Observatory of Rome)09/07/2024, 17:30Slowly rotating pulsarsTalk in a parallel session
1E 161348-5055 (1E 1613), the source at the center of the supernova remnant RCW103, has defied any easy classification since its discovery, owing to its long-term variability from months to years and a periodicity of 6.67 hr with a variable light curve profile across different flux levels. On June 2016, 1E 1613 emitted a magnetar-like millisecond burst of hard X-rays, accompanied with a factor...
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Nicholas O'Neill (The University of Melbourne)09/07/2024, 17:45Slowly rotating pulsarsTalk in a parallel session
Pulsar timing noise is the stochastic deviation of the pulse arrival times of a pulsar away from their long term trend. In the standard two-component crust-superfluid neutron star model, timing noise can be explained as the perturbation of the two components by irregular torques. Interactions between the crust and superfluid cause these perturbations to decay exponentially with a...
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