Towards a theory of extremely intermittent pulsars

Mottez, Fabrice; Bonazzola, S.; Heyvaerts, J.

doi:10.1051/0004-6361/201321182

Cited by 12 publications

(3 citation statements)

References 33 publications

(56 reference statements)

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“…PSR B1931+24 was the first intermittent pulsar discovered; it is known to show normal pulsar behaviour for 5 − 10 days, and then undergo extreme nulling events for 25 − 35 days, making it undetectable (Kramer et al 2006). The possibility that this observed QP behaviour is due to a binary companion of B1931+24 has been studied by Rea et al (2008) and Mottez et al (2013); both concluded that the influence of a companion would not be enough to account for all the properties of the intermittent signal.…”

Section: B1931+24mentioning

confidence: 99%

A search for planetary companions around 800 pulsars from the Jodrell Bank pulsar timing programme

Niţu,

Keith,

Stappers

et al. 2022

Preprint

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We have searched for planetary companions around 800 pulsars monitored at the Jodrell Bank Observatory, with both circular and eccentric orbits of periods between 20 days and 17 years and inclination-dependent planetary masses from 10 −4 to 100 M ⊕ . Using a Bayesian framework, we simultaneously model pulsar timing parameters and a stationary noise process with a power-law power spectral density. We put limits on the projected masses of any planetary companions, which reach as low as 1/100th of the mass of the Moon (∼ 10 −4 M ⊕ ). We find that two-thirds of our pulsars are highly unlikely to host any companions above 2 − 8 M ⊕ . Our results imply that fewer than 0.5% of pulsars could host terrestrial planets as large as those known to orbit PSR B1257+12 (∼ 4 M ⊕ ); however, the smaller planet in this system (∼ 0.02 M ⊕ ) would be undetectable in 95% of our sample, hidden by both instrumental and intrinsic noise processes, although it is not clear if such tiny planets could exist in isolation. We detect significant periodicities in 15 pulsars, however we find that intrinsic quasi-periodic magnetospheric effects can mimic the influence of a planet, and for the majority of these cases we believe this to be the origin of the detected periodicity. Notably, we find that the highly periodic oscillations in PSR B0144+59 are correlated with changes in the pulse profile and therefore can be attributed to magnetospheric effects. We believe the most plausible candidate for planetary companions in our sample is PSR J2007+3120.

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Section: B1931+24mentioning

confidence: 99%

A search for planetary companions around 800 pulsars from the Jodrell Bank pulsar timing programme

Niţu,

Keith,

Stappers

et al. 2022

Preprint

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“…The first discovery of earth-mass exoplanets was indeed around a millisecond pulsar (Wolszczan & Frail 1992). The existence of asteroid belts around millisecond pulsars has been invoked to explain various timing variations and other observational features Shannon et al 2013;Brook 2014;Yu & Huang 2016;Mottez et al 2013a).…”

Section: Introductionmentioning

confidence: 99%

Fast radio burst repeaters produced via Kozai-Lidov feeding of neutron stars in binary systems

Kotera

Silk

2021

A&A

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Neutron stars are likely surrounded by gas, debris, and asteroid belts. Kozai-Lidov perturbations, induced by a distant, but gravitationally bound companion, can trigger the infall of such orbiting bodies onto a central compact object. These effects could lead to the emission of fast radio bursts (FRBs), for example by asteroid-induced magnetic wake fields in the wind of the compact object. A few percent of binary neutron star systems in the Universe, such as neutron star-main sequence star, neutron star-white dwarf, double neutron star, and neutron star-black hole systems, can account for the observed non-repeating FRB rates. More remarkably, we find that wide and close companion orbits lead to non-repeating and repeating sources, respectively, and they allow for one to compute a ratio between repeating and non-repeating sources of a few percent, which is in close agreement with the observations. Three major predictions can be made from our scenario, which can be tested in the coming years: (1) most repeaters should stop repeating after a period between 10 years to a few decades, as their asteroid belts become depleted; (2) some non-repeaters could occasionally repeat, if we hit the short period tail of the FRB period distribution; and (3) series of sub-Jansky level short radio bursts could be observed as electromagnetic counterparts of the mergers of binary neutron star systems.

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“…The first discovery of earth-mass exoplanets was indeed around a millisecond pulsar (Wolszczan & Frail 1992a). The existence of asteroid belts around millisecond pulsars has been invoked to explain various timing variations and other observational features (Cordes & Shannon 2008;Shannon et al 2013;Brook et al 2014;Yu & Huang 2016;Mottez et al 2013a).…”

Section: Introductionmentioning

confidence: 99%

Fast radio burst repeaters produced via Kozai-Lidov feeding of neutron stars in binary systems

Decoene,

Kotera,

Silk

2020

Preprint

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Neutron stars are likely surrounded by gas, debris, and asteroid belts. Kozai-Lidov perturbations, induced by a distant, but gravitationally bound companion, can trigger the infall of such orbiting bodies onto a central compact object. These effects could lead to the emission of fast radio bursts (FRBs), for example by asteroid-induced magnetic wake fields in the wind of the compact object. A few percent of binary neutron star systems in the Universe, such as neutron starmain sequence star, neutron star-white dwarf, double neutron star, and neutron star-black hole systems, can account for the observed non-repeating FRB rates. More remarkably, we find that wide and close companion orbits lead to non-repeating and repeating sources, respectively, and they allow for one to compute a ratio between repeating and non-repeating sources of a few percent, which is in close agreement with the observations. Three major predictions can be made from our scenario, which can be tested in the coming years: 1) most repeaters should stop repeating after a period between 10 years to a few decades, as their asteroid belts become depleted; 2) some non-repeaters could occasionally repeat, if we hit the short period tail of the FRB period distribution; and 3) series of sub-Jansky level short radio bursts could be observed as electromagnetic counterparts of the mergers of binary neutron star systems.

show abstract

Towards a theory of extremely intermittent pulsars

Cited by 12 publications

References 33 publications

A search for planetary companions around 800 pulsars from the Jodrell Bank pulsar timing programme

A search for planetary companions around 800 pulsars from the Jodrell Bank pulsar timing programme

Fast radio burst repeaters produced via Kozai-Lidov feeding of neutron stars in binary systems

Fast radio burst repeaters produced via Kozai-Lidov feeding of neutron stars in binary systems

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