Radio Efficiency of Pulsars

Szary, Andrzej; Zhang, Bing; Melikidze, George I.; Gil, Janusz; Xu, R. X.

doi:10.1088/0004-637x/784/1/59

Cited by 72 publications

(81 citation statements)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our best-fit model FDM-20 that showed the closest match to the observed catalogued radio DNSs had the following pulsar parameters: a) Uniform birth magnetic field distribution (10 10 -10 13 G); b) Uniform birth spin period distribution (10-100 ms); c) Magnetic field decay time-scale (1000 Myrs); d) Magnetic field decay mass-scale (0.02 M ); e) CE mass accretion following MacLeod & Ramirez-Ruiz (2015); f) A lognormal pulsar luminosity function following Szary et al (2014).…”

Section: Discussionmentioning

confidence: 99%

“…However, there are radio pulsars observed beyond the empirical death lines (Young et al 1999). In addition, rejecting pulsars in our simulations once they cross the death lines leads to a pile up at the death line boundary, which is not observed (Szary et al 2014). We hence use a 'hybrid' approach in determining radio pulsar death, described as follows.…”

Section: Pulsar Deathmentioning

confidence: 99%

See 1 more Smart Citation

Modelling double neutron stars: radio and gravitational waves

Chattopadhyay

Stevenson

Hurley

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We have implemented prescriptions for modelling pulsars in the rapid binary population synthesis code COMPAS. We perform a detailed analysis of the double neutron star (DNS) population, accounting for radio survey selection effects. The surface magnetic field decay timescale (≈1000 Myr) and mass scale (≈0.02 M ) are the dominant uncertainties in our model. Mass accretion during common envelope evolution plays a non-trivial role in recycling pulsars. We find a best-fit model that is in broad agreement with the observed Galactic DNS population. Though the pulsar parameters (period and period derivative) are strongly biased by radio selection effects, the observed orbital parameters (orbital period and eccentricity) closely represent the intrinsic distributions. The number of radio observable DNSs in the Milky Way at present is ≈ 2500 in our model, only ≈ 10% of the predicted total number of DNSs in the galaxy. Using our model calibrated to the Galactic DNS population, we make predictions for DNS mergers observed in gravitational waves. The DNS chirp mass distribution varies from ≈1.1M to ≈2.1M and median is obtained to be 1.14 M . The expected effective spin χ eff for isolated DNSs is 0.03 from our model. We predict that ≈34% of the current Galactic isolated DNSs will merge within a Hubble time, and have a median total mass of 2.7 M . Finally, we discuss implications for fast radio bursts and post-merger remnant gravitational-waves.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Pulsar Deathmentioning

confidence: 99%

Modelling double neutron stars: radio and gravitational waves

Chattopadhyay

Stevenson

Hurley

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…As such, death-lines (or valleys) are frequently included in pulsar population syntheses. Very recently, a reasonable reproduction of the P-Ṗ diagram has been carried out without the adoption of a death-line, or any luminosity law (Szary et al 2014). Instead, the study invoked an inverse correlation between radio efficiency and age.…”

Section: Pos(aaska14)039mentioning

confidence: 99%

Understanding the Neutron Star Population with the SKA

Tauris¹,

Kaspi²,

Breton³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

View full text Add to dashboard Cite

Since their discovery in the late 1960's the population of known neutron stars has grown to ∼2500. This sample has yielded many surprises and demonstrated that the observational properties of neutron stars are remarkably diverse. The surveys that will be performed with the SKA will produce a further tenfold increase in the number of Galactic neutron stars known. Moreover, the SKA's broad spectral coverage, sub-arraying and multi-beaming capabilities will allow us to characterise these sources with unprecedented efficiency, in turn enabling a giant leap in the understanding of their properties. We review the neutron star population and outline strategies for studying each of the growing number of diverse classes that are populating the "neutron star zoo". Questions that will be addressed by the much larger statistical samples and vastly improved timing efficiency provided by SKA include: (i) the spin period and spin-down rate distributions (and thus magnetic fields) at birth, and the associated information about the supernovae wherein they are formed; (ii) the radio pulsar-magnetar connection; (iii) the link between normal radio pulsars, intermittent pulsars and rotating radio transients; (iv) the slowest possible spin period for a radio pulsar (revealing the conditions at the pulsar death-line); (v) proper motions of pulsars (revealing supernova kick physics); (vi) the mass distribution of neutron stars; (vii) the fastest possible spin period for a recycled pulsar (constraining magnetosphere-accretion disc interactions, gravitational wave radiation and the equation-of-state); (viii) the origin of high eccentricity millisecond pulsars; (ix) the formation channels for recently identified triple systems; and finally (x) how isolated millisecond pulsars are formed. We can also expect that the first phase of the SKA (SKA1), and in particular the full SKA (SKA2), will break new ground unveiling exotic and heretofore unknown systems that will challenge our current knowledge and theories, thus fostering the development of new research areas. Some possibilities for future landmark discoveries representing significant milestones in the astrophysics of compact objects include: (i) sub-millisecond pulsars; (ii) neutron stars born as millisecond pulsars; (iii) neutron stars with masses below 1.1 or above 2.5 M ; (iv) neutron star-black hole binaries; and (v) a triple system containing a pair of neutron stars.Advancing Astrophysics with the Square Kilometre Array

show abstract

“…When new surveys had increased the detected sample ten fold, Lyne et al (1985) could estimate birth rates and Bhattacharya et al (1992) determined magnetic field longevity. Using the modern sample of over 2,000 pulsars, statistical studies of e.g., radio beaming fractions (van Leeuwen & Verbunt 2004), birth locations (Faucher-Giguère & Kaspi 2006), and radio luminosities (Szary et al 2014) have improved our understanding of the pulsar population. Such parent populations can be used to optimise the strategies for such pulsar surveys as using LOFAR (van Leeuwen & Stappers 2010) and the Square Kilometre Array (SKA; Smits et al 2009), and predict the outcomes to within a factor of a few (cf.…”

Section: Introductionmentioning

confidence: 99%

Synthesising the intrinsic FRB population using frbpoppy

Gardenier

Leeuwen

Connor

et al. 2019

A&A

View full text Add to dashboard Cite

Context. Fast Radio Bursts (FRBs) are radio transients of an unknown origin. Naturally, we are curious as to their nature. Enough FRBs have been detected for a statistical approach to parts of this challenge to be feasible. To understand the crucial link between detected FRBs and the underlying FRB source classes we perform FRB population synthesis, to determine how the underlying population behaves. The Python package we developed for this synthesis, frbpoppy, is open source and freely available. Aims. Our goal is to determine the current best fit FRB population model. Our secondary aim is to provide an easy-to-use tool for simulating and understanding FRB detections. It can compare surveys, or inform us of the intrinsic FRB population. Methods. frbpoppy simulates intrinsic FRB populations and the surveys that find them, to produce virtual observed populations. These resulting populations can then be compared with real data, allowing constrains to be placed on underlying physics and selection effects.Results. We are able to replicate real Parkes and ASKAP FRB surveys, in terms of both detection rates and distributions observed. We also show the effect of beam patterns on the observed dispersion measure (DM) distributions. We compare four types of source models. The "Complex" model, featuring a range of luminosities, pulse widths and spectral indices, reproduces current detections best. Conclusions. Using frbpoppy, an open-source FRB population synthesis package, we explain current FRB detections and offer a first glimpse of what the true population must be.

show abstract

Radio Efficiency of Pulsars

Cited by 72 publications

References 35 publications

Modelling double neutron stars: radio and gravitational waves

Modelling double neutron stars: radio and gravitational waves

Understanding the Neutron Star Population with the SKA

Synthesising the intrinsic FRB population using frbpoppy

Contact Info

Product

Resources

About