MODELING THE NON-RECYCLED<i>FERMI</i>GAMMA-RAY PULSAR POPULATION

Perera, B. B. P.; McLaughlin, M. A.; Cordes, J. M.; Kerr, M.; Burnett, T. H.; Harding, A. K.

doi:10.1088/0004-637x/776/1/61

Cited by 11 publications

(12 citation statements)

References 68 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The fraction above confirms the domination of radioquiet pulsars and is perfectly consistent with the predictions of population synthesis with OM model which gives a value of 0.65 [13]. The PC model with inverse Compton gamma-ray production estimates the fraction as 0.25 [11] which is excluded by the observation.…”

Section: Resultssupporting

confidence: 81%

See 1 more Smart Citation

Blind search for radio-quiet and radio-loud gamma-ray pulsars with Fermi-LAT data

Рубцов

Sokolova

2015

Jetp Lett.

View full text Add to dashboard Cite

The Fermi Large Area Telescope (LAT) has observed more than a hundred of gamma-ray pulsars, about one third of which are radio-quiet, i.e. not detected at radio frequencies. The most of radioloud pulsars are detected by Fermi LAT by using the radio timing models, while the radio-quiet ones are discovered in a blind search. The difference in the techniques introduces an observational selection bias and, consequently, the direct comparison of populations is complicated. In order to produce an unbiased sample, we perform a blind search of gamma-ray pulsations using Fermi-LAT data alone. No radio data or observations at optical or X-ray frequencies are involved in the search process. We produce a gamma-ray selected catalog of 25 non-recycled gamma-ray pulsars found in a blind search, including 16 radio-quiet and 9 radio-loud pulsars. This results in the direct measurement of the fraction of radio-quiet pulsars εRQ = 64 ± 10%, which is in agreement with the existing estimates from the population modeling in the outer magnetosphere model. The Polar cap models are disfavored due to a lower expected fraction and the prediction of age dependence. The age, gamma-ray energy flux, spin-down luminosity and sky location distributions of the radio-loud and radio-quiet pulsars from the catalog do not demonstrate any statistically significant difference. The results indicate that the radio-quiet and radio-loud pulsars belong to one and the same population. The catalog shows no evidence for the radio beam evolution.

show abstract

Section: Resultssupporting

confidence: 81%

“…In these models, pulsars are observed as radio-quiet only if existing radio survey sensitivity is not sufficient to detect radio emission [11,12]. In the OM gamma-ray and radio beams naturally possess different * grisha@ms2.inr.ac.ru † sokol@ms2.inr.ac.ru geometry, which leads to a geometrical explanation of radio-quietness [13].…”

Section: Introductionmentioning

confidence: 99%

Blind search for radio-quiet and radio-loud gamma-ray pulsars with Fermi-LAT data

Рубцов

Sokolova

2015

Jetp Lett.

View full text Add to dashboard Cite

show abstract

“…Neutron Star Population with SKA Thomas M. Tauris by Bates et al (2014) find α −1.4 and β 0.5 which is very similar to the relationship found for the gamma-ray pulsar population (Perera et al 2013). This combination of parameters leads inexorably to the conclusion that the radio luminosity decays significantly with time.…”

Section: Pos(aaska14)039supporting

confidence: 80%

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

“…Allowed ranges of parameters are very limited, B d ∼ 10 13 G and P i < ∼ 3 ms. Such an NS with short P i is very rare from the initial period distribution obtained by pulsar population studies (Faucher-Giguére & Kaspi 2006;Perera et al 2013), the associated supernova remnants (Popov & Turolla 2012), and the total injected energy of pulsar wind nebulae (PWNe; Tanaka & Takahara 2013). The observed FRB luminosity is almost comparable to the spindown luminosity in the allowed parameter region at t = 3.3 yr. Then, the observed FRB flux density at 1.4GHz will rapidly decay toward < ∼ 1 Jy because the NS age in the allowed region is already t ≫ t sd .…”

Section: Constraints On Grp-like Emission Modelmentioning

confidence: 99%

Constraints on pulsed emission model for repeating FRB 121102

Kisaka

Enoto

Shibata

2017

Publications of the Astronomical Society of Japan

View full text Add to dashboard Cite

Recent localization of the repeating Fast Radio Burst (FRB) 121102 revealed the distance of its host galaxy and luminosities of the bursts. We investigated constraints on the young neutron star (NS) model, that (a) the FRB intrinsic luminosity is supported by the spin-down energy, and (b) the FRB duration is shorter than the NS rotation period. In the case of a circular cone emission geometry, conditions (a) and (b) determine the NS parameters within very small ranges, compared with that from only condition (a) discussed in previous works. Anisotropy of the pulsed emission does not affect the area of the allowed parameter region by virtue of condition (b). The determined parameters are consistent with those independently limited by the properties of the possible persistent radio counterpart and the circumburst environments such as surrounding materials. Since the NS in the allowed parameter region is older than the spin-down timescale, the hypothetical GRP-like model expects a rapid radio flux decay of < ∼ 1 Jy within a few years as the spin-down luminosity decreases. The continuous monitoring will give a hint of discrimination of the models. If no flux evolution will be seen, we need to consider an alternative model, e.g., the magnetically powered flare.

show abstract

MODELING THE NON-RECYCLEDFERMIGAMMA-RAY PULSAR POPULATION

Cited by 11 publications

References 68 publications

Blind search for radio-quiet and radio-loud gamma-ray pulsars with Fermi-LAT data

Blind search for radio-quiet and radio-loud gamma-ray pulsars with Fermi-LAT data

Understanding the Neutron Star Population with the SKA

Constraints on pulsed emission model for repeating FRB 121102

Contact Info

Product

Resources

About