Effects of the background radiation on radio pulsar and supernova remnant searches and the birth rates of these objects

Ankay, A.; Guseinov, O. H.; Tagieva, S. O.

doi:10.1080/10556790500055408

Cited by 6 publications

(5 citation statements)

References 25 publications

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“…Identifying pulsar proper motions and velocities is critical in understanding the nature of pulsar and NS astrophysics. Applications of pulsar velocity measurements include determining the birth rate of pulsars (Ankay et al 2004), further understanding supernova remnants (Migliazzo et al 2002) and the Galactic distribution of the progenitor population (Chennamangalam & Lorimer 2014), and for this work, calculating the collision rate of as-teroids with a NS. Pulsar velocities are calculated by measuring their proper motions and distances.…”

Section: Neutron Star Velocitymentioning

confidence: 99%

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

Smallwood

Martin

Zhang

2019

Monthly Notices of the Royal Astronomical Society

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The origin of fast radio bursts (FRBs) is still a mystery. One model proposed to interpret the only known repeating object, FRB 121102, is that the radio emission is generated from asteroids colliding with a highly magnetized neutron star (NS). With N -body simulations, we model a debris disc around a central star with an eccentric orbit intruding NS. As the NS approaches the first periastron passage, most of the comets are scattered away rather than being accreted by the NS. To match the observed FRB rate, the debris belt would have to be at least three orders of magnitude more dense than the Kuiper belt. We also consider the rate of collisions on to the central object but find that the density of the debris belt must be at least four orders of magnitude more dense than the Kuiper belt. These discrepancies in the density arise even if (1) one introduces a Kuiper-belt like comet belt rather than an asteroid belt and assume that comet impacts can also make FRBs; (2) the NS moves ∼ 2 orders of magnitude slower than their normal proper-motion velocity due to supernova kicks; and (3) the NS orbit is coplanar to the debris belt, which provides the highest rate of collisions.

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Section: Neutron Star Velocitymentioning

confidence: 99%

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

Smallwood

Martin

Zhang

2019

Monthly Notices of the Royal Astronomical Society

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“…The distance to the Sun is taken to be d = 8.5 kpc. According to Ankay et al (2004) and Lorimer et al (1993), the Galactic pulsar birth rate is likely between 1/125 yr −1 and 1/250 yr −1 . We assume a conservative pulsar birth rate of 1/100 yr −1 , implying the total number of pulsars in the Galaxy is N psr = 10 8 .…”

Section: Properties and Population Analysis Of Grps With Diffuse Fluxmentioning

confidence: 99%

MODELING THE NON-RECYCLEDFERMIGAMMA-RAY PULSAR POPULATION

Perera

McLaughlin

Cordes

et al. 2013

ApJ

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We use Fermi Gamma-ray Space Telescope detections and upper limits on non-recycled pulsars obtained from the Large Area Telescope (LAT) to constrain how the gamma-ray luminosity L γ depends on the period P and the period derivativeṖ. We use a Bayesian analysis to calculate a best-fit luminosity law, or dependence of L γ on P andṖ , including different methods for modeling the beaming factor. An outer gap (OG) magnetosphere geometry provides the best-fit model, which is L γ ∝ P −aṖ b where a = 1.36 ± 0.03 and b = 0.44 ± 0.02, similar to but not identical to the commonly assumed L γ ∝ √Ė ∝ P −1.5Ṗ 0.5. Given upper limits on gamma-ray fluxes of currently known radio pulsars and using the OG model, we find that about 92% of the radio-detected pulsars have gamma-ray beams that intersect our line of sight. By modeling the misalignment of radio and gamma-ray beams of these pulsars, we find an average gamma-ray beaming solid angle of about 3.7π for the OG model, assuming a uniform beam. Using LAT-measured diffuse fluxes, we place a 2σ upper limit on the average braking index and a 2σ lower limit on the average surface magnetic field strength of the pulsar population of 3.8 and 3.2 × 10 10 G, respectively. We then predict the number of non-recycled pulsars detectable by the LAT based on our population model. Using the 2 yr sensitivity, we find that the LAT is capable of detecting emission from about 380 non-recycled pulsars, including 150 currently identified radio pulsars. Using the expected 5 yr sensitivity, about 620 non-recycled pulsars are detectable, including about 220 currently identified radio pulsars. We note that these predictions significantly depend on our model assumptions.

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“…Numerous factors contribute to selection effects, primarily including characteristics of the pulsar population, the distance to observed sources, telescope sensitivity, observation frequency, Galactic background radiation, and dispersion measure. In addition to the effects of observing frequency and instrumental characteristics, the Galactic background radiation and dispersion measure significantly influence pulsar searches (Ankay et al 2004).…”

Section: Selection Effects and Correction Methodsmentioning

confidence: 99%

Modeling the Radial Distribution of Pulsars in the Galaxy

Xie,

Wang,

Wang

et al. 2024

ApJL

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The Parkes 20 cm multibeam pulsar surveys have discovered nearly half of the known pulsars and revealed many distant pulsars with high dispersion measures. Using a sample of 1301 pulsars from these surveys, we have explored the spatial distribution and birth rate of normal pulsars. The pulsar distances used to calculate the pulsar surface density are estimated from the YMW16 electron-density model. When estimating the impact of the Galactic background radiation on our survey, we projected pulsars in the galaxy onto the Galactic plane, assuming that the flux density distribution of pulsars is uniform in all directions, and utilized the most up-to-date background temperature map. We also used an up-to-date version of the ATNF Pulsar Catalogue to model the distribution of pulsar flux densities at 1400 MHz. We derive an improved radial distribution for the pulsar surface density projected onto the Galactic plane, which has a maximum value at ∼4 kpc from the Galactic center. We also derive the local surface density and birth rate of pulsars, obtaining 47 ± 5 kpc−2 and ∼4.7 ± 0.5 kpc−2 Myr−1, respectively. For the total number of potentially detectable pulsars in the galaxy, we obtain (1.1 ± 0.2) × 104 and (1.1 ± 0.2)×105 before and after applying the Tauris & Manchester beaming correction model. The radial distribution function is used to estimate the proportion of pulsars in each spiral arm and the Galactic center.

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Effects of the background radiation on radio pulsar and supernova remnant searches and the birth rates of these objects

Cited by 6 publications

References 25 publications

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

MODELING THE NON-RECYCLEDFERMIGAMMA-RAY PULSAR POPULATION

Modeling the Radial Distribution of Pulsars in the Galaxy

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