A Numerical Model for the Multiwavelength Lightcurves of PSR J0030+0451

Chen, Alexander Y.; Yuan, Yajie; Vasilopoulos, Georgios

doi:10.3847/2041-8213/ab85c5

Cited by 34 publications

(26 citation statements)

References 32 publications

(42 reference statements)

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“…By comparing the observed ∆ − δ diagram with their estimations from the model, these authors favoured the cases with high conductivities; as the conductivity increases, the system converges to the FFE limit. Chen et al (2020) recently suggested a force-free magnetospheric model and presented radio, X-ray, and gamma-ray light curves in agreement with the observations of the millisecond pulsar (MSP) PSR J0030+0451, providing an estimation of the magnetic inclination of the pulsar of ∼80 • . More recently, Kalapotharakos et al (2020) proposed the FFE model by taking into account an off-centred dipole field and quadrupole components, the Kerr-metric for the ray-tracing of photons from a distant observer to the hot spots on the surface of the star.…”

Section: Introductionsupporting

confidence: 61%

Constraining millisecond pulsar geometry using time-aligned radio and gamma-ray pulse profile

Benli

Pétri

Mitra

2021

A&A

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Context. Since the launch of the Fermi Gamma-Ray Space Telescope, several hundred gamma-ray pulsars have been discovered, some being radio-loud and some radio-quiet with time-aligned radio and gamma-ray light curves. In the second Fermi Pulsar Catalogue, 117 new gamma-ray pulsars have been reported based on three years of data collected by the Large Area Telescope on the Fermi satellite, providing a wealth of information such as the peak separation Δ of the gamma-ray pulsations and the radio lag δ between the gamma-ray and radio pulses. Aim. We selected several radio-loud millisecond gamma-ray pulsars with period P in the range 2–6 ms and showing a double peak in their gamma-ray profiles. We attempted to constrain the geometry of their magnetosphere, namely the magnetic axis and line-of-sight inclination angles for each of these systems. Method. We applied a force-free dipole magnetosphere from the stellar surface up to the striped wind region – well outside the light cylinder – to fit the observed pulse profiles in gamma-rays, consistently with their phase alignment with the radio profile. In deciding whether a fitted curve is reasonable or not, we employed a least-square method to compare the observed gamma-ray intensity with that found from our model, emphasising the amplitude of the gamma-ray peaks, their separation, and the phase lag between radio and gamma-ray peaks. Results. We obtained the best fits and reasonable parameters in agreement with observations for ten millisecond pulsars. Eventually, we constrained the geometry of each pulsar described by the magnetic inclination α and the light-of-sight inclination ζ. We found that both angles are larger than approximately 45°.

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Section: Introductionsupporting

confidence: 61%

Constraining millisecond pulsar geometry using time-aligned radio and gamma-ray pulse profile

Benli

Pétri

Mitra

2021

A&A

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“…Pair production in relation to the coherent emission of millisecond pulsars (MSP) is a subject that has received little attention, but is now of increased interest as a consequence of the NICER J0030+0451 observations (Riley et al 2019, Miller et al 2019, Bilous et al 2019. These provide the first evidence for a quadrupole component in the surface magnetic flux density whose properties have been further analysed by Chen, Yuan & Vasilopoulos (2020) and Kalapotharakos et al (2021).…”

Section: Introductionmentioning

confidence: 71%

Pair production in the millisecond pulsar J0030+0451

Jones

2021

Preprint

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The electric field accelerating electrons in the Timokhin-Arons polar-cap model as applied to millisecond pulsars is so high that the electron Lorentz factors are limited either by radiation reaction or by the Breit-Wheeler process. In the former case, it is possible to obtain an upper limit for curvature radiation momentum components perpendicular to the local magnetic field which is independent of the flux-line radius of curvature. The threshold value for single-photon conversion to pairs is high but is possibly reached in J0030+0451. However, owing to the high polar-cap temperature reported, direct pair production by the Breit-Wheeler process is probably more important. If the existence of coherent radio emission in millisecond pulsars is assumed to need a high-multiplicity pair plasma, then it follows that the primary electrons also produce gamma-rays in the Fermi -LAT energy band for which the magnetosphere is completely transparent. The absence of these, in phase with the radio emission, would be an immediate indication that ultra-high energy electrons and an active Timokhin-Arons polar cap are not present in J0030+0451.

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“…The preferred configuration of the temperature distribution for PSR J0030+0451 found by the independent analyses of Miller et al (2019) and Riley et al (2019) consists of one highly elongated (in the longitudinal direction) region and a second smaller, less elongated region, both on the hemisphere below the stellar equator relative to the observer's line of sight. Such a temperature distribution is difficult to reconcile with a standard dipole field, but could be reproduced by assuming a dipole+quadrupole field 2 (see, e.g., Gralla et al 2017;Lockhart et al 2019;Chen et al 2020;Kalapotharakos et al 2021). In such a case, the strength of the surface magnetic field inferred using a magnetic dipole braking formula could substantially underestimate the strength of the magnetic field within the atmospheres of hot spots (see Miller et al 2019).…”

Section: Neutron Star Model Atmospheresmentioning

confidence: 99%

Constraining the Neutron Star Mass--Radius Relation and Dense Matter Equation of State with NICER. III. Model Description and Verification of Parameter Estimation Codes

Bogdanov,

Dittmann,

et al. 2021

Preprint

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We describe the X-ray pulse profile models we use, and how we use them, to analyze Neutron Star Interior Composition Explorer (NICER) observations of rotation-powered millisecond pulsars to obtain information about the mass-radius relation of neutron stars and the equation of state of the dense matter in their cores. Here we detail our modeling of the observed profile of PSR J0030+0451 that we analyzed in Miller et al. (2019) andRiley et al. (2019) and describe a cross-verification of computations of the pulse profiles of a star with R/M ∼ 3, in case stars this compact need to be considered in future analyses. We also present our early cross-verification efforts of the parameter estimation procedures used by Miller et al. (2019) and Riley et al. (2019) by analyzing two distinct synthetic data sets. Both codes yielded credible regions in the mass-radius plane that are statistically consistent with one another and both gave posterior distributions for model parameter values consistent with the values that were used to generate the data. We also summarize the additional tests of the parameter estimation procedure of Miller et al. ( 2019) that used synthetic pulse profiles and the NICER pulse profile of PSR J0030+0451. We then illustrate how the precision of mass and radius estimates depends on the pulsar's spin rate and the size of its hot spot by analyzing four different synthetic pulse profiles. Finally, we assess possible sources of systematic error in these estimates made using this technique, some of which may warrant further investigation.

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A Numerical Model for the Multiwavelength Lightcurves of PSR J0030+0451

Cited by 34 publications

References 32 publications

Constraining millisecond pulsar geometry using time-aligned radio and gamma-ray pulse profile

Constraining millisecond pulsar geometry using time-aligned radio and gamma-ray pulse profile

Pair production in the millisecond pulsar J0030+0451

Constraining the Neutron Star Mass--Radius Relation and Dense Matter Equation of State with NICER. III. Model Description and Verification of Parameter Estimation Codes

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