Young and rotation-powered neutron stars (NSs) are commonly observed as rapidly-spinning pulsars. They dissipate their rotational energy by emitting pulsar wind with electromagnetic radiation spin down at a steady rate, according to the simple steadily-rotating magnetic dipole model. In reality, however, multiwavelength observations of from NS surface magnetosphere have revealed that evolution properties NSs highly diverse, often dubbed 'NS zoo'. particular, many young magnetized show high...

We analyse the rotation measures (RMs) of pulsars to study random magnetic field in Galaxy without using any large-scale models. Since spatial fluctuations interstellar have scales extending up a few kiloparsecs, cannot be evaluated by analysis residuals derived from observed RMs and those predicted simple model which is fitted so as minimize variance. propose use pairs are seen almost same directions on sky. obtain mean strengths |$\mid B_{\parallel} \mid$| regions between paired...

We present spectral analysis of the Crab Nebula obtained with {\it Chandra} X-ray observatory. The spectrum is characterized by a power-law whose index varies across nebula. variation can be discussed in terms particle injection from pulsar two different directions: equatorial plane containing torus and symmetry axis along jet. In plane, spectra within are hardest, photon $α\approx 1.9$, almost independent surface brightness. At periphery torus, gradually softens outer, lower brightness...

Broadband (0.8–70 keV) spectra of the persistent X-ray emission from nine magnetars were obtained with Suzaku, including three objects in apparent outburst. The soft component was detected all them, a typical blackbody temperature kT ∼ 0.5 keV, while hard-tail component, dominating above ∼10 at ∼1 mCrab intensity seven them. Therefore, spectrum composed and may be considered to common property magnetars, both their active quiescent states. Wide-band spectral analyses revealed that has 1–60...

Abstract The 1–70 keV persistent spectra of 15 magnetars, observed with Suzaku from 2006 to 2013, were studied as a complete sample. Combined early NuSTAR observations four hard X-ray emitters, nine objects showed power-law emission dominating at <?CDATA $\gtrsim 10$?> the 15–60 flux ∼1– $11\times {10}^{-11}$?> erg s −1 cm −2 . luminosity ${L}_{{\rm{h}}}$?> , relative that soft-thermal surface radiation ${L}_{{\rm{s}}}$?> tends become higher toward younger and strongly magnetized objects....

We report the first clear detection of X-ray pulsation magnetospheric origin from a millisecond pulsar, PSR B1821-24, with Advanced Satellite for Cosmology and Astrophysics. The photon arrival time shows periodicity 3.05 ms period, as observed in radio band. pulse is double peaked. pulses are characterized by sharp temporal profile hard power-law spectrum phase-averaged index ~1.9. These two features quite similar to X-ray/γ-ray Crab pulsar characteristic nonthermal emission magnetosphere...

We present new ASCA observations covering the 0.5-10 keV X-ray range of cooling neutron star candidates PSR 0656+14 and 1055-52. Previous ROSAT had shown that two-component models, either two blackbodies or a blackbody plus power-law, provided best spectral fits to their emission. The combined spectrum reveals components with T ≈ 8 × 105 K 1.5 106 shows evidence power-law component is needed account for higher energy photons. This three-component fit gives reduced χ2 half value more...

We investigate a stationary pair production cascade in the outer magnetosphere of spinning neutron star. The charge depletion due to global flows charged particles causes large electric field along magnetic lines. Migratory electrons and/or positrons are accelerated by this radiate γ-rays via curvature and inverse Compton processes. Some these collide with X-rays materialize as pairs gap. replenished charges partially screen field, which is self-consistently solved together energy...

We study the structure of a stationary and axisymmetric charge-deficient region (or potential gap) in outer magnetosphere spinning neutron star. Assuming existence global current flow patterns magnetosphere, charge depletion causes large electric field along magnetic lines. This longitudinal accelerates migratory electrons and/or positrons to ultrarelativistic energies. These relativistic electrons/positrons radiate γ-ray photons by curvature radiation. γ-rays, turn, produce yet more...

We developed a magneto-turbulent model for the cosmic ray (CR) electrons seen in radio halo clusters of galaxies. Steady state momentum distribution functions CR are calculated given spectra turbulent Alfven waves. The spectrum produced by obtained electron is compared to observed Coma halo. find that cluster well reproduced when spectral index waves 2.8. energy steeper than expected from turbulence theory, suggesting back reaction particle acceleration. fitting procedure constraints...

We present numerical solutions for axisymmetric thermo-centrifugal winds with a dipole magnetic flux distribution on the stellar surface. Parameters of models are chosen to be those typical Sun, except angular velocity Ω0, which is increased up 60 times solar value. The moment not but kept constant. value β plasma about unity surface, and range ratio Ω0 ωA/Cs 0–2.6, where ωA equatorial radius Alfvén surface Cs sound velocity. As more than 10 value, centrifugal (electromagnetic) driving force...

A two-dimensional electrodynamic model is used to study particle acceleration and non-thermal emission mechanisms in the pulsar magnetospheres. We solve distribution of accelerating electric field with process pair-creation meridional plane, which includes rotational axis magnetic axis. By solving evolutions Lorentz factor, pitch angle, we calculate spectrum optical through $γ$-ray bands curvature radiation, synchrotron inverse-Compton not only for outgoing particles, but also ingoing were...

We report here the first measurement of spin-down rate 65 ms X-ray pulsar within supernova remnant G11.2-0.3. The period derivative is measured to be = (4.40) × 10-14 s s-1 using Advanced Satellite for Cosmology and Astrophysics BeppoSAX. From its derivative, corresponding surface magnetic field (B 1.7 1012 G) characteristic age [P/(2) 2.4 104 yr] are derived. physical association with historical record A.D. 386 discussed in context . If was formed during event, initial pulse should have...

Relativistic acceleration and electron-positron pair production are supposed to occur deep within the light-cylinder, leading an outflowing plasma stream consisting of highy γ primary electrons a high-density sea moderate-γ pairs. The potential difference between star associated degree sub-rotation both quite modest. assumption strictly dissipation-free flow would lead singularities in magnetic field, occurring short distance beyond light-cylinder. quasi-steady model proposed necessarily has...

The age of a supernova remnant (SNR) is, though undoubtedly one the most important properties for study its evolution, difficult to estimate reliably in cases. In this study, we compare dynamical and plasma ages SNRs characteristic their associated pulsars with corresponding SNRs' that are generally thought be reliable ($t_{\rm r}$): historical light-echo SNRs, kinematic ejecta knots neutron stars (NS). or NS is time they have taken reach current positions from explosion center. We use all...

There are differing views in the literature as to location of an accelerating electric field component Eǁ along magnetic field, because assumptions about appropriate boundary conditions.

view Abstract Citations (48) References (28) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Magnetosphere of the Rotation-powered Pulsar: A DC Circuit Model Shibata, Shinpei large-scale magnetospheric current system is analyzed in order to study global structure magnetosphere rotation-powered pulsars. Local models are constructed for parts with adjustable free parameters, and they linked a model by imposing link conditions. The operating points obtained...

Abstract To explain the pulsed emission of rotation powered pulsars from radio to gamma-ray, polar cap models, slot gap and outer models are proposed. Recent observations suggest that these likely co-exist in same magnetosphere. If so, their mutual relation is known be troublesome (Harding 2009), due boundary conditions direction current, which properly assumed each acceleration model. We performed a particle simulation for global magnetospheric structure. Based on this simulation, we...

ABSTRACT Previous works have suggested a correlation between the X-ray luminosity <?CDATA ${L}_{{\rm{x}}}$?> and rotational ${L}_{\mathrm{rot}}$?> of radio pulsars. However, none obtained regression lines is statistically acceptable due to large scatter. We construct statistical model that has an intrinsic – relation reproduces observed distribution about it by using Monte Carlo simulator, which takes into account effects obscuring relation, i.e., anisotropy radiation, additional heating,...

We investigate a stationary pair-production cascade in the outer magnetosphere of spinning neutron star. The charge depletion due to global flows charged particles causes large electric field along magnetic lines. Migratory electrons and/or positrons are accelerated by this radiate curvature gamma rays, some which collide with X-rays materialize as pairs gap. replenished charges partially screen field, is self-consistently solved together distribution functions and rays. If no current...

We have detected pulsed X-ray emission from the fastest millisecond pulsar known, PSR B1937+21 (P = 1.558 ms), with ASCA. The is as a point source above ~1.7 keV, no indication of nebulosity. flux in 2-10 keV band found to be f (3.7 ± 0.6) × 10-13 ergs s-1 cm-2, which implies an isotropic luminosity LX 4πD2f ~ (5.7 1.0) 1032(D/3.6 kpc)2 s-1, where D distance, and efficiency ~5 10-4, relative spin-down power pulsar. pulsation at period predicted by radio ephemeris very narrow primary peak,...

In this paper, we present an expanding disc model to derive polarization properties of the Crab nebula. The distribution function plasma and energy density magnetic field are prescribed as distance from pulsar by using Kennel Coroniti (1984) with $σ= 0.003$, where $σ$ is ratio Poynting flux kinetic in bulk motion just before termination shock. Unlike previous models, introduce disordered field, which parameterized fractional component. Flow dynamics not solved. mean toroidal. Averaged degree...

The main issue regarding the pulsar magnetosphere is how rotation power converted into both particle beams which cause pulsed emissions, and a highly relativistic wind of electron–positron plasmas forms surrounding nebulae shining in X-rays TeV γ-rays. As sequel to our previous paper, we carried out three-dimensional simulation for axisymmetric global magnetosphere. We present results additional calculations, are higher resolution models pair creation rate cases, detailed analysis solution....

We study the structure of a stationary and axisymmetric charge-deficient region (or potential gap) in outer magnetosphere spinning neutron star. A large electric field along magnetic lines is created this gap accelerates migratory electrons (e−) and/or positrons (e+) to ultrarelativistic energies. Assuming that immersed dense soft photon field, these relativistic e± radiate γ-ray photons via inverse Compton (IC) scattering. These γ-rays, turn, produce yet more radiating particles by...

The simplest model illustrating the effect of magnetospheric charge-current field on structure a pulsar magnetic has region within light-cylinder filled with Goldreich-Julian charge density which corotates neutron star, but no electric currents along lines. This previously been studied for axisymmetric case, rotation and dipolar axes aligned. analogous problem is now solved two mutually perpendicular, so that not only material current arising from rotating charges also displacement...