On the evolution of anomalous X-ray pulsars and soft gamma ray repeaters with fallback disks

We show that the period clustering of anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs), their X-ray luminosities, ages and statistics can be explained with fallback disks with large initial specific angular momentum. The disk evolution models are developed by comparison to self-similar analytical models. The initial disk mass and angular momentum set the viscous timescale. An efficient torque, with (1 - w^2) dependence on the fastness parameter w leads to period clustering in the observed AXP-SGR period range under a wide range of initial conditions. The timescale t_0 for the early evolution of the fallback disk, and the final stages of fallback disk evolution, when the disk becomes passive, are the crucial determinants of the evolution. The disk becomes passive at temperatures around 100 K, which provides a natural cutoff for the X-ray luminosity and defines the end of evolution in the observable AXP and SGR phase. This low value for the minimum temperature for active disk turbulence indicates that the fallback disks are active up to a large radius greater than ~10^{12} cm. We find that transient AXPs and SGRs are likely to be older than their persistent cousins. A fallback disk with mass transfer rates corresponding to the low quiescent X-ray luminosities of the transient sources in early evolutionary phases would have a relatively lower initial mass, such that the mass-flow rate in the disk is not sufficient for the inner disk to penetrate into the light cylinder of the young neutron star, making mass accretion onto the neutron star impossible. The transient AXP phase therefore must start later. The model results imply that the transient AXP/SGRs, although older, are likely to be similar in number to persistent sources (abridged).Comment: 42 pages, 22 figures. Accepted for publication in the Astrophysical Journa

On the evolution of the radio pulsar PSR J1734−3333

Recent measurements showed that the period derivative of the ‘hig h-B’ radio pulsar PSR J1734−3333 is increasing with time. For neutron stars evolving with fallback disks, this rotational behavior is expected in certain phases of the long-term evolution. Using the same model as employed earlier to explain the evolution of anomalous X-ray pulsars and soft gamma-ray repeaters, we show that the period,the first and second period derivatives and the X-ray luminosity of this source can simultaneously acquire the observed values for a neutron star evolving with a fallback disk. We find that the required strength of the dipole field that can produce the source properties is in the range of 10^12 − 10^13 G on the pole of the neutron star. When the model source reaches the current state properties of PSR J1734−3333, accretion onto the star has not started yet, allowing the source to operate as a regular radio pulsar. Our results imply that PSR J1734−3333 is at an age of ∼3×10^4 −2×10^5years. Such sources will have properties like the X-ray dim isolated neutron stars or transient AXPs at a later epoch of weak accretion from the diminished fallback disk

On the outburst light curves of soft X-Ray transients as response of the accretion disk to mass deposition

We note that the solution of accretion disk dynamics for an initial delta-function mass distribution gives a light curve that fits both the rise and the decay pattern of the outburst light curves of black-hole soft X-ray transients (BSXTs) until the onset of the first mini outburst quite well. The Green's function solution of Lynden-Bell & Pringle (1974) is employed for two differenttime-independent viscosity laws to calculate the expected count rates of X-ray photons in the Ginga energy bands as a function of time. For both models basic characteristics of the outburst light curves of two typical sources GS 2000+25 and GS/GRS 1124-68 are reproduced together with plausible values of the thin disk parameter $\alpha$ and the recurrence times. This agreement with the outburst light curves and the source properties during quiescence support the idea of mass accumulation and the sporadic release of accumulated mass at the outer disk

The Energy Spectrum of Anomalous X-ray Pulsars and Soft Gamma-ray Repeaters

Assuming that AXPs and SGRs accrete matter from a fallback disk, we attempt to explain both the soft and the hard X-ray emission as the result of the accretion process. We also attempt to explain their radio emission or the lack of it. We test the hypothesis that the power-law, hard X-ray spectra are produced in the accretion flow mainly by bulk-motion Comptonization of soft photons emitted at the neutron star surface. Fallback disk models invoke surface dipole magnetic fields of $10^{12} - 10^{13}$ G, which is what we assume here. Unlike normal X-ray pulsars, for which the accretion rate is highly super-Eddington, the accretion rate is approximately Eddington in AXPs and SGRs and thus the bulk-motion Comptonization operates efficiently. As an illustrative example we reproduce both the hard and the soft X-ray spectra of AXP 4U 0142+61 well using the XSPEC package compTB. Our model seems to explain both the hard and the soft X-ray spectra of AXPs and SGRs, as well as their radio emission or the lack of it, in a natural way. It might also explain the short bursts observed in these sources. On the other hand, it cannot explain the giant X-ray outbursts observed in SGRs, which may result from the conversion of magnetic energy in local multipole fields.Comment: 6 pages, 2 figures, minor corrections, accepted for publication in A&

On the X-Ray Light Curve, Pulsed-Radio Emission, and Spin Frequency Evolution of the Transient Anomalous X-Ray Pulsar Xte J1810--197 During its X-Ray Outburst

We show that: (i) the long-term X-ray outburst light curve of the transient AXP XTE J1810-197 can be accounted for by a fallback disk that is evolving towards quiescence through a disk instability after having been heated by a soft gamma-ray burst, (ii) the spin-frequency evolution of this source in the same period can also be explained by the disk torque acting on the magnetosphere of the neutron star, (iii) most significantly, recently observed pulsed-radio emission from this source coincides with the epoch of minimum X-ray luminosity. This is natural in terms of a fallback disk model, as the accretion power becomes so low that it is not sufficient to suppress the beamed radio emission from XTE J1810-197.Comment: 13 pages, 2 Figures, accepted for publication in Ap

Abspaltung ortho-ständiger Substituenten aus ionisierten Phenyl-2-propanonen nach Elektronenstoßaktivierung

Die Molekülionen der Phenyl-2-propanone 2a-4a verlieren positionsspezifisch o-ständige Cl -, Br - bzw. I -Atome unter Bildung von (M-Hal')+- Ionen (m/z 133) hoher Intensität (70/12 eV; 1. und 2. FFR) und identischer Struktur (MIKE-CAD-Spektren). Die Fragmentionen bei m/z 133 aus o- Chlorphenyl-2-propanon (2a) und 2,2-Dimethyl-2,3-dihydro[fc]furan (11) sind von ähnlicher, aber nicht identischer Struktur. Die stoßaktivierten (2. FFR) (M-Br*)+-Ionen aus o-Bromphenyl-2-propanon (3a) und 1-Brom-lphenyl- 2-propanon (12) liefern praktisch deckungsgleiche Spektren. Die Hauptreaktion der (M-Hal')+-Ionen aus 2a-4a ist die Abspaltung von CO, das ausschließlich das C-Atom der Carbonylgruppe enthält (13C-Markierung). Der mechanistische Verlauf der Reaktionsfolge wird diskutiert (Abb. 5 und 8). In the gas phase, the phenyl-2-propanone molecules 2a-4a lose upon electron impact chloro-, bromo-, and iodo-radicals specifically at the orthoposition of the phenyl group giving rise to strong (M-Hal')+-ions (70/12 eV; 1st and 2nd FFR) of identical structure as confirmed by their MIKECAD- spectra. The daughter ions at m/z 133 from o-chlorophenyl-2-propanone (2a) and 2,2-dimethyl-2,3-dihydro[b]furane (11) are structurally similar but not identical (similarity index 99.8). The collisionally activated (2nd FFR) (M-Br')+-ions from o-bromophenyl-2-propanone (3a) and 1- bromo-1-phenyl-2-propanone (12) produce virtually congruent spectra. The most important subsequent fragmentation of the (M-Hal')+-ions from 2a-4a is the loss of CO which incorporates the C-atom of the carbonyl group exclusively (13C labelling). Mechanistic aspects of the fragmentation sequences are discussed (Figs. 5 and 8)

Cross Sections for Neutron–Deuteron Elastic Scattering in the Energy Range 135–250 MeV

We report new measurements of the neutron–deuteron elastic scattering cross section at energies from 135 to 250 MeV and center-of-mass angles from 80° to 130°. Cross sections for neutron-proton elastic scattering were also measured with the same experimental setup for normalization purposes. Our nd cross section results are compared with predictions based on Faddeev calculations including three-nucleon forces, and with cross sections measured with charged particle and neutron beams at comparable energies

The Investigation of Stability of Tunnels and Settlements with Centrifuge Modeling

In most of the larger cities underground transportation systems have been gettingdesired. Such systems are constructed in urban areas and involve a tunnel, especially in softground and in shallow zones.One of major concerns for tunneling operations in urban area is the effect onneighboring buildings, because the tunneling operation and near structures highly interacteach other. Whatever the used construction method is, the excavation of a tunnel causesdisplacement around the opening and may expand towards the ground surface. Thedislocations of the buildings interact with the ground movement, and the rigidity of existingstructures will promote reduction of the magnitude of displacements induced by tunneling.In this investigation, to determine displacements induced by tunneling, the centrifugemodeling was used. The small scale centrifuge model provided dependable information aboutthe face collapse of a shallow tunnel. A required support pressure for shield driven tunnels insoft materials, and the ground deformations along the longitudinal section of the tunnelmodel, can be identified by simulating a loss of tunnel face stability

X-Ray and Infrared Enhancement of Anomalous X-ray Pulsar 1E 2259+58

The long term (~1.5 years) X-ray enhancement and the accompanying infrared enhancement light curves of the anomalous X-ray pulsar 1E 2259+58 following the major bursting epoch can be accounted for by the relaxation of a fall back disk that has been pushed back by a gamma-ray flare. The required burst energy estimated from the results of our model fits is low enough for such a burst to have remained below the detection limits. We find that an irradiated disk model with a low irradiation efficiency is in good agreement with both X-ray and infrared data. Non-irradiated disk models also give a good fit to the X-ray light curve, but are not consistent with the infrared data for the first week of the enhancement.Comment: 17 pages, 3 figures, accepted for publication in Ap