透明导电氧化物薄膜的抗伽马辐照性能研究

利用射频磁控溅射法制备出具有良好光电性能的In₂O₃: W（IWO）薄膜,与购置的In₂O₃: Sn（ITO）薄膜一起,在伽马射线地面加速模拟试验设备中进行辐照试验。对辐照前后两种薄膜样品的微观结构、表面形貌、光电性能和元素价态进行对比分析,并用正电子湮没方法研究辐照前后的缺陷情况。结果表明,伽马射线辐照可引起ITO及IWO薄膜样品中氧空位缺陷的少量增加,且缺陷主要产生于薄膜表层及薄膜与基底界面结合处。高能伽马光子作用于透明导电氧化物薄膜,主要通过破坏其内部结合能较低的化学键,并实现薄膜系统中元素之间的选择性重组。ITO与IWO具有良好的抗伽马辐照性能,IWO相比ITO更适合于抗伽马辐照相关应用。     

New results on the time histories of gamma-ray bursts

A study of the morphology of 14 short ( 1 s) gamma ray bursts observed by the Franco Soviet SIGNE detectors onboard the VENERA spacecraft between 1978 and 1982 is presented. We find two major groups of short bursts characterised not only by their different durations ( 1 s and 100 ms respectively), but also by different e-folding rise and decay times. A study of the time history of the impulsive portion of the 1979 March 5 event at 2 ms resolution shows evidence for a previously undiscovered 23ms quasi periodicity. These results are discussed in the context of neutron star models for gamma ray bursters.     

Possible consequences of a disk around B0656+14 on e–e and near-1 Hz gravitational wave production

Nearby pulsars B0656+14 and Geminga were proposed in the literature as the main sources of cosmic-ray positrons observed near Earth above 10 GeV. B0656+14 has comparable distance from Earth, similar magnetic field and period of Geminga. However, observations in the R and I bands indicate the presence of a disk of approximately 10⁻⁴ M_⊙ around B0656+14. Radio and pulsed γ-ray flux observations from this pulsar are also consistent with supernova fallback material and disk entering the light cylinder and partially quenching the development of electromagnetic showers in the magnetosphere. If this is the case, B0656+14 has unlikely given any contribution to e⁺ and e⁻ observed near Earth. Absolute flux measurements and the level of anisotropy in the high energy electron and positron arrival directions above 50 GeV will help in revealing if none, one of both nearby pulsars are sources of these particles observed near Earth.     

New insights from cross-correlation studies between solar activity indices and cosmic-ray flux during Forbush decrease events

Observed galactic cosmic ray intensity can be subjected to a transient decrease. These so-called Forbush decreases are driven by coronal mass ejection induced shockwaves in the heliosphere. By combining in situ measurements by space borne instruments with ground-based cosmic ray observations, we investigate the relationship between solar energetic particle flux, various solar activity indices, and intensity measurements of cosmic rays during such an event. We present cross-correlation study done using proton flux data from the SOHO/ERNE instrument, as well as data collected during some of the strongest Forbush decreases over the last two completed solar cycles by the network of neutron monitor detectors and different solar observatories. We have demonstrated connection between the shape of solar energetic particles fluence spectra and selected coronal mass ejection and Forbush decrease parameters, indicating that power exponents used to model these fluence spectra could be valuable new parameters in similar analysis of mentioned phenomena. They appear to be better predictor variables of Forbush decrease magnitude in interplanetary magnetic field than coronal mass ejection velocities.