PHYS.324 G- SCORING - MAY 2015

Nuclear Physics B, 2003

Events with a final-state proton carrying a large fraction of the proton beam momentum, x L > 0.6, and the square of the transverse momentum p 2 T < 0.5 GeV 2 , have been studied in e + p collisions with the ZEUS detector at HERA. Data with different photon virtualities were used: Q 2 < 0.02 GeV 2 , 0.1 < Q 2 < 0.74 GeV 2 and 3 < Q 2 < 254 GeV 2 , corresponding to integrated luminosities of 0.9, 1.85 and 3.38 pb −1 . The cross sections are given as a function of x L , p 2 T , Q 2 and the Bjorken scaling variable, x. The ratio of the cross section for leading proton production to the inclusive e + p cross section shows only a mild dependence on Q 2 and on x. In the region 0.6 < x L < 0.97, the relative yield of protons is only a weak function of x L .

International Journal of Applied Mathematical Research, 2013

In this paper, Laplace Adomian Decomposition Method (LADM) and the Multistage Laplace Adomian Decomposition Method (MLADM) were applied to obtain solutions to the Chen system for the non-chaotic and chaotic case. The study shows that the LADM only gives reliable results for t <<1. Comparison between the MLADM and the classical fourthorder Runge-Kutta (RK4) solutions shows that the MLADM performs well with high accuracy. The study shows that MLADM is a powerful and promising tool for solving nonlinear systems of ODEs of chaotic and non-chaotic nature.

Coronal mass ejections (CMEs) are the solar events which carry large amounts of plasma and magnetic fields into the heliosphere and are responsible for interplanetary shocks, geomagnetic disturbances in earth's magnetosphere and Forbush decreases in cosmic ray intensity. We have studied large Forbush decreases magnitude ≥8.00% observed during the period of 1997-2006, with coronal mass ejections, interplanetary shocks, magnetic clouds and geomagnetic storms. We have found that all the large Forbush decreases are associated with coronal mass ejections, majority of them are halo coronal mass ejections (H-CMEs) (94.44%).Halo coronal mass ejections (H-CMEs), which are related to Forbush decreases, are associated with strong X-ray solar flares of category X, M and C class with association rate of 23.52%, 58.82%, 17.64% respectively. We have further determined that vast majority of the Forbush decreases (95.00%) are associated with interplanetary shocks and the related shocks are forward shocks. The interplanetary shocks which are related to Forbush decreases, 52.63% of them are related to magnetic clouds and most of the magnetic clouds (80.00%) are of excellent or good quality. The start time of 90.00% magnetic clouds are found after the arrival time of interplanetary shocks. We have further determined that Forbush decreases which are associated with halo coronal mass ejections (H-CMEs), 94.11 %of them are associated with geomagnetic storms and 73.68% of them are intense geomagnetic storms. The onset time 84.21% geomagnetic storms are found after the onset time of Forbush decreases. We have concluded that halo coronal mass ejections (H-CMEs) associated with X-ray solar flares and related to interplanetary shocks, magnetic clouds or combination of both are mainly responsible for large Forbush decreases in cosmic ray intensity and geomagnetic storms in earth's magnetosphere.

The Astrophysical Journal, 2013

We report results from TeV gamma-ray observations of the microquasar Cygnus X-3. The observations were made with the Very Energetic Radiation Imaging Telescope Array System (VERITAS) over a time period from 2007 June 11 to 2011 November 28. VERITAS is most sensitive to gamma rays at energies between 85 GeV to 30 TeV. The effective exposure time amounts to a total of about 44 hours, with the observations covering six distinct radio/X-ray states of the object. No significant TeV gamma-ray emission was detected in any of the states, nor with all observations combined. The lack of a positive signal, especially in the states where GeV gamma rays were detected, places constraints on TeV gamma-ray production in Cygnus X-3. We discuss the implications of the results.

2000

J 02 03 11:30

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