Grouping-Enabled and Privacy-Enhancing Communications Schemes for VANETs

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Cloud Forensics Investigation: Tracing Infringing Sharing of Copyrighted Content in Cloud

Cloud Computing is becoming a significant technology trend nowadays, but its abrupt rise also creates a brand new front for cybercrime investigation with various challenges. One of the challenges is to track down infringing sharing of copyrighted content in cloud. To solve this problem, we study a typical type of content sharing technologies in cloud computing, analyze the challenges that the new technologies bring to forensics, formalize a procedure to get digital evidences and obtain analytical results based on the evidences to track down illegal uploader. Furthermore, we propose a reasoning model based on the probability distribution in a Bayesian Network to evaluate the analytical result of forensics examinations. The proposed method can accurately and scientifically track down the origin infringing content uploader and owner. Keywords: cloud forensics, peer to peer, file sharing, tracking, CloudFron

CoChecker: Detecting Capability and Sensitive Data Leaks from Component Chains in Android

Studies show that malicious applications can obtain sensitive data from and perform protected operations in a mobile phone using an authorised yet vulnerable application as a deputy (referred to as privilege escalation attack). Thus it is desirable to have a checker that can help developers check whether their applications are vulnerable to these attacks. In this paper, we introduce our tool, CoChecker, to identify the leak paths (chains of components) that would lead to privilege escalation attacks using static taint analysis. We propose to build a call graph to model the execution of multiple entry points in a component and eliminate the false negatives due to the Android's event-driven programming paradigm. We further carry out inter-component communication through intent-tracing and formulate the call graph of the analyzed app. The evaluation of CoChecker on the state-of-the-art test suit DroidBench and randomly downloaded apps shows that it is both efficient and effective. ? 2014 Springer International Publishing Switzerland.EI

Multi-messenger Observations of a Binary Neutron Star Merger

International audienceOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s}}$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg(2) at a luminosity distance of ${40}_{-8}^{+8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 $\,{M}_{\odot }$. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc}}$) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta