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      Characterization of Environmental Dust in the Dammam Area and Mud After-Effects on Bisphenol-A Polycarbonate Sheets

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          Abstract

          Owing to recent climate changes, dust storms are increasingly common, particularly in the Middle East region. Dust accumulation and subsequent mud formation on solid surfaces in humid environments typically have adverse effects on surface properties such as optical transmittance, surface texture, and microhardness. This is usually because the mud, which contains alkaline and ionic species, adheres strongly to the surface, often through chemical bonds, and is therefore difficult to remove. In this study, environmental dust and the after-effects of mud formed on a polycarbonate sheet, which is commonly used as a protective glass in photovoltaic cells. Ionic compounds (OH ) are shown to significantly affect the optical, mechanical, and textural characteristics of the polycarbonate surface, and to increase the adhesion work required to remove the dry mud from the polycarbonate surface upon drying. Such ability to modify characteristics of the polycarbonate surface could address the dust/mud-related limitations of superhydrophobic surfaces.

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          Extreme collisions between planetesimals as the origin of warm dust around a Sun-like star

          The slow but persistent collisions between asteroids in our Solar System generate a tenuous cloud of dust known as the zodiacal light (because of the light the dust reflects). In the young Solar System, such collisions were more common and the dust production rate should have been many times larger. Yet copious dust in the zodiacal region around stars much younger than the Sun has rarely been found. Dust is known to orbit around several hundred main-sequence stars, but this dust is cold and comes from a Kuiper-belt analogous region out beyond the orbit of Neptune. Despite many searches, only a few main-sequence stars reveal warm (> 120 K) dust analogous to zodiacal dust near the Earth. Signs of planet formation (in the form of collisions between bodies) in the regions of stars corresponding to the orbits of the terrestrial planets in our Solar System have therefore been elusive. Here we report an exceptionally large amount of warm, small, silicate dust particles around the solar-type star BD+20,307 (HIP 8920, SAO 75016). The composition and quantity of dust could be explained by recent frequent or huge collisions between asteroids or other 'planetesimals' whose orbits are being perturbed by a nearby planet.
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            A late Miocene dust shower from the break-up of an asteroid in the main belt.

            Throughout the history of the Solar System, Earth has been bombarded by interplanetary dust particles (IDPs), which are asteroid and comet fragments of diameter approximately 1-1,000 microm. The IDP flux is believed to be in quasi-steady state: particles created by episodic main belt collisions or cometary fragmentation replace those removed by comminution, dynamical ejection, and planetary or solar impact. Because IDPs are rich in 3He, seafloor sediment 3He concentrations provide a unique means of probing the major events that have affected the IDP flux and its source bodies over geological timescales. Here we report that collisional disruption of the >150-km-diameter asteroid that created the Veritas family 8.3 +/- 0.5 Myr ago also produced a transient increase in the flux of interplanetary dust-derived 3He. The increase began at 8.2 +/- 0.1 Myr ago, reached a maximum of approximately 4 times pre-event levels, and dissipated over approximately 1.5 Myr. The terrestrial IDP accretion rate was overwhelmingly dominated by Veritas family fragments during the late Miocene. No other event of this magnitude over the past approximately 10(8) yr has been deduced from main belt asteroid orbits. One remarkably similar event is present in the 3He record 35 Myr ago, but its origin by comet shower or asteroid collision remains uncertain.
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              Interplanetary dust from the explosive dispersal of hydrated asteroids by impacts

              The Earth accretes about 30,000 tons of dust particles per year, with sizes in the range of 20-400 microm (refs 1, 2). Those particles collected at the Earth's surface--termed micrometeorites--are similar in chemistry and mineralogy to hydrated, porous meteorites, but such meteorites comprise only 2.8% of recovered falls. This large difference in relative abundances has been attributed to 'filtering' by the Earth's atmosphere, that is, the porous meteorites are considered to be so friable that they do not survive the impact with the atmosphere. Here we report shock-recovery experiments on two porous meteorites, one of which is hydrated and the other is anhydrous. The application of shock to the hydrated meteorite reduces it to minute particles and explosive expansion results upon release of the pressure, through a much broader range of pressures than for the anhydrous meteorite. Our results indicate that hydrated asteroids will produce dust particles during collisions at a much higher rate than anhydrous asteroids, which explains the different relative abundances of the hydrated material in micrometeorites and meteorites: the abundances are established before contact with the Earth's atmosphere.
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                Author and article information

                Journal
                Sci Rep
                Sci Rep
                Scientific Reports
                Nature Publishing Group
                2045-2322
                14 April 2016
                2016
                : 6
                : 24308
                Affiliations
                [1 ]Mechanical Engineering Department and Centre of Excellence in Renewable Energy, King Fahd University of Petroleum & Minerals , Dhahran, Saudi Arabia
                [2 ]Chemistry Department, King Fahd University of Petroleum & Minerals , Dhahran, Saudi Arabia
                [3 ]Mechanical Engineering Department, King Fahd University of Petroleum & Minerals , Dhahran, Saudi Arabia
                [4 ]Mechanical Engineering Department, Massachusetts Institute of Technology , Boston, USA
                Author notes
                Article
                srep24308
                10.1038/srep24308
                4830985
                27076199
                826669ed-183e-4176-85aa-f08811f263a9
                Copyright © 2016, Macmillan Publishers Limited

                This work is licensed under a Creative Commons Attribution 4.0 International License. The images or other third party material in this article are included in the article’s Creative Commons license, unless indicated otherwise in the credit line; if the material is not included under the Creative Commons license, users will need to obtain permission from the license holder to reproduce the material. To view a copy of this license, visit http://creativecommons.org/licenses/by/4.0/

                History
                : 29 October 2015
                : 21 March 2016
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