A Review of Experimental Techniques for Aerosol Hygroscopicity Studies
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Articles and Also and Instrumental Development
Atmos. Chem. Phys., 19, 12631–12686, 2019 https://doi.org/10.5194/acp-19-12631-2019 © Author(s) 2019. This work is distributed under the Creative Commons Attribution 4.0 License. A review of experimental techniques for aerosol hygroscopicity studies Mingjin Tang1, Chak K. Chan2, Yong Jie Li3, Hang Su4,5, Qingxin Ma6, Zhijun Wu7, Guohua Zhang1, Zhe Wang8, Maofa Ge9, Min Hu7, Hong He6,10,11, and Xinming Wang1,10,11 1State Key Laboratory of Organic Geochemistry and Guangdong Key Laboratory of Environmental Protection and Resources Utilization, Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou 510640, China 2School of Energy and Environment, City University of Hong Kong, Kowloon, Hong Kong, China 3Department of Civil and Environmental Engineering, Faculty of Science and Technology, University of Macau, Avenida da Universidade, Taipa, Macau, China 4Center for Air Pollution and Climate Change Research, Institute for Environmental and Climate Research, Jinan University, Guangzhou 511443, China 5Department of Multiphase Chemistry, Max Planck Institute for Chemistry, Mainz 55118, Germany 6State Key Joint Laboratory of Environment Simulation and Pollution Control, Research Center for Eco-Environmental Sciences, Chinese Academy of Sciences, Beijing 100085, China 7State Key Joint Laboratory of Environmental Simulation and Pollution Control, College of Environmental Sciences and Engineering, Peking University, Beijing 100871, China 8Department of Civil and Environmental Engineering, Hong Kong Polytechnic University, Hong Kong, China 9State Key Laboratory for Structural Chemistry of Unstable and Stable Species, Institute of Chemistry, Chinese Academy of Sciences, Beijing 100190, China 10University of Chinese Academy of Sciences, Beijing 100049, China 11Center for Excellence in Regional Atmospheric Environment, Institute of Urban Environment, Chinese Academy of Sciences, Xiamen 361021, China Correspondence: Mingjin Tang ([email protected]) and Chak K. -
Understanding Second-Person Storytelling
Evgenia Iliopoulou Because of You: Understanding Second-Person Storytelling Lettre Evgenia Iliopoulou born in 1986, lives in Zurich, Switzerland, and specializes in narratology, theory of literature and interdisciplinary approaches within Comparative Literature. She holds an undergraduate degree in Greek Philology from her hometown University of Patras, Greece, and an MA in Comparative Literature from Ludwig Maximilian University of Munich, Germany. In 2014, during her doctoral studies, Zurich University sponsored her participation in the summer session of School of Theory and Criticism at Cornell University in the US. Evgenia Iliopoulou Because of You: Understanding Second-Person Storytelling This work was accepted as a PhD thesis by the Faculty of Arts and Social Scien- ces, University of Zurich in the fall semester 2017 on the recommendation of the Doctoral Committee: Prof. Dr. Thomas Fries «main supervisor», Prof. Dr. Sandro Zanetti. Published with the support of the Swiss National Science Foundation. Bibliographic information published by the Deutsche Nationalbibliothek The Deutsche Nationalbibliothek lists this publication in the Deutsche Na- tionalbibliografie; detailed bibliographic data are available in the Internet at http://dnb.d-nb.de This work is licensed under the Creative Commons Attribution-NonCommercial-No- Derivatives 4.0 (BY-NC-ND) which means that the text may be used for non-commer- cial purposes, provided credit is given to the author. For details go to http://creativecommons.org/licenses/by-nc-nd/4.0/ To create an adaptation, translation, or derivative of the original work and for commer- cial use, further permission is required and can be obtained by contacting rights@ transcript-verlag.de Creative Commons license terms for re-use do not apply to any content (such as graphs, figures, photos, excerpts, etc.) not original to the Open Access publication and further permission may be required from the rights holder. -
A Complete Bibliography of Publications in Journal for the History of Astronomy
A Complete Bibliography of Publications in Journal for the History of Astronomy Nelson H. F. Beebe University of Utah Department of Mathematics, 110 LCB 155 S 1400 E RM 233 Salt Lake City, UT 84112-0090 USA Tel: +1 801 581 5254 FAX: +1 801 581 4148 E-mail: [email protected], [email protected], [email protected] (Internet) WWW URL: http://www.math.utah.edu/~beebe/ 10 May 2021 Version 1.28 Title word cross-reference $8.95 [Had84]. $87 [CWW17]. $89.95 [Gan15]. 8 = 1;2;3 [Cov15]. $90 [Ano15f]. $95 [Swe17c]. c [Kin87, NRKN16, Rag05]. mul [Kur19]. muld [Kur19]. [Kur19]. · $100 [Apt14]. $120 [Hen15b]. $127 [Llo15]. 3 [Ano15f, Ash82, Mal10, Ste12a]. ∆ [MS04]. $135.00 [Smi96]. $14 [Sch15]. $140 [GG14]. $15 [Jar90]. $17.95 [Had84]. $19.95 -1000 [Hub83]. -4000 [Gin91b]. -601 [Mul83, Nau98]. 20 [Ost07]. 2000 [Eva09b]. [Hub83]. -86 [Mar75]. -Ft [Edd71b, Mau13]. $24.95 [Lep14, Bro90]. $27 [W lo15]. $29 -inch [Ost07]. -year [GB95]. -Year-Old [Sha14]. $29.25 [Hea15]. $29.95 [Eva09b]. [Ger17, Mes15]. 30 [Mau13]. $31.00 [Bra15]. $34 [Sul14]. $35 Zaga´_ n [CM10]. [Ano15f, Dev14b, Lau14, Mir17, Rap15a]. $38 [Dan19b, Vet19]. $39.95 [Mol14b]. /Catalogue [Kun91]. /Charles [Tur07]. $39.99 [Bec15]. $40 [Dun20, LF15, Rob86]. /Collected [Gin93]. /Heretic [Tes10]. 40 [Edd71b]. $42 [Nau98]. $45 [Kes15]. /the [War08]. $49.95 [Ree20]. $49.99 [Bec15]. $50 [Kru17, Rem15]. $55 [Bon19b]. $60 [Mal15]. 0 [Ave18, Hei14a, Oes15, Swe17c, Wlo15, 600 [GB95]. $72 [Ave18]. $79 [Wil15]. 1 2 Ash82]. [Dic97a]. 1970 [Kru08]. 1971 [Wil75]. 1973 [Doe19]. 1975 [Ost80]. 1976 [Gin02d]. 1979 1 [Ano15f, BH73a, Ber14, Bru78b, Eva87b, [Ano78d]. -
Constraining the Evolutionary History of the Moon and the Inner Solar System: a Case for New Returned Lunar Samples
Space Sci Rev (2019) 215:54 https://doi.org/10.1007/s11214-019-0622-x Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples Romain Tartèse1 · Mahesh Anand2,3 · Jérôme Gattacceca4 · Katherine H. Joy1 · James I. Mortimer2 · John F. Pernet-Fisher1 · Sara Russell3 · Joshua F. Snape5 · Benjamin P. Weiss6 Received: 23 August 2019 / Accepted: 25 November 2019 / Published online: 2 December 2019 © The Author(s) 2019 Abstract The Moon is the only planetary body other than the Earth for which samples have been collected in situ by humans and robotic missions and returned to Earth. Scien- tific investigations of the first lunar samples returned by the Apollo 11 astronauts 50 years ago transformed the way we think most planetary bodies form and evolve. Identification of anorthositic clasts in Apollo 11 samples led to the formulation of the magma ocean concept, and by extension the idea that the Moon experienced large-scale melting and differentiation. This concept of magma oceans would soon be applied to other terrestrial planets and large asteroidal bodies. Dating of basaltic fragments returned from the Moon also showed that a relatively small planetary body could sustain volcanic activity for more than a billion years after its formation. Finally, studies of the lunar regolith showed that in addition to contain- ing a treasure trove of the Moon’s history, it also provided us with a rich archive of the past 4.5 billion years of evolution of the inner Solar System. Further investigations of samples returned from the Moon over the past five decades led to many additional discoveries, but also raised new and fundamental questions that are difficult to address with currently avail- able samples, such as those related to the age of the Moon, duration of lunar volcanism, the Role of Sample Return in Addressing Major Questions in Planetary Sciences Edited by Mahesh Anand, Sara Russell, Yangting Lin, Meenakshi Wadhwa, Kuljeet Kaur Marhas and Shogo Tachibana B R. -
Modeling and Mapping of the Structural Deformation of Large Impact Craters on the Moon and Mercury
MODELING AND MAPPING OF THE STRUCTURAL DEFORMATION OF LARGE IMPACT CRATERS ON THE MOON AND MERCURY by JEFFREY A. BALCERSKI Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy Department of Earth, Environmental, and Planetary Sciences CASE WESTERN RESERVE UNIVERSITY August, 2015 CASE WESTERN RESERVE UNIVERSITY SCHOOL OF GRADUATE STUDIES We hereby approve the thesis/dissertation of Jeffrey A. Balcerski candidate for the degree of Doctor of Philosophy Committee Chair Steven A. Hauck, II James A. Van Orman Ralph P. Harvey Xiong Yu June 1, 2015 *we also certify that written approval has been obtained for any proprietary material contained therein ~ i ~ Dedicated to Marie, for her love, strength, and faith ~ ii ~ Table of Contents 1. Introduction ............................................................................................................1 2. Tilted Crater Floors as Records of Mercury’s Surface Deformation .....................4 2.1 Introduction ..............................................................................................5 2.2 Craters and Global Tilt Meters ................................................................8 2.3 Measurement Process...............................................................................12 2.3.1 Visual Pre-selection of Candidate Craters ................................13 2.3.2 Inspection and Inclusion/Exclusion of Altimetric Profiles .......14 2.3.3 Trend Fitting of Crater Floor Topography ................................16 2.4 Northern -
Ages of Large Lunar Impact Craters and Implications for Bombardment During the Moon’S Middle Age ⇑ Michelle R
Icarus 225 (2013) 325–341 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Ages of large lunar impact craters and implications for bombardment during the Moon’s middle age ⇑ Michelle R. Kirchoff , Clark R. Chapman, Simone Marchi, Kristen M. Curtis, Brian Enke, William F. Bottke Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, United States article info abstract Article history: Standard lunar chronologies, based on combining lunar sample radiometric ages with impact crater den- Received 20 October 2012 sities of inferred associated units, have lately been questioned about the robustness of their interpreta- Revised 28 February 2013 tions of the temporal dependance of the lunar impact flux. In particular, there has been increasing focus Accepted 10 March 2013 on the ‘‘middle age’’ of lunar bombardment, from the end of the Late Heavy Bombardment (3.8 Ga) until Available online 1 April 2013 comparatively recent times (1 Ga). To gain a better understanding of impact flux in this time period, we determined and analyzed the cratering ages of selected terrains on the Moon. We required distinct ter- Keywords: rains with random locations and areas large enough to achieve good statistics for the small, superposed Moon, Surface crater size–frequency distributions to be compiled. Therefore, we selected 40 lunar craters with diameter Cratering Impact processes 90 km and determined the model ages of their floors by measuring the density of superposed craters using the Lunar Reconnaissance Orbiter Wide Angle Camera mosaic. Absolute model ages were computed using the Model Production Function of Marchi et al. -
Lunar Impact Basins Revealed by Gravity Recovery and Interior
Lunar impact basins revealed by Gravity Recovery and Interior Laboratory measurements Gregory Neumann, Maria Zuber, Mark Wieczorek, James Head, David Baker, Sean Solomon, David Smith, Frank Lemoine, Erwan Mazarico, Terence Sabaka, et al. To cite this version: Gregory Neumann, Maria Zuber, Mark Wieczorek, James Head, David Baker, et al.. Lunar im- pact basins revealed by Gravity Recovery and Interior Laboratory measurements. Science Advances , American Association for the Advancement of Science (AAAS), 2015, 1 (9), pp.e1500852. 10.1126/sci- adv.1500852. hal-02458613 HAL Id: hal-02458613 https://hal.archives-ouvertes.fr/hal-02458613 Submitted on 26 Jun 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. RESEARCH ARTICLE PLANETARY SCIENCE 2015 © The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. Distributed Lunar impact basins revealed by Gravity under a Creative Commons Attribution NonCommercial License 4.0 (CC BY-NC). Recovery and Interior Laboratory measurements 10.1126/sciadv.1500852 Gregory A. Neumann,1* Maria T. Zuber,2 Mark A. Wieczorek,3 James W. Head,4 David M. H. Baker,4 Sean C. Solomon,5,6 David E. Smith,2 Frank G. -
GRAIL Gravity Observations of the Transition from Complex Crater to Peak-Ring Basin on the Moon: Implications for Crustal Structure and Impact Basin Formation
Icarus 292 (2017) 54–73 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus GRAIL gravity observations of the transition from complex crater to peak-ring basin on the Moon: Implications for crustal structure and impact basin formation ∗ David M.H. Baker a,b, , James W. Head a, Roger J. Phillips c, Gregory A. Neumann b, Carver J. Bierson d, David E. Smith e, Maria T. Zuber e a Department of Geological Sciences, Brown University, Providence, RI 02912, USA b NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA c Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA d Department of Earth and Planetary Sciences, University of California, Santa Cruz, CA 95064, USA e Department of Earth, Atmospheric and Planetary Sciences, MIT, Cambridge, MA 02139, USA a r t i c l e i n f o a b s t r a c t Article history: High-resolution gravity data from the Gravity Recovery and Interior Laboratory (GRAIL) mission provide Received 14 September 2016 the opportunity to analyze the detailed gravity and crustal structure of impact features in the morpho- Revised 1 March 2017 logical transition from complex craters to peak-ring basins on the Moon. We calculate average radial Accepted 21 March 2017 profiles of free-air anomalies and Bouguer anomalies for peak-ring basins, protobasins, and the largest Available online 22 March 2017 complex craters. Complex craters and protobasins have free-air anomalies that are positively correlated with surface topography, unlike the prominent lunar mascons (positive free-air anomalies in areas of low elevation) associated with large basins. -
Science Concept 3: Key Planetary
Science Concept 6: The Moon is an Accessible Laboratory for Studying the Impact Process on Planetary Scales Science Concept 6: The Moon is an accessible laboratory for studying the impact process on planetary scales Science Goals: a. Characterize the existence and extent of melt sheet differentiation. b. Determine the structure of multi-ring impact basins. c. Quantify the effects of planetary characteristics (composition, density, impact velocities) on crater formation and morphology. d. Measure the extent of lateral and vertical mixing of local and ejecta material. INTRODUCTION Impact cratering is a fundamental geological process which is ubiquitous throughout the Solar System. Impacts have been linked with the formation of bodies (e.g. the Moon; Hartmann and Davis, 1975), terrestrial mass extinctions (e.g. the Cretaceous-Tertiary boundary extinction; Alvarez et al., 1980), and even proposed as a transfer mechanism for life between planetary bodies (Chyba et al., 1994). However, the importance of impacts and impact cratering has only been realized within the last 50 or so years. Here we briefly introduce the topic of impact cratering. The main crater types and their features are outlined as well as their formation mechanisms. Scaling laws, which attempt to link impacts at a variety of scales, are also introduced. Finally, we note the lack of extraterrestrial crater samples and how Science Concept 6 addresses this. Crater Types There are three distinct crater types: simple craters, complex craters, and multi-ring basins (Fig. 6.1). The type of crater produced in an impact is dependent upon the size, density, and speed of the impactor, as well as the strength and gravitational field of the target. -
Characterization of Previously Unidentified Lunar Pyroclastic Deposits Using Lunar Reconnaissance Orbiter Camera Data J
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 117, E00H25, doi:10.1029/2011JE003893, 2012 Characterization of previously unidentified lunar pyroclastic deposits using Lunar Reconnaissance Orbiter Camera data J. Olaf Gustafson,1 J. F. Bell III,2,3 L. R. Gaddis,4 B. R. Hawke,5 and T. A. Giguere5,6 Received 1 July 2011; revised 31 March 2012; accepted 14 April 2012; published 8 June 2012. [1] We used a Lunar Reconnaissance Orbiter Camera (LROC) global monochrome Wide-angle Camera (WAC) mosaic to conduct a survey of the Moon to search for previously unidentified pyroclastic deposits. Promising locations were examined in detail using LROC multispectral WAC mosaics, high-resolution LROC Narrow Angle Camera (NAC) images, and Clementine multispectral (ultraviolet-visible or UVVIS) data. Out of 47 potential deposits chosen for closer examination, 12 were selected as probable newly identified pyroclastic deposits. Potential pyroclastic deposits were generally found in settings similar to previously identified deposits, including areas within or near mare deposits adjacent to highlands, within floor-fractured craters, and along fissures in mare deposits. However, a significant new finding is the discovery of localized pyroclastic deposits within floor-fractured craters Anderson E and F on the lunar farside, isolated from other known similar deposits. Our search confirms that most major regional and localized low-albedo pyroclastic deposits have been identified on the Moon down to 100 m/pix resolution, and that additional newly identified deposits are likely to be either isolated small deposits or additional portions of discontinuous, patchy deposits. Citation: Gustafson, J. O., J. F. Bell III, L. R. Gaddis, B. -
Constraining the Evolutionary History of the Moon and the Inner Solar System: a Case for New Returned Lunar Samples
Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Tartèse, Romain, et al. "Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples." Space Science Reviews, 215 (December 2019): 54. © 2019, The Author(s). As Published http://dx.doi.org/10.1007/s11214-019-0622-x Publisher Springer Science and Business Media LLC Version Final published version Citable link https://hdl.handle.net/1721.1/125329 Terms of Use Creative Commons Attribution 4.0 International license Detailed Terms https://creativecommons.org/licenses/by/4.0/ Space Sci Rev (2019) 215:54 https://doi.org/10.1007/s11214-019-0622-x Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples Romain Tartèse1 · Mahesh Anand2,3 · Jérôme Gattacceca4 · Katherine H. Joy1 · James I. Mortimer2 · John F. Pernet-Fisher1 · Sara Russell3 · Joshua F. Snape5 · Benjamin P. Weiss6 Received: 23 August 2019 / Accepted: 25 November 2019 / Published online: 2 December 2019 © The Author(s) 2019 Abstract The Moon is the only planetary body other than the Earth for which samples have been collected in situ by humans and robotic missions and returned to Earth. Scien- tific investigations of the first lunar samples returned by the Apollo 11 astronauts 50 years ago transformed the way we think most planetary bodies form and evolve. Identification of anorthositic clasts in Apollo 11 samples led to the formulation of the magma ocean concept, and by extension the idea that the Moon experienced large-scale melting and differentiation. -
Science Concept 3: Key Planetary Processes Are Manifested in the Diversity of Lunar Crustal Rocks
Science Concept 3: Key Planetary Processes are Manifested in the Diversity of Lunar Crustal Rocks Science Concept 3: Key planetary processes are manifested in the diversity of crustal rocks Science Goals: a. Determine the extent and composition of the primary feldspathic crust, KREEP layer, and other products of differentiation. b. Inventory the variety, age, distribution, and origin of lunar rock types. c. Determine the composition of the lower crust and bulk Moon. d. Quantify the local and regional complexity of the current lunar crust. e. Determine the vertical extent and structure of the megaregolith. INTRODUCTION Formation and Evolution of the Moon The Moon is a unique environment, preserving crucial information about the early history and later evolution of the solar system. The lack of major surficial tectonic processes within the past few billion years or so, as well as the lack of significant quantities of surface water, have allowed for excellent preservation of the lithologies and geomorphological features that formed during the major planetary formation events. Fundamental discoveries during the Apollo program showed that the Moon is made up of a variety of volcanic and impact rock types that exhibit a particular range of chemical and mineralogical compositions. The key planetary processes conveyed by this diversity include planetary differentiation, volcanism, and impact cratering. Analysis of Apollo, Luna, and lunar meteoritic samples, as well as orbital data from a series of lunar exploration missions, generated geophysical models that strove to tell the story of the Moon. However, such models are restricted in the sense that they are based on information gathered from the samples that have so far been acquired.