The Newsletter of the Carnegie Institution FA L L 2 0 1 4
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Arxiv:2102.09424V2 [Astro-Ph.EP] 20 Feb 2021 the first Exoplanet
Draft version February 23, 2021 Typeset using LATEX twocolumn style in AASTeX63 Planets Across Space and Time (PAST). I. Characterizing the Memberships of Galactic Components and Stellar Ages: Revisiting the Kinematic Methods and Applying to Planet Host Stars Di-Chang Chen,1, 2 Ji-Wei Xie,1, 2 Ji-Lin Zhou,1, 2 Su-Bo Dong,3 Chao Liu,4, 5 Hai-Feng Wang,6 Mao-Sheng Xiang,7, 8 Yang Huang,9 Ali Luo,7 and Zheng Zheng10 1School of Astronomy and Space Science, Nanjing University, Nanjing 210023, China 2Key Laboratory of Modern Astronomy and Astrophysics, Ministry of Education, Nanjing 210023, China 3Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China 4Key Lab of Space Astronomy and Technology, National Astronomical Observatories, CAS, 100101, China 5University of Chinese Academy of Sciences, Beijing, 100049, China. 6South-Western Institute for Astronomy Research, Yunnan University, Kunming, 650500, China; LAMOST Fellow 7National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China 8Max-Planck Institute for Astronomy, K¨onigstuhl17, D-69117 Heidelberg, Germany 9South-Western Institute for Astronomy Research, Yunnan University, Kunming, 650500, China 10Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 ABSTRACT Over 4,000 exoplanets have been identified and thousands of candidates are to be confirmed. The relations between the characteristics of these planetary systems and the kinematics, Galactic compo- nents, and ages of their host stars have yet to be well explored. Aiming to addressing these questions, we conduct a research project, dubbed as PAST (Planets Across Space and Time). To do this, one of the key steps is to accurately characterize the planet host stars. -
Science Concept 5: Lunar Volcanism Provides a Window Into the Thermal and Compositional Evolution of the Moon
Science Concept 5: Lunar Volcanism Provides a Window into the Thermal and Compositional Evolution of the Moon Science Concept 5: Lunar volcanism provides a window into the thermal and compositional evolution of the Moon Science Goals: a. Determine the origin and variability of lunar basalts. b. Determine the age of the youngest and oldest mare basalts. c. Determine the compositional range and extent of lunar pyroclastic deposits. d. Determine the flux of lunar volcanism and its evolution through space and time. INTRODUCTION Features of Lunar Volcanism The most prominent volcanic features on the lunar surface are the low albedo mare regions, which cover approximately 17% of the lunar surface (Fig. 5.1). Mare regions are generally considered to be made up of flood basalts, which are the product of highly voluminous basaltic volcanism. On the Moon, such flood basalts typically fill topographically-low impact basins up to 2000 m below the global mean elevation (Wilhelms, 1987). The mare regions are asymmetrically distributed on the lunar surface and cover about 33% of the nearside and only ~3% of the far-side (Wilhelms, 1987). Other volcanic surface features include pyroclastic deposits, domes, and rilles. These features occur on a much smaller scale than the mare flood basalts, but are no less important in understanding lunar volcanism and the internal evolution of the Moon. Table 5.1 outlines different types of volcanic features and their interpreted formational processes. TABLE 5.1 Lunar Volcanic Features Volcanic Feature Interpreted Process -
Download Artist's CV
I N M A N G A L L E R Y Michael Jones McKean b. 1976, Truk Island, Micronesia Lives and works in New York City, NY and Richmond, VA Education 2002 MFA, Alfred University, Alfred, New York 2000 BFA, Marywood University, Scranton, Pennsylvania Solo Exhibitions 2018-29 (in progress) Twelve Earths, 12 global sites, w/ Fathomers, Los Angeles, CA 2019 The Commune, SuPerDutchess, New York, New York The Raw Morphology, A + B Gallery, Brescia, Italy 2018 UNTMLY MLDS, Art Brussels, Discovery Section, 2017 The Ground, The ContemPorary, Baltimore, MD Proxima Centauri b. Gleise 667 Cc. Kepler-442b. Wolf 1061c. Kepler-1229b. Kapteyn b. Kepler-186f. GJ 273b. TRAPPIST-1e., Galerie Escougnou-Cetraro, Paris, France 2016 Rivers, Carnegie Mellon University, Pittsburgh, PA Michael Jones McKean: The Ground, The ContemPorary Museum, Baltimore, MD The Drift, Pittsburgh, PA 2015 a hundred twenty six billion acres, Inman Gallery, Houston, TX three carbon tons, (two-person w/ Jered Sprecher) Zeitgeist Gallery, Nashville, TN 2014 we float above to spit and sing, Emerson Dorsch, Miami, FL Michael Jones McKean and Gilad Efrat, Inman Gallery, at UNTITLED, Miami, FL 2013 The Religion, The Fosdick-Nelson Gallery, Alfred University, Alfred, NY Seven Sculptures, (two person show with Jackie Gendel), Horton Gallery, New York, NY Love and Resources (two person show with Timur Si-Qin), Favorite Goods, Los Angeles, CA 2012 circles become spheres, Gentili APri, Berlin, Germany Certain Principles of Light and Shapes Between Forms, Bernis Center for ContemPorary Art, Omaha, NE -
High Energy Signatures of Black Hole Formation with Multimessenger Astronomy Alexander L
University of Wisconsin Milwaukee UWM Digital Commons Theses and Dissertations May 2016 Monsters in the Dark: High Energy Signatures of Black Hole Formation with Multimessenger Astronomy Alexander L. Urban University of Wisconsin-Milwaukee Follow this and additional works at: https://dc.uwm.edu/etd Part of the Astrophysics and Astronomy Commons, and the Physics Commons Recommended Citation Urban, Alexander L., "Monsters in the Dark: High Energy Signatures of Black Hole Formation with Multimessenger Astronomy" (2016). Theses and Dissertations. 1218. https://dc.uwm.edu/etd/1218 This Dissertation is brought to you for free and open access by UWM Digital Commons. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of UWM Digital Commons. For more information, please contact [email protected]. MONSTERS IN THE DARK: HIGH ENERGY SIGNATURES OF BLACK HOLE FORMATION WITH MULTIMESSENGER ASTRONOMY by Alexander L. Urban A Dissertation Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Physics at The University of Wisconsin–Milwaukee May 2016 ABSTRACT MONSTERS IN THE DARK: GLIMPSING THE HIGH ENERGY SIGNATURES OF BLACK HOLE FORMATION WITH MULTIMESSENGER ASTRONOMY by Alexander L. Urban The University of Wisconsin–Milwaukee, 2016 Under the Supervision of Professor Patrick R. Brady When two compact objects inspiral and violently merge it is a rare cosmic event, producing fantastically “luminous” gravitational wave emission. It is also fleeting, stay- ing in the Laser Interferometer Gravitational-wave Observatory’s (LIGO) sensitive band only for somewhere between tenths of a second and several tens of minutes. However, when there is at least one neutron star, disk formation during the merger may power a slew of potentially detectable electromagnetic counterparts, such as short γ-ray bursts (GRBs), afterglows, and kilonovae. -
Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55 -
10/17/2015 1 the Origin of the Solar System Chapter 10
10/17/2015 Guidepost As you explore the origins and the materials that make up the solar system, you will discover the answers to several important questions: What are the observed properties of the solar system? Chapter 10 What is the theory for the origin of the solar system that explains the observed properties? The Origin of the Solar System How did Earth and the other planets form? What do astronomers know about other extrasolar planets orbiting other stars? In this and the following six chapters, we will explore in more detail the planets and other objects that make up our solar system, our home in the universe. A Survey of the Solar System Two Kinds of Planets The solar system consists of eight Planets of our solar system can be divided into two very major planets and several other different kinds: objects. Jovian (Jupiter- like) planets: The planets rotate on their axes and Jupiter, Saturn, revolve around the Sun. Uranus, Neptune The planets have elliptical orbits, sometimes inclined to the ecliptic, and all planets revolve in the same directly; only Venus and Uranus rotate in an alternate direction. Nearly all moons also revolve in the Terrestrial (Earthlike) same direction. planets: Mercury, Venus, Earth, Mars Terrestrial Planets Craters on Planets’ Surfaces Craters (like on our Four inner moon’s surface) are planets of the common throughout solar system the solar system. Relatively small in size Not seen on Jovian and mass planets because (Earth is the Surface of Venus they don’t have a largest and Rocky surface can not be seen solid surface. -
Cosmos: a Spacetime Odyssey (2014) Episode Scripts Based On
Cosmos: A SpaceTime Odyssey (2014) Episode Scripts Based on Cosmos: A Personal Voyage by Carl Sagan, Ann Druyan & Steven Soter Directed by Brannon Braga, Bill Pope & Ann Druyan Presented by Neil deGrasse Tyson Composer(s) Alan Silvestri Country of origin United States Original language(s) English No. of episodes 13 (List of episodes) 1 - Standing Up in the Milky Way 2 - Some of the Things That Molecules Do 3 - When Knowledge Conquered Fear 4 - A Sky Full of Ghosts 5 - Hiding In The Light 6 - Deeper, Deeper, Deeper Still 7 - The Clean Room 8 - Sisters of the Sun 9 - The Lost Worlds of Planet Earth 10 - The Electric Boy 11 - The Immortals 12 - The World Set Free 13 - Unafraid Of The Dark 1 - Standing Up in the Milky Way The cosmos is all there is, or ever was, or ever will be. Come with me. A generation ago, the astronomer Carl Sagan stood here and launched hundreds of millions of us on a great adventure: the exploration of the universe revealed by science. It's time to get going again. We're about to begin a journey that will take us from the infinitesimal to the infinite, from the dawn of time to the distant future. We'll explore galaxies and suns and worlds, surf the gravity waves of space-time, encounter beings that live in fire and ice, explore the planets of stars that never die, discover atoms as massive as suns and universes smaller than atoms. Cosmos is also a story about us. It's the saga of how wandering bands of hunters and gatherers found their way to the stars, one adventure with many heroes. -
Arxiv:2103.02709V1
Draft version September 19, 2021 Typeset using LATEX default style in AASTeX63 A Gaussian Process Regression Reveals No Evidence for Planets Orbiting Kapteyn's Star Anna Bortle,1 Hallie Fausey,1 Jinbiao Ji,1 Sarah Dodson-Robinson,1 Victor Ramirez Delgado,1 and John Gizis1 1University of Delaware Department of Physics and Astronomy 217 Sharp Lab Newark, DE 19716 USA ABSTRACT Radial-velocity (RV) planet searches are often polluted by signals caused by gas motion at the star's surface. Stellar activity can mimic or mask changes in the RVs caused by orbiting planets, resulting in false positives or missed detections. Here we use Gaussian Process (GP) regression to disentangle the contradictory reports of planets vs. rotation artifacts in Kapteyn's star (Anglada-Escud´eet al. 2014; Robertson et al. 2015a; Anglada-Escud´eet al. 2016). To model rotation, we use joint quasi-periodic kernels for the RV and Hα signals, requiring that their periods and correlation timescales be the same. We find that the rotation period of Kapteyn's star is 125 days, while the characteristic active-region lifetime is 694 days. Adding a planet to the RV model produces a best-fit orbital period of 100 years, or 10 times the observing time baseline, indicating that the observed RVs are best explained by star rotation only. We also find no significant periodic signals in residual RV data sets constructed by subtracting off realizations of the best-fit rotation model and conclude that both previously reported \planets" are artifacts of the star's rotation and activity. Our results highlight the pitfalls of using sinusoids to model quasi-periodic rotation signals. -
Bibliography of Refereed Papers: Roger L
Bibliography of refereed papers: Roger L. Davies 203 refereed papers, >24,000 citations, h=75 62 papers >100 citations; 13 papers >500 citations and one has more than 1000 citations. [203] Francesco D'Eugenio, Matthew Colless, Nicholas Scott, Arjen van der Wel, Roger L. Davies, Jesse van de Sande, Sarah M. Sweet, Sree Oh, Brent Groves, Rob Sharp, Matt S. Owers, Joss Bland-Hawthorn, Scott M. Croom, Sarah Brough, Julia J. Bryant, Michael Goodwin, Jon S. Lawrence, Nuria P. F. Lorente, and Samuel N. Richards. The SAMI Galaxy Survey: stellar population and structural trends across the Fundamental Plane. MNRAS, April 2021. [202] Scott M. Croom, Matt S. Owers, Nicholas Scott, Henry Poetrodjojo, Brent Groves, Jesse van de Sande, Tania M. Barone, Luca Cortese, Francesco D'Eugenio, Joss Bland-Hawthorn, Julia Bryant, Sree Oh, Sarah Brough, James Agostino, Sarah Casura, Barbara Catinella, Matthew Colless, Gerald Cecil, Roger L. Davies, Michael J. Drinkwater, Simon P. Driver, Ignacio Ferreras, Caroline Foster, Amelia Fraser-McKelvie, Jon Lawrence, Sarah K. Leslie, Jochen Liske, Angel´ R. L´opez-S´anchez, Nuria P. F. Lorente, Rebecca McElroy, Anne M. Medling, Danail Obreschkow, Samuel N. Richards, Rob Sharp, Sarah M. Sweet, Dan S. Taranu, Edward N. Taylor, Edoardo Tescari, Adam D. Thomas, James Tocknell, and Sam P. Vaughan. The SAMI Galaxy Survey: the third and final data release. MNRAS, February 2021. [201] Romina Ahumada and others. The 16th Data Release of the Sloan Digital Sky Surveys: First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra. ApJS, 249(1):3, July 2020. [200] S. -
Viability: a Priority Criterion for the Mitigation of Climate Change and Other Complex Socio-Ecological Issues
ARTICLE .77 Viability: A Priority Criterion for the Mitigation of Climate Change and other Complex Socio-Ecological Issues Graeme Taylor Griffith University Australia At present many researchers are exploring ways to improve the resilience of the global system, prevent catastrophic failure, and support the transition to a sustainable global system. This paper makes two interlinked proposals for developing better—and more credible—tools for modeling critical global issues and identifying and managing threats. First, proven risk management methods from other fields can be usefully applied to the assessment and mitigation of large, complex socio- ecological problems. Second, using viability as the priority criterion for the design of our models will not only highlight systemic threats, but also help us develop constructive interventions. socio-ecological, risk management, viability, modeling, non-linear, systems, safety, critical, causal diagrams, Bayesian networks The need for new models and methods Critical global problems like climate change, growing shortages of essential resources (such as water, food, energy and critical minerals) and the loss of biodiversity are getting worse. Many experts (Bierbaum et al., 2007) believe that humanity’s greatest challenge is to find ways to keep these problems from becoming catastrophic. Attention is increasingly focusing on risk assessment and management. Christopher Field, co-chair of the 2014 Intergovernmental Panel on Climate Change (IPCC) report on the impacts of rising temperatures, states: “The IPCC has transitioned to what I consider to be a full and rich recognition that the climate change problem is about managing risk” (Reuters, 2013). Awareness is growing also that better methods are needed to assess global risks and ensuring desirable outcomes. -
1 Exploring the Cosmos: the Rhetoric of Successful
EXPLORING THE COSMOS: THE RHETORIC OF SUCCESSFUL SCIENCE TELEVISION By ALEXANDREA MATTHEWS A THESIS PRESENTED TO THE GRADUATE SCHOOL OF THE UNIVERSITY OF FLORIDA IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF MASTER OF ARTS IN MASS COMMUNICATION UNIVERSITY OF FLORIDA 2015 1 © 2015 Alexandrea Matthews 2 To my mom, Dina Matthews, for the never-ending love, encouragement, and support 3 ACKNOWLEDGEMENTS I thank my chair, Dr. Debbie Treise, who not only guided me through my thesis but my entire graduate school experience. She has been patient and always accommodating, answering my many questions by e-mail almost immediately, even on weekends, and always found time for me despite her busy schedule. Through the research, coding, and analysis, she has always offered me invaluable insight and editing. I could not be more grateful to have had such a caring, supportive, and experienced thesis chair, advisor, and professor. Thank you for always going above and beyond in these roles. I also thank my other two committee members, Dr. Johanna Cleary and Dr. Elizabeth Lada. They have been supportive and enthusiastic about my research from the beginning and have offered me guidance that really shaped my methodology and research. Dr. Cleary gave me insight from her expertise in telecommunications and offered many great suggestions. Dr. Lada helped me from her expertise in astronomy, as both a committee member and a professor, who gave me the knowledge to approach my thesis from a more informed perspective. I am so thankful to have had such an experienced, diverse committee which could offer me guidance from multiple areas. -
Exoplanet.Eu Catalog Page 1 Star Distance Star Name Star Mass
exoplanet.eu_catalog star_distance star_name star_mass Planet name mass 1.3 Proxima Centauri 0.120 Proxima Cen b 0.004 1.3 alpha Cen B 0.934 alf Cen B b 0.004 2.3 WISE 0855-0714 WISE 0855-0714 6.000 2.6 Lalande 21185 0.460 Lalande 21185 b 0.012 3.2 eps Eridani 0.830 eps Eridani b 3.090 3.4 Ross 128 0.168 Ross 128 b 0.004 3.6 GJ 15 A 0.375 GJ 15 A b 0.017 3.6 YZ Cet 0.130 YZ Cet d 0.004 3.6 YZ Cet 0.130 YZ Cet c 0.003 3.6 YZ Cet 0.130 YZ Cet b 0.002 3.6 eps Ind A 0.762 eps Ind A b 2.710 3.7 tau Cet 0.783 tau Cet e 0.012 3.7 tau Cet 0.783 tau Cet f 0.012 3.7 tau Cet 0.783 tau Cet h 0.006 3.7 tau Cet 0.783 tau Cet g 0.006 3.8 GJ 273 0.290 GJ 273 b 0.009 3.8 GJ 273 0.290 GJ 273 c 0.004 3.9 Kapteyn's 0.281 Kapteyn's c 0.022 3.9 Kapteyn's 0.281 Kapteyn's b 0.015 4.3 Wolf 1061 0.250 Wolf 1061 d 0.024 4.3 Wolf 1061 0.250 Wolf 1061 c 0.011 4.3 Wolf 1061 0.250 Wolf 1061 b 0.006 4.5 GJ 687 0.413 GJ 687 b 0.058 4.5 GJ 674 0.350 GJ 674 b 0.040 4.7 GJ 876 0.334 GJ 876 b 1.938 4.7 GJ 876 0.334 GJ 876 c 0.856 4.7 GJ 876 0.334 GJ 876 e 0.045 4.7 GJ 876 0.334 GJ 876 d 0.022 4.9 GJ 832 0.450 GJ 832 b 0.689 4.9 GJ 832 0.450 GJ 832 c 0.016 5.9 GJ 570 ABC 0.802 GJ 570 D 42.500 6.0 SIMP0136+0933 SIMP0136+0933 12.700 6.1 HD 20794 0.813 HD 20794 e 0.015 6.1 HD 20794 0.813 HD 20794 d 0.011 6.1 HD 20794 0.813 HD 20794 b 0.009 6.2 GJ 581 0.310 GJ 581 b 0.050 6.2 GJ 581 0.310 GJ 581 c 0.017 6.2 GJ 581 0.310 GJ 581 e 0.006 6.5 GJ 625 0.300 GJ 625 b 0.010 6.6 HD 219134 HD 219134 h 0.280 6.6 HD 219134 HD 219134 e 0.200 6.6 HD 219134 HD 219134 d 0.067 6.6 HD 219134 HD