SARA SEAGER Physics and Planetary Science, Massachusetts Institute of Technology, Cambridge
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Guest Editorial: My Formative Years with the Rasc by Sara Seager I First Learned About Astronomy As a Small Child
INTRODUCTION 9 GUEST EDITORIAL: MY FORMATIVE YEARS WITH THE RASC BY SARA SEAGER I first learned about astronomy as a small child. One of my first memories is looking through a telescope at the Moon. I was completely stunned by what I saw. The Moon— huge and filled with craters—was a world in and of itself. I was with my father, at a star party hosted by the RASC. Later, when I was 10 years old and on my first camping trip, I remember awakening late one night, stepping outside the tent, and looking up. Stars—millions of them it seemed—filled the entire sky and took my breath away. As a teenager in the late 1980s, I joined the RASC Toronto Centre and deter- minedly attended the bimonthly Friday night meetings held in what was then the Planetarium building. Much of the information went over my head, but I can still clearly remember the excitement of the group whenever a visiting professor presented on a novel topic. An RASC member offered a one-semester evening class on astron- omy, and we were able to use the planetarium to learn about the night sky. The RASC events were a highlight of my high school and undergraduate years. While majoring in math and physics at the University of Toronto, I was thrilled to intern for two summers at the David Dunlap Observatory (DDO). I carried out an observing program of variable stars (including Polaris, the North Star), using the 61-cm (24″) and 48-cm (19″) telescopes atop the DDO’s administration building for simultaneous photometry of the target and comparison stars. -
Me Gustaría Dirigir Una Misión 'Starshade' Para Encontrar Un Gemelo De La Tierra
CIENCIAS SARA SEAGER, PROFESORA DE FÍSICA Y CIENCIA PLANETARIA EN EL MIT “Me gustaría dirigir una misión ‘starshade’ para encontrar un gemelo de la Tierra” Esta astrofísica del Instituto Tecnológico de Massachusetts (EE UU) está empeñada en observar un planeta extrasolar parecido al nuestro y, para poderlo ver, su sueño es desplegar un enorme ‘girasol’ en el espacio que oculte la cegadora luz de su estrella anfitriona. Es una de las aventuras en las que está embarcada y que cuenta en su último libro, Las luces más diminutas del universo, una historia de amor, dolor y exoplanetas. Enrique Sacristán 30/7/2021 08:30 CEST Sara Seager y uno de los pósteres de exoplanetas (facilitados por el Jet Propulsion Laboratory) que adornan el pasillo de su despacho en el Instituto Tecnológico de Massachusetts. / MIT/JPL- NASA Con tan solo diez años quedó deslumbrada por el cielo estrellado durante una acampada, una experiencia que recomienda a todo el mundo: “Este año la lluvia de meteoros de las perseidas, alrededor del 12 de agosto, cae cerca de una luna nueva, por lo que el cielo estará especialmente oscuro y habrá buenas condiciones para observar las estrellas fugaces”, nos adelanta la astrofísica Sara Seager. Nació en julio de 1971 en Toronto (Canadá) y hoy es una experta mundial en la búsqueda de exoplanetas, en especial los similares a la Tierra y con CIENCIAS indicios de vida. Se graduó en su ciudad natal y se doctoró en Harvard; luego pasó por el Instituto de Estudios Avanzados en Princeton y el Instituto Carnegie de Washington; hasta que en 2007 se asentó como profesora en el Instituto Tecnológico de Massachusetts (MIT). -
Universidade De São Paulo Instituto De Astronomia E Geofisica Mestrado Profissional Em Ensino De Astronomia
UNIVERSIDADE DE SÃO PAULO INSTITUTO DE ASTRONOMIA E GEOFISICA MESTRADO PROFISSIONAL EM ENSINO DE ASTRONOMIA JOSÉ IVAN SPINARDI ELABORAÇÃO DE UMA SEQUÊNCIA DIDÁTICA EM ASTROBIOLOGIA PARA O ENSINO FUNDAMENTAL 2 SÃO PAULO 2017 “Versão corrigida. O original encontra-se disponível na Unidade.” JOSÉ IVAN SPINARDI ELABORAÇÃO DE UMA SEQUÊNCIA DIDÁTICA EM ASTROBIOLOGIA PARA O ENSINO FUNDAMENTAL 2 Dissertação apresentada ao Instituto de Astronomia e Geofísica da Universidade de São Paulo obtenção do título de mestre em ensino de Astronomia. Área de concentração: Ensino de Astronomia. Orientador: Prof. Dr. Amâncio Cesar Santos Friaça SÃO PAULO 2017 “O materialismo dialético ensina que a matéria nunca permanece em repouso, mas, pelo contrário, está em constante movimento, desenvolve-se e, evoluindo, eleva-se a níveis cada vez mais altos e adquire formas de movimento cada vez mais complexas. Ao elevar-se de um degrau ao outro, a matéria adquire novos atributos. Um deles é a vida cujo surgimento marca uma etapa, um escalão determinado do desenvolvimento histórico da matéria. Durante o decorrer desse desenvolvimento é que surgiu a vida, como uma nova qualidade.” Alexander Oparin “Se não existe vida fora da Terra, então o Universo é um grande desperdício de espaço” Carl Sagan “Há vidas sim em outros planetas, porém, não desenvolvidas.” Um aluno da 8ª série A. AGRADECIMENTOS À minha família. Ao meu sobrinho Luiz Lucas pelo suporte em informática. Às educadoras Erika Reyes Molina e Giovanni Scataglia Botelho Paz, pelo apoio e confiança. À Professora Maria Helena Pereira, da EMEF João Guimaraes Rosa, pela cessão de suas aulas para a aplicação das atividades. -
Hunting for Transits of Super-Earth GJ 581E 2 June 2011
Hunting for transits of Super-Earth GJ 581e 2 June 2011 terrestrial-mass exoplanet in the habitable zone". They found that, despite the small amount of light Gliese 581d receives from its star, a carbon dioxide atmosphere could maintain temperatures above the freezing point of water at the surface. If the orbital inclination of a planetary system is just right, then one or more planets may be observed to cross (transit) the disk of the star, dimming the brightness of the star by a tiny fraction. By measuring this effect, it is possible to derive the Artist's concept of Gliese 581 e. Image: size of the planet. JohnVanVliet/Wikipedia. If Gliese 581e transits its host star, then it must have a radius smaller than 1.4 times that of the Earth since a larger planet would have been (PhysOrg.com) -- An international team of detected by MOST. In terms of composition, this astronomers has ruled out transits of a water-rich suggests that planet e does not have a hydrogen or or hydrogen-helium atmosphere planet for Gliese helium atmosphere, nor does it contain more than 581e. The host star itself is relatively quiet which 25% water. Therefore it must be a solid rocky means good news for the potential habitability of at planet. However, if the planet does not transit, its least one of its planets. size and therefore its composition cannot be constrained, but the inclination of its orbit can. The study was conducted using observations acquired by MOST (Microvariability & Oscillations "Although transits were not detected for Gliese of STars), Canada's only space telescope. -
Exoplanet Exploration Collaboration Initiative TP Exoplanets Final Report
EXO Exoplanet Exploration Collaboration Initiative TP Exoplanets Final Report Ca Ca Ca H Ca Fe Fe Fe H Fe Mg Fe Na O2 H O2 The cover shows the transit of an Earth like planet passing in front of a Sun like star. When a planet transits its star in this way, it is possible to see through its thin layer of atmosphere and measure its spectrum. The lines at the bottom of the page show the absorption spectrum of the Earth in front of the Sun, the signature of life as we know it. Seeing our Earth as just one possibly habitable planet among many billions fundamentally changes the perception of our place among the stars. "The 2014 Space Studies Program of the International Space University was hosted by the École de technologie supérieure (ÉTS) and the École des Hautes études commerciales (HEC), Montréal, Québec, Canada." While all care has been taken in the preparation of this report, ISU does not take any responsibility for the accuracy of its content. Electronic copies of the Final Report and the Executive Summary can be downloaded from the ISU Library website at http://isulibrary.isunet.edu/ International Space University Strasbourg Central Campus Parc d’Innovation 1 rue Jean-Dominique Cassini 67400 Illkirch-Graffenstaden Tel +33 (0)3 88 65 54 30 Fax +33 (0)3 88 65 54 47 e-mail: [email protected] website: www.isunet.edu France Unless otherwise credited, figures and images were created by TP Exoplanets. Exoplanets Final Report Page i ACKNOWLEDGEMENTS The International Space University Summer Session Program 2014 and the work on the -
The Search for Worlds Like Our Own
ASTROBIOLOGY Volume 10, Number 1, 2010 Education Articles ª Mary Ann Liebert, Inc. DOI: 10.1089=ast.2009.0380 The Search for Worlds Like Our Own Malcolm Fridlund,1 Carlos Eiroa,2 Thomas Henning,3 Tom Herbst,3 Helmut Lammer,4 Alain Le´ger,5 Rene´ Liseau,6 Francesco Paresce,7 Alan Penny,8,9 Andreas Quirrenbach,10 Huub Ro¨ttgering,11 Franck Selsis,12 Glenn J. White,9,13 Olivier Absil,14,15 Denis Defre`re,15 C. Hanot,15 Daphne Stam,16 Jean Schneider,17 Giovanna Tinetti,18 Anders Karlsson,19 Phillipe Gondoin,19 Roland den Hartog,19 Luigi D’Arcio,19 Anna-Maria Stankov,19 Mikael Kilter,19 Christian Erd,19 Charles Beichman,20 Daniel Coulter,21 William Danchi,22 Michael Devirian,21 Kenneth J. Johnston,23 Peter Lawson,21 Oliver P. Lay,21 Jonathan Lunine,24 and Lisa Kaltenegger25 Abstract The direct detection of Earth-like exoplanets orbiting nearby stars and the characterization of such planets— particularly, their evolution, their atmospheres, and their ability to host life—constitute a significant problem. The quest for other worlds as abodes of life has been one of mankind’s great questions for several millennia. For instance, as stated by Epicurus *300 BC: ‘‘Other worlds, with plants and other living things, some of them similar and some of them different from ours, must exist.’’ Demokritos from Abdera (460–370 BC), the man who invented the concept of indivisible small parts—atoms—also held the belief that other worlds exist around the stars and that some of these worlds may be inhabited by life-forms. -
Professor Sara Seager Massachusetts Institute of Technology
Professor Sara Seager Massachusetts Institute of Technology Address: Department of Earth Atmospheric and Planetary Science Building 54 Room 1718 Massachusetts Institute of Technology 77 Massachusetts Avenue Cambridge, MA, USA 02139 Phone: (617) 253-6779 (direct) E-mail: [email protected] Citizenship: US citizen since 7/20/2010 Birthdate: 7/21/1971 Professional History 1/2011–present: Massachusetts Institute of Technology, Cambridge, MA USA • Class of 1941 Professor (1/2012–present) • Professor of Planetary Science (7/2010–present) • Professor of Physics (7/2010–present) • Professor of Aeronautical and Astronautical Engineering (7/2017–present) 1/2007–12/2011: Massachusetts Institute of Technology, Cambridge, MA USA • Ellen Swallow Richards Professorship (1/2007–12/2011) • Associate Professor of Planetary Science (1/2007–6/2010) • Associate Professor of Physics (7/2007–6/2010) • Chair of Planetary Group in the Dept. of Earth, Atmospheric, and Planetary Sciences (2007–2015) 08/2002–12/2006: Carnegie Institution of Washington, Washington, DC, USA • Senior Research Staff Member 09/1999–07/2002: Institute for Advanced Study, Princeton NJ • Long Term Member (02/2001–07/2002) • Short Term Member (09/1999–02/2001) • Keck Fellow Educational History 1994–1999 Ph.D. “Extrasolar Planets Under Strong Stellar Irradiation” Department of Astronomy, Harvard University, MA, USA 1990–1994 B.Sc. in Mathematics and Physics University of Toronto, Canada NSERC Science and Technology Fellowship (1990–1994) Awards and Distinctions Academic Awards and Distinctions 2018 American Philosophical Society Member 2018 American Academy of Arts and Sciences Member 2015 Honorary PhD, University of British Columbia 2015 National Academy of Sciences Member 2013 MacArthur Fellow 2012 Raymond and Beverly Sackler Prize in the Physical Sciences 2012 American Association for the Advancement of Science Fellow 2007 Helen B. -
Esocast Episode 6: Lightest Exoplanet Found 00:00 [Visual Starts]
ESOcast Episode 6: Lightest exoplanet found 00:00 [Visual starts] [Narrator] A: Artist’s impression of Gliese 581e 1. The holy grail of current exoplanet research is the detection of a rocky, Earth-like planet in the ‘habitable zone,’ region around the host star with the right conditions for water to be liquid on their surface. The latest result from the European Southern Observatory comes closer than ever to attaining these goals. 00:25 ESOcast intro This is the ESOcast! Cutting-edge science and life behind the scenes of ESO, the European Southern Observatory. Exploring the Universe’s ultimate frontier with our host Dr. J, a.k.a. Dr. Joe Liske. 00:42 [Dr. J] 2. Hello and welcome to another episode of the ESOcast. This time we have some very exciting A: Artist’s impression of Gliese 581e news for you, it’s another major ESO discovery. We’d like to tell you about the discovery of the B: Artist’s impression of Gliese 581d smallest, or rather lightest, and possibly most Earth- like planet so far discovered outside of our own Solar System. We’d also like to report on yet another planet within the same system that has now been shown to lie within the habitable zone of its parent star, meaning that it could host liquid water and possibly even life. 01:13 [Narrator] 3. Gliese 581 is a seemingly inconspicuous red C: Zoom-in on Gliese 581e dwarf star located 20.5 light-years away in the constellation Libra, or “the Scales”. It is among the 100 closest stars to us and weighs only one third the mass of the Sun. -
The Hitchhiker's Guide to the Drake Equation
The Hitchhiker’s Guide to the Drake Equation: Past, Present, and Future Dr. Kaitlin Rasmussen (she/they) ExoExplorers Series — June 11, 2021 University of Michigan | Heising-Simons Foundation THE BIG QUESTION: ARE WE ALONE? THE BIG ANSWER: THE DRAKE EQUATION THE BIG ANSWER: THE DRAKE EQUATION N = NUMBER OF ADVANCED CIVILIZATIONS IN THE MILKY WAY THE BIG ANSWER: THE DRAKE EQUATION R*= STAR FORMATION RATE THE BIG ANSWER: THE DRAKE EQUATION f_p = PLANET FORMATION RATE THE BIG ANSWER: THE DRAKE EQUATION n_e = NUMBER OF HABITABLE WORLDS PER STAR THE BIG ANSWER: THE DRAKE EQUATION f_l = NUMBER OF HABITABLE WORLDS ON WHICH LIFE APPEARS THE BIG ANSWER: THE DRAKE EQUATION f_i = NUMBER OF INTELLIGENT LIFE-BEARING WORLDS THE BIG ANSWER: THE DRAKE EQUATION f_c = NUMBER OF INTELLIGENT, TECHNOLOGICAL CIVILIZATIONS THE BIG ANSWER: THE DRAKE EQUATION L = AVERAGE LENGTH OF A TECHNOLOGICALLY CAPABLE CIVILIZATION HOW CAN WE CONSTRAIN THIS? HOW CAN WE CONSTRAIN THIS? PAST: WHEN PRESENT: HOW FUTURE: HOW DID PLANET CAN WE BETTER WILL WE BE FORMATION CONSTRAIN ABLE TO TELL BEGIN IN THE PLANETARY AN EXO-VENUS UNIVERSE? ATMOSPHERES? FROM AN EXO-EARTH? HOW CAN WE CONSTRAIN THIS? PAST: WHEN DID PLANET FORMATION BEGIN IN THE UNIVERSE? THE SEARCH FOR EXOPLANETS AROUND METAL-POOR (ANCIENT) STARS WITH T(r)ESS (SEAMSTRESS) Stars began to form soon after the Big Bang—but when did stars begin to have planets? ➔ What is the minimum metallicity for a planet to form? ➔ What kinds of planetary systems were they? ➔ Can an ancient star support life? WHERE DO WE BEGIN? 1. A large-scale transit survey 2. -
De Natura Rerum: Exoplanets and Exoearths Pierre Léna Que L’Homme Contemple La Nature Dans Sa Haute Et Pleine Majesté… Que La Terre Lui Paraisse Comme Un Point
De Natura Rerum: Exoplanets and ExoEarths Pierre Léna Que l’homme contemple la nature dans sa haute et pleine majesté… que la Terre lui paraisse comme un point. Blaise Pascal (1623-1662) Pensées Introduction At the 2004 Plenary Session of the Pontifical Academy of Sciences on Paths of Discovery, I presented a paper with the title The case of exoplanets [Léna 2005]. It was then close to the 10th anniversary of the discovery of the first exoplanet in 1995. There is no point in repeating here this paper. But in the last decade, the discoveries on this subject have been so considerable that, the 20th anniversary coming, it is worth addressing the topic again. During the first decade 1995-2004, only 133 exoplanets had been discovered by an indirect method, and the first direct image of an exoplanet was not even confirmed. Today in our Galaxy containing the Earth, statistics begin to indicate that on average every star has a planet, which means over 100 billions of exoplanets for this galaxy alone, of which nearly 2000 are now identified and more or less characterized. How does the subject of exoplanets relate with the Evolving concepts of nature, the title of this Plenary Session? In the 2005 paper, I recalled the long history of a quest which began metaphysically with Democritus, was disputed theologically during the Middle Age, provided phantasies to poets and writers, until it emerged as a scientific problem, to be addressed with the investigative methods of astronomy during the 19th century. Along this path, Giordano Bruno, who expressed ideas close to Lucretius’s ones, was condemned to the fire for multiple reasons, including this one. -
Extrasolar Planets
Extrasolar Planets Dieter Schmitt Lecture Max Planck Institute for Introduction to Solar System Research Solar System Physics Katlenburg-Lindau Uni Göttingen, 8 June 2009 Outline • Historical Overview • Detection Methods • Planet Statistics • Formation of Planets • Physical Properties • Habitability Historical overview • 1989: planet / brown dwarf orbiting HD 114762 (Latham et al.) • 1992: two planets orbiting pulsar PSR B1257+12 (Wolszczan & Frail) • 1995: first planet around a solar-like star 51 Peg b (Mayor & Queloz) • 1999: first multiple planetary system with three planets Ups And (Edgar et al.) • 2000: first planet by transit method HD 209458 b (Charbonneau et al.) • 2001: atmosphere of HD 209458 b (Charbonneau et al.) • 2002: astrometry applied to Gliese 876 (Benedict et al.) • 2005: first planet by direct imaging GQ Lupi b (Neuhäuser et al.) • 2006: Earth-like planet by gravitational microlensing (Beaulieu et al.) • 2007: Gliese 581d, small exoplanet near habitability zone (Selsis et al.) • 2009: Gliese 581e, smallest exoplanet with 1.9 Earth masses (Mayor et al.) • As of 7 June 2009: 349 exoplanets in 296 systems (25 systems with 2 planets, 9 with 3, 2 with 4 and 1 with 5) www.exoplanet.eu Our Solar System 1047 MJ 0.39 AU 0.00314 MJ 1 MJ 0.30 MJ 0.046 MJ 0.054 MJ 1 AU 5.2 AU 9.6 AU 19 AU 30 AU 1 yr 11.9 yr 29.5 yr 84 yr 165 yr Definition Planet IAU 2006: • in orbit around the Sun / star • nearly spherical shape / sufficient mass for hydrostatic equilib. • cleared neighbourhood around its orbit Pluto: dwarf planet, as Ceres Brown -
Extrasolar Planets
Extrasolar Planets Dieter Schmitt Lecture Max Planck Institute for Introduction to Solar System Research Solar System Physics KatlenburgLindau Uni Göttingen, 8 June 2009 Outline • Historical Overview • Detection Methods • Planet Statistics • Formation of Planets • Physical Properties • Habitability Historical overview • 1989: planet / brown dwarf orbiting HD 114762 (Latham et al.) • 1992: two planets orbiting pulsar PSR B1257+12 (Wolszczan & Frail) • 1995: first planet around a solarlike star 51 Peg b (Mayor & Queloz) • 1999: first multiple planetary system with three planets Ups And (Edgar et al.) • 2000: first planet by transit method HD 209458 b (Charbonneau et al.) • 2001: atmosphere of HD 209458 b (Charbonneau et al.) • 2002: astrometry applied to Gliese 876 (Benedict et al.) • 2005: first planet by direct imaging GQ Lupi b (Neuhäuser et al.) • 2006: Earthlike planet by gravitational microlensing (Beaulieu et al.) • 2007: Gliese 581d, small exoplanet near habitability zone (Selsis et al.) • 2009: Gliese 581e, smallest exoplanet with 1.9 Earth masses (Mayor et al.) • As of 7 June 2009: 349 exoplanets in 296 systems (25 systems with 2 planets, 9 with 3, 2 with 4 and 1 with 5) www.exoplanet.eu Our Solar System 1047 MJ 0.39 AU 0.00314 MJ 1 MJ 0.30 MJ 0.046 MJ 0.054 MJ 1 AU 5.2 AU 9.6 AU 19 AU 30 AU 1 yr 11.9 yr 29.5 yr 84 yr 165 yr Definition Planet IAU 2006: • in orbit around the Sun / star • nearly spherical shape / sufficient mass for hydrostatic equilib. • cleared neighbourhood around its orbit Pluto: dwarf planet, as Ceres Brown