Can Be Set In
Total Page:16
File Type:pdf, Size:1020Kb

Load more
Recommended publications
-
Towards a Classification System of Terrestrial Planets
7RZDUGVD&ODVVL¿FDWLRQ6\VWHPRI7HUUHVWULDO3ODQHWV Charles H. Lineweaver and Jose A. Robles Planetary Science Institute, Research School of Astronomy and Astrophysics, Research School of Earth Sciences, The Australian National University, Canberra ACT 0200 Australia. Abstract: The focus of extrasolar planet searches has become the detection of habitable terrestrial planets. Planetary mass and orbit have large and obvious effects on habitability. Since the chemical compositions of terrestrial planets also play an important role in habitability, we propose the creation RIDFODVVL¿FDWLRQV\VWHPIRU(DUWKOLNHSODQHWVEDVHGRQWKHDEXQGDQFHVRIHOHPHQWVPRVWLPSRUWDQW IRUKDELWDELOLW\:HGHVFULEHWKHPHWKRGRORJ\IRUWKHFUHDWLRQRIVXFKDFODVVL¿FDWLRQV\VWHPEDVHG on the observed chemical abundances of stars. Keywords: Terrestrial planet formation, Solar system, chemical composition Introduction %DFNJURXQGIRUWKH&UHDWLRQRID3ODQHW&ODVVL¿FDWLRQ6\VWHP 6FLHQWL¿FXQGHUVWDQGLQJRIDJURXSRIQHZREMHFWVEHJLQVZLWKDXVHIXOFODVVL¿FDWLRQVFKHPH)RU a century astronomers have relied on the Hertzsprung-Russell diagram to classify stars according to their colour and magnitude. In the Hertzsprung-Russell diagram the Sun is seen to be part of the PDLQVHTXHQFHRIK\GURJHQEXUQLQJVWDUV$QDQDORJRXVFODVVL¿FDWLRQV\VWHPIRUSODQHWVKDV\HWWR emerge. In our Solar System we have: small rocky planets close to the Sun (Mercury, Venus, Earth, Mars, asteroids), the gas giants (Jupiter and Saturn), then the ice giants (Uranus and Neptune) and ¿QDOO\DVZDUPRIVPDOOGLUW\VQRZEDOOV 3OXWRDQGFRPSDQ\ 7KLVUXGLPHQWDU\RUELWDOUDGLXV -
The Search for Another Earth – Part II
GENERAL ARTICLE The Search for Another Earth – Part II Sujan Sengupta In the first part, we discussed the various methods for the detection of planets outside the solar system known as the exoplanets. In this part, we will describe various kinds of exoplanets. The habitable planets discovered so far and the present status of our search for a habitable planet similar to the Earth will also be discussed. Sujan Sengupta is an 1. Introduction astrophysicist at Indian Institute of Astrophysics, Bengaluru. He works on the The first confirmed exoplanet around a solar type of star, 51 Pe- detection, characterisation 1 gasi b was discovered in 1995 using the radial velocity method. and habitability of extra-solar Subsequently, a large number of exoplanets were discovered by planets and extra-solar this method, and a few were discovered using transit and gravi- moons. tational lensing methods. Ground-based telescopes were used for these discoveries and the search region was confined to about 300 light-years from the Earth. On December 27, 2006, the European Space Agency launched 1The movement of the star a space telescope called CoRoT (Convection, Rotation and plan- towards the observer due to etary Transits) and on March 6, 2009, NASA launched another the gravitational effect of the space telescope called Kepler2 to hunt for exoplanets. Conse- planet. See Sujan Sengupta, The Search for Another Earth, quently, the search extended to about 3000 light-years. Both Resonance, Vol.21, No.7, these telescopes used the transit method in order to detect exo- pp.641–652, 2016. planets. Although Kepler’s field of view was only 105 square de- grees along the Cygnus arm of the Milky Way Galaxy, it detected a whooping 2326 exoplanets out of a total 3493 discovered till 2Kepler Telescope has a pri- date. -
The 29Th Annual Meeting the 29Th Annual Meeting of the Society Took Place on April 17Th, 2016 Program and Abstracts Program
The 29th annual meeting The 29th annual meeting of the society took place on April 17th, 2016 Program and Abstracts Program: Program of the 29th annual meeting Time Lecturer Lecture Title 8:45- Refreshments & Gathering 9:05 Session 1 -Astrobiology (Doron Lancet, Chair; Amri Wandel, Organizer) 9:05- Gonen Ashkenasy Opening Remarks 9:15 (BGU) 9:15- Ravit Helled Methane-Rich Planets and the Characterization of Exoplanets 9:45 (TAU) 9:45- Sohan Jheeta (NoR Formation of Glycolaldehyde (HOCH2CHO) from Pure 10:10 HGT, LUCA) Methanol in Astrophysical Ice Analogues 10:10- Joseph Is Liquid Water Essential for Life? A Reassessment 10:35 Gale (HUJI) 10:35- Coffee break 11:00 Session 2 - Evolution (Addy Pross, Chair) 11:00- Robert Pascal Identifying the Kinetic, Thermodynamic and Chemical 11:40 (CNRS Conditions for Stability and Complexity in Living Systems Montpellier) 11:40- Omer Markovitch Predicting Proto-Species Emergence in Complex Networks 12:05 (Newcastle) 12:05- Amir Aharoni Engineering a Species Barrier in Yeast 12:30 (BGU) 12:30- Jayanta Nanda Spontaneous Evolution of β-Sheet Forming Self Replicating 12:55 (BGU) Peptides 12:55- Lunch 14:05 Session 3 - Origins of Order and Complexity (Gonen Ashkenasy, Chair; Tal Mor, Organizer) 14:05- Prof. Zvi HaCohen, Greetings 14:15 Rector (BGU) 14:15- Doron Composomics: a Common Biotic Thread 14:45 Lancet (WIS) 14:45- Avshalom Elitzur Living State Physics: Does Life's Uniqueness Elude Scientific 15:10 (IYAR) Definition? 15:10- Tal Mor Origins of Translation: Speculations about the First and the 15:35 -
Kuchner, M. & Seager, S., Extrasolar Carbon Planets, Arxiv:Astro-Ph
Extrasolar Carbon Planets Marc J. Kuchner1 Princeton University Department of Astrophysical Sciences Peyton Hall, Princeton, NJ 08544 S. Seager Carnegie Institution of Washington, 5241 Broad Branch Rd. NW, Washington DC 20015 [email protected] ABSTRACT We suggest that some extrasolar planets . 60 ML will form substantially from silicon carbide and other carbon compounds. Pulsar planets and low-mass white dwarf planets are especially good candidate members of this new class of planets, but these objects could also conceivably form around stars like the Sun. This planet-formation pathway requires only a factor of two local enhancement of the protoplanetary disk’s C/O ratio above solar, a condition that pileups of carbonaceous grains may create in ordinary protoplanetary disks. Hot, Neptune- mass carbon planets should show a significant paucity of water vapor in their spectra compared to hot planets with solar abundances. Cooler, less massive carbon planets may show hydrocarbon-rich spectra and tar-covered surfaces. The high sublimation temperatures of diamond, SiC, and other carbon compounds could protect these planets from carbon depletion at high temperatures. arXiv:astro-ph/0504214v2 2 May 2005 Subject headings: astrobiology — planets and satellites, individual (Mercury, Jupiter) — planetary systems: formation — pulsars, individual (PSR 1257+12) — white dwarfs 1. INTRODUCTION The recent discoveries of Neptune-mass extrasolar planets by the radial velocity method (Santos et al. 2004; McArthur et al. 2004; Butler et al. 2004) and the rapid development 1Hubble Fellow –2– of new technologies to study the compositions of low-mass extrasolar planets (see, e.g., the review by Kuchner & Spergel 2003) have compelled several authors to consider planets with chemistries unlike those found in the solar system (Stevenson 2004) such as water planets (Kuchner 2003; Leger et al. -
Our Earth Is the Carbon Planet, Life Planet. Carbon Enables Life
Our Earth is The Carbon Planet, Life Planet. Carbon Enables Life Letter to the Editor & To all Honourable Members of Parliament Carbon is the universe’s fourth most abundant element after hydrogen, helium, oxygen. It’s one of the least abundant elements in Earth's crust. Carbon has three main forms: - Diamond - among hardest materials - Graphite - soft - Amorphous - non-crystalline, powdery. Carbon forms more compounds than any other element - almost ten million organic compounds, a tiny fraction of its possible compounds. Carbon is the chemical basis of all known life and present in all known life forms. Trees, animals, bacteria… Life on Earth was possible because of carbon, evolved with carbon and depends on carbon. In human bodies, after oxygen, carbon is the second most abundant element - 18.5%. Life cycles: carbon is the key component in biology, many vital processes such as photosynthesis and bodily processes (breathing, digestion) Carbon occurs naturally throughout the atmosphere, crust, oceans and life forms. Humans depend on carbon for food, energy, shelter, transport. The IPCC and governments falsely frame carbon as black pollution using: - language - ‘emissions’, ‘carbon pollution’, ‘fugitive emissions’; - costly, useless bureaucratic measurement ingraining carbon as pollution; - tax; - glossy advertisements misrepresenting carbon using sinister black animations and footage of third world industry; - schools indoctrinating children. Carbon is natural, essential and ‘green’. Carbon dioxide is invisible. We’re carbon. We need carbon. Carbon is not humanity’s enemy. It’s ‘a girl’s best friend’. Carbon is not pollution. It’s essential to life. The issue is not CO2. The issue is the IPCC. -
Does the Rapid Appearance of Life on Earth Suggest That Life Is Common in the Universe?
ASTROBIOLOGY Volume 2, Number 3, 2002 © Mary Ann Liebert, Inc. Does the Rapid Appearance of Life on Earth Suggest that Life Is Common in the Universe? CHARLES H. LINEWEAVER 1,2 and TAMARA M. DAVIS 1 ABSTRACT It is sometimes assumed that the rapidity of biogenesis on Earth suggests that life is common in the Universe. Here we critically examine the assumptions inherent in this if-life-evolved- rapidly-life-must-be-common argument. We use the observational constraints on the rapid- ity of biogenesis on Earth to infer the probability of biogenesis on terrestrial planets with the same unknown probability of biogenesis as the Earth. We find that on such planets, older than ,1 Gyr, the probability of biogenesis is .13% at the 95% confidence level. This quan- tifies an important term in the Drake Equation but does not necessarily mean that life is com- mon in the Universe. Key Words: Biogenesis—Drake Equation. Astrobiology 2, 293–304. THE BIOGENESIS LOTTERY duction–oxidation pairs are common (Nealson and Conrad, 1999). UCHOFCURRENTASTROBIOLOGICALRESEARCH Mis focused on learning more about the early It is difficult to translate this circumstantial ev- evolution of the Earth and about the origin of life. idence into an estimate of how common life is in We may be able to extrapolate and generalize our the Universe. Without definitive detections of ex- knowledge of how life formed here to how it traterrestrial life we can say very little about how might have formed elsewhere. Indirect evidence common it is or even whether it exists. Our exis- suggesting that life may be common in the Uni- tence on Earth can tell us little about how com- verse includes: mon life is in the Universe or about the proba- bility of biogenesis on a terrestrial planet because, Sun-like stars are common. -
The Drake Equation the Drake Equation, Which We Encountered in the Very First Lecture of This Class, Is a Way to Take the Questi
The Drake Equation The Drake equation, which we encountered in the very first lecture of this class, is a way to take the question “How many communicative civilizations are there currently in our galaxy?” and break it into several factors that we estimate as best we can. In this class we will go into detail about this equation. We will find that we now have a decent idea of the values of a couple of the factors, but that many are still guesswork. We’ll do our best to make our guesses informed. We will also discover that some people have reformulated the equation by adding a number of other factors they consider crucial to having technologically adept life. The remarkable and subtle effect of this is that, depending on how many factors you think appropriate, you can get the conclusions you want while appearing reasonable and conservative throughout. That is, if you think many civilizations exist, you can use the Drake equation to demonstrate this. If you think we are the only ones, you can get the equation to say that as well. With this in mind, we should approach the Drake equation as a way of framing our discussion as opposed to as a method of determining the answer rigorously. The equation itself and its factors The original form of the equation was written by Frank Drake in 1960 in preparation for a meeting in Green Bank, West Virginia. It says: ∗ N = R × fp × ne × fl × fi × fc × L . (1) Here: • N is the number of currently active, communicative civilizations in our galaxy. -
Nasa and the Search for Technosignatures
NASA AND THE SEARCH FOR TECHNOSIGNATURES A Report from the NASA Technosignatures Workshop NOVEMBER 28, 2018 NASA TECHNOSIGNATURES WORKSHOP REPORT CONTENTS 1 INTRODUCTION .................................................................................................................................................................... 1 What are Technosignatures? .................................................................................................................................... 2 What Are Good Technosignatures to Look For? ....................................................................................................... 2 Maturity of the Field ................................................................................................................................................... 5 Breadth of the Field ................................................................................................................................................... 5 Limitations of This Document .................................................................................................................................... 6 Authors of This Document ......................................................................................................................................... 6 2 EXISTING UPPER LIMITS ON TECHNOSIGNATURES ....................................................................................................... 9 Limits and the Limitations of Limits ........................................................................................................................... -
Drake's Equation
Drake’s equation: estimating the number of extraterrestrial civilizations in our galaxy Raphaëlle D. Haywood This activity was largely inspired from an outreach project developed by Exscitec members at Imperial College London, UK. Goals In this workshop, we estimate the number of communicating civilizations in our galaxy! In this first session you will go through the different ingredients required. You will make estimates for each of the variables using both results from recent scientific studies and your best guesses. Next week we will go over each variable in more detail -- make a note of any questions you may have so that we can discuss them. We will compare and discuss everyone’s estimates of N, and will discuss their implications for finding life as well as for the survival of our own species. Outline Estimating the number of extraterrestrial civilizations out there may at first seem like a daunting task, but in 1961 Prof. Frank Drake found a way to break this problem down into a series of much more manageable steps. This is neatly summarized in the following equation, where each of the variables relates to a specific topic: R⁎: Number of Sun-type stars that form each year in our galaxy fp: Fraction of Sun-type stars that host planets ne: Number of Earth-like planets per planetary system, so that fp x ne is the fraction of Sun-type stars that have Earth-like planets fl: Fraction of Earth-like planets where life develops fi: Fraction of life-bearing planets where intelligent life evolves fc: Fraction of planets hosting intelligent life where a communicative, technological civilization arises L: Lifetime (in years) of technologically-advanced, communicating civilizations To obtain N, we simply estimate each of these parameters separately and then we multiply them together. -
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. -
Mapping and Planetary Spatial Infrastructure Team
The Ol Doinyo Lengai volcano, Tanzania, as an analogue for Carbon Planets Jani Radebaugh, Rory Barnes, Jeff Keith Department of Geological Sciences, Brigham Young University, Department of Physics, University of Washington Field Analogues are Valuable • Knowledge of landforms on other planets is incomplete • Similar physics, materials can be found on Earth • Earth landscapes can yield important information about other planets MEDUSA FOSSE FORMATION, MARS DUNHUANG, CHINA, 40 N 93 E Field Analogues are Valuable • Knowledge of landforms on other planets is incomplete • Similar physics, materials can be found on Earth • Earth landscapes can yield important information about other planets TITAN Field Analogues are Valuable • Knowledge of landforms on other planets is incomplete • Similar physics, materials can be found on Earth • Earth landscapes can yield important information about other planets DUNHUANG, CHINA, 40 N 93 E Field Analogues are Valuable • Yardangs: Wind important, but also bedrock, rainfall, gravels LUT DESERT, IRAN Field Analogues of exoplanets?? • We’ve yet to even “see” an exoplanet • They are planetary surfaces worth studying as we do for our solar system TRAPPIST-1 Carbon Planets • Postulated to form in carbon-rich nebular environments (Seager and Kuchner 2005) • When C/O>0.8 in the disk (Bond et al. 2010) • May reach >75% carbon in the habitable zone! ARTIST LUYTEN Carbon Planets • Even in our solar system, carbon is enriched in certain locations • Mercury may have had graphite crust on magma ocean (Peplowski et al. 2016) Mercury MESSENGER M-dwarf Carbon Planets • Carbon planets orbiting M-dwarf stars could spend millions/billions of years closer than the habitable zone during pre-main-sequence (e.g. -
Carl Sagan 1934–1996
Carl Sagan 1934–1996 A Biographical Memoir by David Morrison ©2014 National Academy of Sciences. Any opinions expressed in this memoir are those of the author and do not necessarily reflect the views of the National Academy of Sciences. CARL SAGAN November 9, 1934–December 20, 1996 Awarded 1994 NAS Pubic Welfare Medal Carl Edward Sagan was a founder of the modern disci- plines of planetary science and exobiology (which studies the potential habitability of extraterrestrial environments for living things), and he was a brilliant educator who was able to inspire public interest in science. A visionary and a committed defender of rational scientific thinking, he transcended the usual categories of academia to become one of the world’s best-known scientists and a true celebrity. NASA Photo Courtesy of Sagan was propelled in his careers by a wealth of talent, By David Morrison a large share of good luck, and an intensely focused drive to succeed. His lifelong quests were to understand our plane- tary system, to search for life beyond Earth, and to communicate the thrill of scientific discovery to others. As an advisor to the National Aeronautics and Space Administration (NASA) and a member of the science teams for the Mariner, Viking, Voyager, and Galileo missions, he was a major player in the scientific exploration of the solar system. He was also a highly popular teacher, but his influence reached far beyond the classroom through his vivid popular writing and his mastery of the medium of television. The early years Born in 1934, Sagan grew up in a workingclass Jewish neighborhood of Brooklyn, New York, and attended public schools there and in Rahway, New Jersey.