Natural Intelligence and Anthropic Reasoning
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Lecture-29 (PDF)
Life in the Universe Orin Harris and Greg Anderson Department of Physics & Astronomy Northeastern Illinois University Spring 2021 c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 1 / 95 Overview Dating Rocks Life on Earth How Did Life Arise? Life in the Solar System Life Around Other Stars Interstellar Travel SETI Review c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 2 / 95 Dating Rocks Zircon Dating Sedimentary Grand Canyon Life on Earth How Did Life Arise? Life in the Solar System Life Around Dating Rocks Other Stars Interstellar Travel SETI Review c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 3 / 95 Zircon Dating Zircon, (ZrSiO4), minerals incorporate trace amounts of uranium but reject lead. Naturally occuring uranium: • U-238: 99.27% • U-235: 0.72% Decay chains: • 238U −→ 206Pb, τ =4.47 Gyrs. • 235U −→ 207Pb, τ = 704 Myrs. 1956, Clair Camron Patterson dated the Canyon Diablo meteorite: τ =4.55 Gyrs. c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 4 / 95 Dating Sedimentary Rocks • Relative ages: Deeper layers were deposited earlier • Absolute ages: Decay of radioactive isotopes old (deposited last) oldest (depositedolder first) c 2012-2021 G. Anderson., O. Harris Universe: Past, Present & Future – slide 5 / 95 Grand Canyon: Earth History from 200 million - 2 billion yrs ago. Dating Rocks Life on Earth Earth History Timeline Late Heavy Bombardment Hadean Shark Bay Stromatolites Cyanobacteria Q: Earliest Fossils? Life on Earth O2 History Q: Life on Earth How Did Life Arise? Life in the Solar System Life Around Other Stars Interstellar Travel SETI Review c 2012-2021 G. -
Arxiv:1508.05435V1 [Physics.Bio-Ph]
Fast nastic motion of plants and bio-inspired structures Q. Guo1,2, E. Dai3, X. Han4, S. Xie5, E. Chao3, Z. Chen4 1College of Materials Science and Engineering, FuJian University of Technology, Fuzhou 350108, China 2Fujian Provincial Key Laboratory of Advanced Materials Processing and Application, Fuzhou 350108, China 3Department of Biomedical Engineering, Washington University, St. Louis, MO 63130 USA 4Thayer School of Engineering, Dartmouth College, Hanover, New Hampshire, NH 03755, USA 5Department of Energy, Environmental, and Chemical Engineering, Washington University, St. Louis, MO 63130 USA ∗ (Dated: August 25, 2015) The capability to sense and respond to external mechanical stimuli at various timescales is es- sential to many physiological aspects in plants, including self-protection, intake of nutrients, and reproduction. Remarkably, some plants have evolved the ability to react to mechanical stimuli within a few seconds despite a lack of muscles and nerves. The fast movements of plants in response to mechanical stimuli have long captured the curiosity of scientists and engineers, but the mechanisms behind these rapid thigmonastic movements still are not understood completely. In this article, we provide an overview of such thigmonastic movements in several representative plants, including Dionaea, Utricularia, Aldrovanda, Drosera, and Mimosa. In addition, we review a series of studies that present biomimetic structures inspired by fast moving plants. We hope that this article will shed light on the current status of research on the fast movements of plants and bioinspired struc- tures and also promote interdisciplinary studies on both the fundamental mechanisms of plants’ fast movements and biomimetic structures for engineering applications, such as artificial muscles, multi-stable structures, and bioinspired robots. -
Terrestrial Planets Across Space and Time 3
A Preprint typeset using LTEX style emulateapj v. 11/10/09 TERRESTRIAL PLANETS ACROSS SPACE AND TIME Erik Zackrisson1∗, Per Calissendorff2, Juan Gonzalez´ 2, Andrew Benson3, Anders Johansen4, Markus Janson2 ABSTRACT The study of cosmology, galaxy formation and exoplanets has now advanced to a stage where a cosmic inventory of terrestrial planets may be attempted. By coupling semi-analytic models of galaxy formation to a recipe that relates the occurrence of planets to the mass and metallicity of their host stars, we trace the population of terrestrial planets around both solar-mass (FGK type) and lower- mass (M dwarf) stars throughout all of cosmic history. We find that the mean age of terrestrial planets in the local Universe is 7 ± 1 Gyr for FGK hosts and 8 ± 1 Gyr for M dwarfs. We estimate that hot Jupiters have depleted the population of terrestrial planets around FGK stars by no more than ≈ 10%, and that only ≈ 10% of the terrestrial planets at the current epoch are orbiting stars in a metallicity range for which such planets have yet to be confirmed. The typical terrestrial planet in the local Universe is located in a spheroid-dominated galaxy with a total stellar mass comparable to that of the Milky Way. When looking at the inventory of planets throughout the whole observable Universe, we argue for a total of ≈ 1×1019 and ≈ 5×1020 terrestrial planets around FGK and M stars, respectively. Due to light travel time effects, the terrestrial planets on our past light cone exhibit a mean age of just 1.7 ± 0.2 Gyr. -
Investigating Plant Physiology with Wisconsin Fast Plants™ Investigating Plant Physiology with Wisconsin Fast Plants™
Investigating Plant Physiology with Wisconsin Fast Plants™ Investigating Plant Physiology with Wisconsin Fast Plants™ Table of Contents Introduction to Investigating Plant Physiology with Wisconsin Fast Plants™ . .4 Investigating Nutrition with Wisconsin Fast Plants™ . .4 Investigating Plant Nutrition Activity . .7 Introduction to Tropisms . .10 Investigating Tropisms with Wisconsin Fast Plants™ . .10 Materials in the Wisconsin Fast Plants™ Hormone Kit • 1 pack of Standard Wisconsin Fast Plants™ • 1 packet anti-algal square (2 squares per packet) Seeds • 8 watering pipettes • 1 pack of Rosette-Dwarf Wisconsin Fast • 1 L potting soil Plants™ Seeds • 1 package of dried bees • 100-ppm Gibberellic Acid (4 oz) • four 4-cell quads • 1oz pelleted fertilizer • 16 support stakes • 2 watering trays • 16 support rings • 2 watering mats • Growing Instructions • wicks (package of 70) For additional activities, student pages and related resources, please visit the Wisconsin Fast Plants’ website at www.fastplants.org Investigating Plant Physiology with Wisconsin Fast Plants™ Plant physiology is the study of how plants individual is the result of the genetic makeup function. The activities and background (genotype) of that organism being expressed in information in this booklet are designed to the environment in which the organism exists. support investigations into three primary areas Components of the environment are physical of plant physiology: Nutrition, Tropism, and (temperature, light, gravity), chemical (water, Hormone Response (using gibberellin). elements, salts, complex molecules), and biotic (microbes, animals and other plants). Fundamental to the study of physiology is Environmental investigations in this booklet understanding the role that environment plays focus on the influence of nutrients, gravity, and in the functioning and appearance (phenotype) a growth-regulating hormone. -
Tropism Flip Book Unit 8
Name ____________________________________________________________ Period _______ 7th Grade Science Tropism Flip Book Unit 8 Directions: You are going to create a quick reference chart for the various types of Tropism . Tropism is a term that refers to how an organism grows due to an external stimulus. For each type of tropism, you will need to provide a definition and a picture/example of that type of tropism. Below is a list of terms that you will include in your “Flip Book”. Flip Book Terms: Internal Stimuli External Stimuli Gravitropism Phototropism Geotropism Hydrotropism Thigmatropism How Do You Create a Flip Book? Step 1: Obtain 4 half sheets of paper. Stack the sheets of paper on top of each other. They should be staggered about a 2 cm. See the picture below. 2 cm 2 cm 2 cm Step 2: Now fold the top half of the 4 pieces of paper forward. Now all of the pieces of paper are staggered 2 cm. You should have 8 tabs. Place two staples at the very top. Staples Tab #1 Tab #2 Tab #3 Tab #4 Tab #5 Tab #6 Tab #7 Tab #8 Step 3: On the very top tab (Tab #1) you are going to write/draw the words " Tropism Flip Book ". You may use markers or colored pencils throughout this project to color and decorate your flip book. Also write your name and period. See the example below. Tropism Flip Book Your Name Period Step 4: At the bottom of each tab you are going to write each of the flip book terms (Internal Stimuli, External Stimuli, Gravitropism, Phototropism, Geotropism, Hydrotropism, and Thigmatropism ). -
Intergalactic Spreading of Intelligent Life and Sharpening the Fermi Paradox
Eternity in six hours: intergalactic spreading of intelligent life and sharpening the Fermi paradox Stuart Armstronga,∗, Anders Sandberga aFuture of Humanity Institute, Philosophy Department, Oxford University, Suite 8, Littlegate House 16/17 St. Ebbe's Street, Oxford, OX1 1PT UK Abstract The Fermi paradox is the discrepancy between the strong likelihood of alien intelligent life emerging (under a wide variety of assumptions), and the ab- sence of any visible evidence for such emergence. In this paper, we extend the Fermi paradox to not only life in this galaxy, but to other galaxies as well. We do this by demonstrating that traveling between galaxies { indeed even launching a colonisation project for the entire reachable universe { is a rela- tively simple task for a star-spanning civilization, requiring modest amounts of energy and resources. We start by demonstrating that humanity itself could likely accomplish such a colonisation project in the foreseeable future, should we want to, and then demonstrate that there are millions of galaxies that could have reached us by now, using similar methods. This results in a considerable sharpening of the Fermi paradox. Keywords: Fermi paradox, interstellar travel, intergalactic travel, Dyson shell, SETI, exploratory engineering 1. Introduction 1.1. The classical Fermi paradox The Fermi paradox, or more properly the Fermi question, consists of the apparent discrepancy between assigning a non-negligible probability for intelligent life emerging, the size and age of the universe, the relative rapidity ∗Corresponding author Email addresses: [email protected] (Stuart Armstrong), [email protected] (Anders Sandberg) Preprint submitted to Acta Astronautica March 12, 2013 with which intelligent life could expand across space or otherwise make itself visible, and the lack of observations of any alien intelligence. -
Why Is the Definition of Life and Life's Origins on Earth
WHY IS THE DEFINITION OF LIFE AND LIFE’S ORIGINS ON EARTH IMPORTANT IN EXTRATERRESTRIAL RESEARCH Jan Jędryszek 1;78703924449250650000000000000 000000000000000000000000000000 000000000000000000000000000000 000000000000000000000000000000 000000000000000000000000000000 000000000000000000000000000000 000000000000000000000000000000 000000000000000000000000000000 0 1. Introduction Plan 2. Life – Is a definition of a “living system” possible? – Life’s origins? 3. Looking for life 4. Thompson Jr. – Future findings and results – Advantages The 2nd Law & Entropy ENTROPY - . "a measure of disorder or randomness in a closed system.“ -The American Heritage Dictionary . "mixedupness." -J. Willard Gibbs, theoretical physicist Can you reduce entropy? • The total entropy of system A can not decrease without increasing the entropy of system B. • Hence, in a system isolated from its environment, the entropy of that system will tend not to decrease. Humans don’t dissolve. Are we isolated systems? We are NOT Gibbs Free Energy G = H − TS • H - enthalpy (joules) • T - temperature (kelvins) • S - entropy (joule per kelvin) ∆G negative = reaction can occur spontaneously. +5.5 kcal/mole. Glucose Fructose -7.3 kcal/mole ATP ADP P ATP ATP P ADP ATP P Sucrose P ADP ATP -1.8 kcal/mole -7.3 kcal/mole. (the reaction will occur +5.5 kcal/ mole spontaneously. ) P Sucrose P ADP Gibbs Free Energy is the basic principle behind all enzymatic action in biological organisms Entropy is NOT an obstacle for life. Abiogenesis The natural process of life arising from non- living matter. Life? • Life - The ability to grow, change, etc. that Life separates plants and animals from things like water or rocks. • Life is not a “thing” • It’s a process • Millions of biochemical reactions in every single cell in our bodies. -
Multiscale Integration of Environmental Stimuli in Plant
Multiscale integration of environmental stimuli in plant tropism produces complex behaviors Derek E. Moultona,1,2 , Hadrien Oliveria,1 , and Alain Gorielya,1,2 aMathematical Institute, University of Oxford, Oxford OX2 6GG, United Kingdom Edited by Enrico Coen, John Innes Center, Norwich, United Kingdom, and approved November 4, 2020 (received for review July 30, 2020) Plant tropism refers to the directed movement of an organ or expanding at different rates in response to the chemical and organism in response to external stimuli. Typically, these stimuli molecular signals. However, one cannot understand the change induce hormone transport that triggers cell growth or deforma- in shape of the plant and its position in relation to the direction tion. In turn, these local cellular changes create mechanical forces of the environmental stimulus at this level. To assess the effec- on the plant tissue that are balanced by an overall deformation tiveness of the growth response, one needs to zoom out. The net of the organ, hence changing its orientation with respect to the effect of a nonuniform cell expansion due to hormone signaling stimuli. This complex feedback mechanism takes place in a three- is a tissue-level differential growth (1) as depicted in Fig. 2. At dimensional growing plant with varying stimuli depending on the tissue level, each cross-section of the plant can be viewed the environment. We model this multiscale process in filamen- as a continuum of material that undergoes nonuniform growth tary organs for an arbitrary stimulus by explicitly linking hormone and/or remodeling (17). Differential growth locally creates cur- transport to local tissue deformation leading to the generation vature and torsion, but it also generates residual stress (18). -
ASTR1000 Lecture (Meisel, Spring 2021)
An introduction to the Drake Equation Zach Meisel Ohio University - ASTR1000 How many intelligent, communicating extraterrestrial civilizations are out there? • The Drake Equation is a tool to approach this question in a semi-quantitative way • The number of civilizations that we could communicate with ( ) is determined by the rate of star formation ( ), the fraction of those stars with planets ( ), the number those planets for a given star that are habitable ( ), the fraction of those habitable planets that develop life ( ), the fraction of those life-developing planets that result in intelligent life ( ), the fraction of civilizations that develop the ability to communicate over long distances ( ), and the lifetime of that civilization ( ) • Putting it all together: = readily (much) more quantifiablespeculative in = • The rate of star formation can be calculated by considering the mass of stars in the Milky Way, an initial mass function, and stellar lifetimes to arrive at something like ~4 stars/year Licquia & Newman ApJ 2015 JohannesBuchner in = •The fraction of stars with planets is thought to be ~1, taking into account the sensitivity of exoplanet detection methods and assuming a planetary mass function Cassan et al. Nature 2012 in = • The number of habitable planets per planet-hosting star is based on the criterion adopted for habitability (e.g. atmosphere conditions, moons, methane-based life, light flux, temperature) • Using a (likely) rocky surface and (likely) ability to sustain liquid water, ~60 of the ~4,600 exoplanets detected to date are considered potentially habitable. Adding moons into the picture (see Intro to Solar System Life) probably doubles this number • So ~0.02 isn’t unreasonable, though detection bias & expanding criteria for habitability could make this ~1 Kopparapu et al. -
Deforestation and World Population Sustainability
Deforestation and world population sustainability: a quantitative analysis Mauro Bologna1 and Gerardo Aquino2,3,4* 1Departamento de Ingenier´ıa Electrica-Electr´ onica,´ Universidad de Tarapaca´ 2The Alan Turing Institute, London, UK 3University of Surrey, Guildford, UK. 4Goldsmiths, University of London, UK *[email protected] +these authors contributed equally to this work ABSTRACT In this paper we afford a quantitative analysis of the sustainability of current world population growth in relation to the parallel deforestation process adopting a statistical point of view. We consider a simplified model based on a stochastic growth process driven by a continuous time random walk, which depicts the technological evolution of human kind, in conjunction with a deterministic generalised logistic model for humans-forest interaction and we evaluate the probability of avoiding the self-destruction of our civilisation. Based on the current resource consumption rates and best estimate of technological rate growth our study shows that we have very low probability, less than 10% in most optimistic estimate, to survive without facing a catastrophic collapse. Introduction In the last few decades, the debate on climate change has assumed global importance with consequences on national and global policies. Many factors due to human activity are considered as possible responsible of the observed changes: among these water and air contamination (mostly greenhouse effect) and deforestation are the mostly cited. While the extent of human contribution to the greenhouse effect and temperature changes is still a matter of discussion, the deforestation is an undeniable fact. Indeed before the development of human civilisations, our planet was covered by 60 million square kilometres of forest1. -
Terrestrial Planets Across Space and Time 3
A Preprint typeset using LTEX style emulateapj v. 11/10/09 TERRESTRIAL PLANETS ACROSS SPACE AND TIME Erik Zackrisson1∗, Per Calissendorff1,2, Juan Gonzalez´ 2, Andrew Benson3, Anders Johansen4, Markus Janson2 ABSTRACT The study of cosmology, galaxy formation and exoplanetary systems has now advanced to a stage where a cosmic inventory of terrestrial planets may be attempted. By coupling semi-analytic models of galaxy formation to a recipe that relates the occurrence of planets to the mass and metallicity of their host stars, we trace the population of terrestrial planets around both solar-mass (FGK type) and lower-mass (M dwarf) stars throughout all of cosmic history. We find that the mean age of terrestrial planets in the local Universe is 8 ± 1 Gyr and that the typical planet of this type is located in a spheroid-dominated galaxy with total stellar mass about twice that of the Milky Way. We estimate that hot Jupiters have depleted the population of terrestrial planets around FGK stars at redshift z = 0 by no more than ≈ 10%, and predict that ≈ 1/3 of the terrestrial planets in the local Universe are orbiting stars in a metallicity range for which such planets have yet to be been detected. When looking at the inventory of planets throughout the whole observable Universe (i.e. in all galaxies on our past light cone) we argue for a total of ≈ 2 × 1019 and ≈ 7 × 1020 terrestrial planets around FGK and M stars, respectively. Due to the hierarchical formation of galaxies and lookback-time effects, the average terrestrial planet on our past light cone has an age of just 1.7 ± 0.2 Gyr and is sitting in a galaxy with a stellar mass a factor of ≈ 2 lower than that of the Milky Way. -
Fermi Paradox from Wikipedia, the Free Encyclopedia Jump To: Navigation, Search
Fermi paradox From Wikipedia, the free encyclopedia Jump to: navigation, search This article is about the absence of evidence for extraterrestrial intelligence. For the type of estimation problem, see Fermi problem. For the music album, see Fermi Paradox (album). For the short story, see The Fermi Paradox Is Our Business Model. A graphical representation of the Arecibo message – Humanity's first attempt to use radio waves to actively communicate its existence to alien civilizations The Fermi paradox (or Fermi's paradox) is the apparent contradiction between high estimates of the probability of the existence of extraterrestrial civilization and humanity's lack of contact with, or evidence for, such civilizations.[1] The basic points of the argument, made by physicists Enrico Fermi and Michael H. Hart, are: • The Sun is a young star. There are billions of stars in the galaxy that are billions of years older; • Some of these stars likely have Earth-like planets[2] which, if the Earth is typical, may develop intelligent life; • Presumably some of these civilizations will develop interstellar travel, as Earth seems likely to do; • At any practical pace of interstellar travel, the galaxy can be completely colonized in just a few tens of millions of years. According to this line of thinking, the Earth should have already been colonized, or at least visited. But no convincing evidence of this exists. Furthermore, no confirmed signs of intelligence elsewhere have been spotted, either in our galaxy or the more than 80 billion other galaxies of the