Chapter 18: Life On Earth

Chapter 1
How Science Works

  • The Scientific Method
  • Evidence
  • Measurements
  • Units and the Metric System
  • Measurement Errors
  • Estimation
  • Dimensions
  • Mass, Length, and Time
  • Observations and Uncertainty
  • Precision and Significant Figures
  • Errors and Statistics
  • Scientific Notation
  • Ways of Representing Data
  • Logic
  • Mathematics
  • Geometry
  • Algebra
  • Logarithms
  • Testing a Hypothesis
  • Case Study of Life on Mars
  • Theories
  • Systems of Knowledge
  • The Culture of Science
  • Computer Simulations
  • Modern Scientific Research
  • The Scope of Astronomy
  • Astronomy as a Science
  • A Scale Model of Space
  • A Scale Model of Time
  • Questions

Chapter 2
Early Astronomy

  • The Night Sky
  • Motions in the Sky
  • Navigation
  • Constellations and Seasons
  • Cause of the Seasons
  • The Magnitude System
  • Angular Size and Linear Size
  • Phases of the Moon
  • Eclipses
  • Auroras
  • Dividing Time
  • Solar and Lunar Calendars
  • History of Astronomy
  • Stonehenge
  • Ancient Observatories
  • Counting and Measurement
  • Astrology
  • Greek Astronomy
  • Aristotle and Geocentric Cosmology
  • Aristarchus and Heliocentric Cosmology
  • The Dark Ages
  • Arab Astronomy
  • Indian Astronomy
  • Chinese Astronomy
  • Mayan Astronomy
  • Questions

Chapter 3
The Copernican Revolution

  • Ptolemy and the Geocentric Model
  • The Renaissance
  • Copernicus and the Heliocentric Model
  • Tycho Brahe
  • Johannes Kepler
  • Elliptical Orbits
  • Kepler's Laws
  • Galileo Galilei
  • The Trial of Galileo
  • Isaac Newton
  • Newton's Law of Gravity
  • The Plurality of Worlds
  • The Birth of Modern Science
  • Layout of the Solar System
  • Scale of the Solar System
  • The Idea of Space Exploration
  • Orbits
  • History of Space Exploration
  • Moon Landings
  • International Space Station
  • Manned versus Robotic Missions
  • Commercial Space Flight
  • Future of Space Exploration
  • Living in Space
  • Moon, Mars, and Beyond
  • Societies in Space
  • Questions

Chapter 4
Matter and Energy in the Universe

  • Matter and Energy
  • Rutherford and Atomic Structure
  • Early Greek Physics
  • Dalton and Atoms
  • The Periodic Table
  • Structure of the Atom
  • Energy
  • Heat and Temperature
  • Potential and Kinetic Energy
  • Conservation of Energy
  • Velocity of Gas Particles
  • States of Matter
  • Thermodynamics
  • Entropy
  • Laws of Thermodynamics
  • Heat Transfer
  • Thermal Radiation
  • Wien's Law
  • Radiation from Planets and Stars
  • Internal Heat in Planets and Stars
  • Periodic Processes
  • Random Processes
  • Questions

Chapter 5
The Earth-Moon System

  • Earth and Moon
  • Early Estimates of Earth's Age
  • How the Earth Cooled
  • Ages Using Radioactivity
  • Radioactive Half-Life
  • Ages of the Earth and Moon
  • Geological Activity
  • Internal Structure of the Earth and Moon
  • Basic Rock Types
  • Layers of the Earth and Moon
  • Origin of Water on Earth
  • The Evolving Earth
  • Plate Tectonics
  • Volcanoes
  • Geological Processes
  • Impact Craters
  • The Geological Timescale
  • Mass Extinctions
  • Evolution and the Cosmic Environment
  • Earth's Atmosphere and Oceans
  • Weather Circulation
  • Environmental Change on Earth
  • The Earth-Moon System
  • Geological History of the Moon
  • Tidal Forces
  • Effects of Tidal Forces
  • Historical Studies of the Moon
  • Lunar Surface
  • Ice on the Moon
  • Origin of the Moon
  • Humans on the Moon
  • Questions

Chapter 6
The Terrestrial Planets

  • Studying Other Planets
  • The Planets
  • The Terrestrial Planets
  • Mercury
  • Mercury's Orbit
  • Mercury's Surface
  • Venus
  • Volcanism on Venus
  • Venus and the Greenhouse Effect
  • Tectonics on Venus
  • Exploring Venus
  • Mars in Myth and Legend
  • Early Studies of Mars
  • Mars Close-Up
  • Modern Views of Mars
  • Missions to Mars
  • Geology of Mars
  • Water on Mars
  • Polar Caps of Mars
  • Climate Change on Mars
  • Terraforming Mars
  • Life on Mars
  • The Moons of Mars
  • Martian Meteorites
  • Comparative Planetology
  • Incidence of Craters
  • Counting Craters
  • Counting Statistics
  • Internal Heat and Geological Activity
  • Magnetic Fields of the Terrestrial Planets
  • Mountains and Rifts
  • Radar Studies of Planetary Surfaces
  • Laser Ranging and Altimetry
  • Gravity and Atmospheres
  • Normal Atmospheric Composition
  • The Significance of Oxygen
  • Questions

Chapter 7
The Giant Planets and Their Moons

  • The Gas Giant Planets
  • Atmospheres of the Gas Giant Planets
  • Clouds and Weather on Gas Giant Planets
  • Internal Structure of the Gas Giant Planets
  • Thermal Radiation from Gas Giant Planets
  • Life on Gas Giant Planets?
  • Why Giant Planets are Giant
  • Gas Laws
  • Ring Systems of the Giant Planets
  • Structure Within Ring Systems
  • The Origin of Ring Particles
  • The Roche Limit
  • Resonance and Harmonics
  • Tidal Forces in the Solar System
  • Moons of Gas Giant Planets
  • Geology of Large Moons
  • The Voyager Missions
  • Jupiter
  • Jupiter's Galilean Moons
  • Jupiter's Ganymede
  • Jupiter's Europa
  • Jupiter's Callisto
  • Jupiter's Io
  • Volcanoes on Io
  • Saturn
  • Cassini Mission to Saturn
  • Saturn's Titan
  • Saturn's Enceladus
  • Discovery of Uranus and Neptune
  • Uranus
  • Uranus' Miranda
  • Neptune
  • Neptune's Triton
  • Pluto
  • The Discovery of Pluto
  • Pluto as a Dwarf Planet
  • Dwarf Planets
  • Questions

Chapter 8
Interplanetary Bodies

  • Interplanetary Bodies
  • Comets
  • Early Observations of Comets
  • Structure of the Comet Nucleus
  • Comet Chemistry
  • Oort Cloud and Kuiper Belt
  • Kuiper Belt
  • Comet Orbits
  • Life Story of Comets
  • The Largest Kuiper Belt Objects
  • Meteors and Meteor Showers
  • Gravitational Perturbations
  • Asteroids
  • Surveys for Earth Crossing Asteroids
  • Asteroid Shapes
  • Composition of Asteroids
  • Introduction to Meteorites
  • Origin of Meteorites
  • Types of Meteorites
  • The Tunguska Event
  • The Threat from Space
  • Probability and Impacts
  • Impact on Jupiter
  • Interplanetary Opportunity
  • Questions

Chapter 9
Planet Formation and Exoplanets

  • Formation of the Solar System
  • Early History of the Solar System
  • Conservation of Angular Momentum
  • Angular Momentum in a Collapsing Cloud
  • Helmholtz Contraction
  • Safronov and Planet Formation
  • Collapse of the Solar Nebula
  • Why the Solar System Collapsed
  • From Planetesimals to Planets
  • Accretion and Solar System Bodies
  • Differentiation
  • Planetary Magnetic Fields
  • The Origin of Satellites
  • Solar System Debris and Formation
  • Gradual Evolution and a Few Catastrophies
  • Chaos and Determinism
  • Extrasolar Planets
  • Discoveries of Exoplanets
  • Doppler Detection of Exoplanets
  • Transit Detection of Exoplanets
  • The Kepler Mission
  • Direct Detection of Exoplanets
  • Properties of Exoplanets
  • Implications of Exoplanet Surveys
  • Future Detection of Exoplanets
  • Questions

Chapter 10
Detecting Radiation from Space

  • Observing the Universe
  • Radiation and the Universe
  • The Nature of Light
  • The Electromagnetic Spectrum
  • Properties of Waves
  • Waves and Particles
  • How Radiation Travels
  • Properties of Electromagnetic Radiation
  • The Doppler Effect
  • Invisible Radiation
  • Thermal Spectra
  • The Quantum Theory
  • The Uncertainty Principle
  • Spectral Lines
  • Emission Lines and Bands
  • Absorption and Emission Spectra
  • Kirchoff's Laws
  • Astronomical Detection of Radiation
  • The Telescope
  • Optical Telescopes
  • Optical Detectors
  • Adaptive Optics
  • Image Processing
  • Digital Information
  • Radio Telescopes
  • Telescopes in Space
  • Hubble Space Telescope
  • Interferometry
  • Collecting Area and Resolution
  • Frontier Observatories
  • Questions

Chapter 11
Our Sun: The Nearest Star

  • The Sun
  • The Nearest Star
  • Properties of the Sun
  • Kelvin and the Sun's Age
  • The Sun's Composition
  • Energy From Atomic Nuclei
  • Mass-Energy Conversion
  • Examples of Mass-Energy Conversion
  • Energy From Nuclear Fission
  • Energy From Nuclear Fusion
  • Nuclear Reactions in the Sun
  • The Sun's Interior
  • Energy Flow in the Sun
  • Collisions and Opacity
  • Solar Neutrinos
  • Solar Oscillations
  • The Sun's Atmosphere
  • Solar Chromosphere and Corona
  • Sunspots
  • The Solar Cycle
  • The Solar Wind
  • Effects of the Sun on the Earth
  • Cosmic Energy Sources
  • Questions

Chapter 12
Properties of Stars

  • Stars
  • Star Names
  • Star Properties
  • The Distance to Stars
  • Apparent Brightness
  • Absolute Brightness
  • Measuring Star Distances
  • Stellar Parallax
  • Spectra of Stars
  • Spectral Classification
  • Temperature and Spectral Class
  • Stellar Composition
  • Stellar Motion
  • Stellar Luminosity
  • The Size of Stars
  • Stefan-Boltzmann Law
  • Stellar Mass
  • Hydrostatic Equilibrium
  • Stellar Classification
  • The Hertzsprung-Russell Diagram
  • Volume and Brightness Selected Samples
  • Stars of Different Sizes
  • Understanding the Main Sequence
  • Stellar Structure
  • Stellar Evolution
  • Questions

Chapter 13
Star Birth and Death

  • Star Birth and Death
  • Understanding Star Birth and Death
  • Cosmic Abundance of Elements
  • Star Formation
  • Molecular Clouds
  • Young Stars
  • T Tauri Stars
  • Mass Limits for Stars
  • Brown Dwarfs
  • Young Star Clusters
  • Cauldron of the Elements
  • Main Sequence Stars
  • Nuclear Reactions in Main Sequence Stars
  • Main Sequence Lifetimes
  • Evolved Stars
  • Cycles of Star Life and Death
  • The Creation of Heavy Elements
  • Red Giants
  • Horizontal Branch and Asymptotic Giant Branch Stars
  • Variable Stars
  • Magnetic Stars
  • Stellar Mass Loss
  • White Dwarfs
  • Supernovae
  • Seeing the Death of a Star
  • Supernova 1987A
  • Neutron Stars and Pulsars
  • Special Theory of Relativity
  • General Theory of Relativity
  • Black Holes
  • Properties of Black Holes
  • Questions

Chapter 14
The Milky Way

  • The Distribution of Stars in Space
  • Stellar Companions
  • Binary Star Systems
  • Binary and Multiple Stars
  • Mass Transfer in Binaries
  • Binaries and Stellar Mass
  • Nova and Supernova
  • Exotic Binary Systems
  • Gamma Ray Bursts
  • How Multiple Stars Form
  • Environments of Stars
  • The Interstellar Medium
  • Effects of Interstellar Material on Starlight
  • Structure of the Interstellar Medium
  • Dust Extinction and Reddening
  • Groups of Stars
  • Open Star Clusters
  • Globular Star Clusters
  • Distances to Groups of Stars
  • Ages of Groups of Stars
  • Layout of the Milky Way
  • William Herschel
  • Isotropy and Anisotropy
  • Mapping the Milky Way
  • Questions

Chapter 15
Galaxies

  • The Milky Way Galaxy
  • Mapping the Galaxy Disk
  • Spiral Structure in Galaxies
  • Mass of the Milky Way
  • Dark Matter in the Milky Way
  • Galaxy Mass
  • The Galactic Center
  • Black Hole in the Galactic Center
  • Stellar Populations
  • Formation of the Milky Way
  • Galaxies
  • The Shapley-Curtis Debate
  • Edwin Hubble
  • Distances to Galaxies
  • Classifying Galaxies
  • Spiral Galaxies
  • Elliptical Galaxies
  • Lenticular Galaxies
  • Dwarf and Irregular Galaxies
  • Overview of Galaxy Structures
  • The Local Group
  • Light Travel Time
  • Galaxy Size and Luminosity
  • Mass to Light Ratios
  • Dark Matter in Galaxies
  • Gravity of Many Bodies
  • Galaxy Evolution
  • Galaxy Interactions
  • Galaxy Formation
  • Questions

Chapter 16
The Expanding Universe

  • Galaxy Redshifts
  • The Expanding Universe
  • Cosmological Redshifts
  • The Hubble Relation
  • Relating Redshift and Distance
  • Galaxy Distance Indicators
  • Size and Age of the Universe
  • The Hubble Constant
  • Large Scale Structure
  • Galaxy Clustering
  • Clusters of Galaxies
  • Overview of Large Scale Structure
  • Dark Matter on the Largest Scales
  • The Most Distant Galaxies
  • Black Holes in Nearby Galaxies
  • Active Galaxies
  • Radio Galaxies
  • The Discovery of Quasars
  • Quasars
  • Types of Gravitational Lensing
  • Properties of Quasars
  • The Quasar Power Source
  • Quasars as Probes of the Universe
  • Star Formation History of the Universe
  • Expansion History of the Universe
  • Questions

Chapter 17
Cosmology

  • Cosmology
  • Early Cosmologies
  • Relativity and Cosmology
  • The Big Bang Model
  • The Cosmological Principle
  • Universal Expansion
  • Cosmic Nucleosynthesis
  • Cosmic Microwave Background Radiation
  • Discovery of the Microwave Background Radiation
  • Measuring Space Curvature
  • Cosmic Evolution
  • Evolution of Structure
  • Mean Cosmic Density
  • Critical Density
  • Dark Matter and Dark Energy
  • Age of the Universe
  • Precision Cosmology
  • The Future of the Contents of the Universe
  • Fate of the Universe
  • Alternatives to the Big Bang Model
  • Space-Time
  • Particles and Radiation
  • The Very Early Universe
  • Mass and Energy in the Early Universe
  • Matter and Antimatter
  • The Forces of Nature
  • Fine-Tuning in Cosmology
  • The Anthropic Principle in Cosmology
  • String Theory and Cosmology
  • The Multiverse
  • The Limits of Knowledge
  • Questions

Chapter 18
Life On Earth

  • Nature of Life
  • Chemistry of Life
  • Molecules of Life
  • The Origin of Life on Earth
  • Origin of Complex Molecules
  • Miller-Urey Experiment
  • Pre-RNA World
  • RNA World
  • From Molecules to Cells
  • Metabolism
  • Anaerobes
  • Extremophiles
  • Thermophiles
  • Psychrophiles
  • Xerophiles
  • Halophiles
  • Barophiles
  • Acidophiles
  • Alkaliphiles
  • Radiation Resistant Biology
  • Importance of Water for Life
  • Hydrothermal Systems
  • Silicon Versus Carbon
  • DNA and Heredity
  • Life as Digital Information
  • Synthetic Biology
  • Life in a Computer
  • Natural Selection
  • Tree Of Life
  • Evolution and Intelligence
  • Culture and Technology
  • The Gaia Hypothesis
  • Life and the Cosmic Environment

Chapter 19
Life in the Universe

  • Life in the Universe
  • Astrobiology
  • Life Beyond Earth
  • Sites for Life
  • Complex Molecules in Space
  • Life in the Solar System
  • Lowell and Canals on Mars
  • Implications of Life on Mars
  • Extreme Environments in the Solar System
  • Rare Earth Hypothesis
  • Are We Alone?
  • Unidentified Flying Objects or UFOs
  • The Search for Extraterrestrial Intelligence
  • The Drake Equation
  • The History of SETI
  • Recent SETI Projects
  • Recognizing a Message
  • The Best Way to Communicate
  • The Fermi Question
  • The Anthropic Principle
  • Where Are They?

Evolution and Intelligence


Life got off to a quick start, gaining a foothold almost as soon as it could on the cooling crust. For two-thirds of the entire history of life on Earth, no organism evolved beyond the simplest, or prokaryotic, design. For the better part of another billion years, eukaryotic cells propagated without any great increase in complexity. After all this time, nothing beyond a single-celled organism existed on the face of the planet. About half a billion years ago, something extraordinary happened on Earth. Simple life forms proliferated and a couple of them eventually developed intelligence. The last half billion years of the Earth's evolution are thus dramatic because they gave rise to one species — Homo sapiens — with the ability to discover and understand the universe.


small timeline showing different events in the evolution of life

The evolution of intelligence occurred relatively recently in the Earth's history. To illustrate this, let us consider the history of the Earth in terms of the analogy of a single year. The Earth forms on January 1, and by the end of February, the first simple cells have a tenacious hold. The atmosphere is enriched with oxygen during the spring and early summer, and by the end of October, cells with nuclei exist for the first time. From here on, life exhibits a startling acceleration in complexity. The oceans filled with multi-cellular life forms in the Cambrian era that begins in mid-November. Land animals do not appear until the end of November. Dinosaurs rule the Earth for the first part of December, and primates first appear on December 26. Our hominid ancestors do not arrive on the scene until 10 A.M. on December 31, and Homo sapiens does not develop until 3.5 minutes before midnight. The entire modern history of astronomy, including our ability to communicate through space with electromagnetic waves, occupies the last tenth of a second of this analog year: a time of 11:59:59.9 P.M on December 31.


A graphical timeline of the Big Bang
There was a period when life made dramatic gains in complexity — October and November in the analogy where the history of Earth is a year. About 600 million years ago, the Earth's oceans witnessed an explosion of multi-celled organisms. This spurt in evolution was probably encouraged by the buildup of oxygen in the atmosphere, which allowed more complex metabolic processes, and by the breakup of the continents, which provided more niches for life. Before the surge in evolution, eukaryotes had only three kingdoms: fungi, plants, and animals. After the surge, each of these three kingdoms generated scores of separate evolutionary lines. As with the origin of life itself, there is evidence for several failed experiments in multi-celled organisms. All higher-level animals, including humans, evolved from only one of these experiments. The rich diversity of life in the pre-Cambrian oceans has been chronicled by Harvard paleontologist Steven Jay Gould in the story of the Burgess Shale, a fossil site in Canada. Throughout this time, few organisms had "hard parts," leaving the fossil record very sketchy. So we rely on fortuitous events like those that led to the Burgess Shale, where entire ecosystems were gently entombed by a mudslide on the ocean floor.


Trilobites, alive during the Cambrian era

The Cambrian fauna included the first hard-bodied sea creatures, the trilobites. Trilobites have two eyes and a complex body structure, but they are extremely primitive by human standards. The vertebrates in the oceans of 500 to 600 million years ago are loosely lumped together as "fishes," but they are strikingly different in function and form. Most did not survive to live in the oceans of today. About 450 million years ago, plants began to spread across the continents, their spores and seeds carried by the wind. Next came the extraordinary migration of certain types of fish to the land. The transition from a streamlined aquatic animal to one that dragged itself around on poorly formed limbs must have conveyed some adaptive advantage, but it is an unlikely and remarkable transition in retrospect. Equally remarkable is the fact that 350 million years ago insects first took to the air, followed 200 million years ago by the descendants of one type of reptile, birds. By this time, the fossil record shows that life had radiated into all possible environments.

It would be a mistake to see the progression towards greater sophistication and complexity as predictable or inevitable. About 225 million years ago, after dinosaurs became established on the land, the fossil record in the oceans shows that 95 percent of all marine species became extinct in a short period of time. The cause of this mass extinction is unknown. Then, 65 million years ago, another mass extinction led to the demise of the dinosaurs. This second catastrophe helped the evolution of the mammals, which were in competition with the dinosaurs for food. Thereafter, many mammals developed complex central nervous systems and large brains, but for many millions of years, there is no sign of high intelligence.


Illustration of primates (chimpanzee, orang-utan, long-arm gibbon and siamang) by 19th century naturalist G.H. Schubert.

Primates appeared on the scene only 4 or 5 million years ago, yet there are many more evolutionary branches and extinct lines before we arrive, some 500,000 years ago, at modern Homo sapiens. It took 99.99% of the time since life began on Earth to develop a human level of intelligence. Humans have only had the ability to explore and communicate with the cosmos for a few hundred years — a blink of the eye in the eons since the motor of life first turned over.

Once life begins, is the eventual development of intelligence inevitable? This question is central to the likelihood of communication with life beyond the Solar System. First, we need to define intelligence. Most people would agree on the relative intelligence of the occupants of this planet. For example, a sequence of species ranked in order of increasing intelligence might be the following: worms, frogs, birds, dogs, chimpanzees, and humans. In general, intelligence corresponds to brain size, which correlates with body mass. Intelligence varies continuously among species, but we can set a high standard. Let's define intelligence as the capability of abstract thought, coupled with the ability to use tools or technology and to control the environment.

Life on Earth often evolves toward organisms of greater complexity. It might be supposed that intelligence carries with it an adaptive advantage and so is favored in natural selection. This optimistic view must be tempered by two facts. First, some life forms such as blue-green bacteria have remained essentially unchanged for 3.5 billion years. Tropical reefs have also been existence a long time, and the coral reefs of today's oceans are just the current version of a recurrent ecosystem. Life can certainly adapt to a changing environment without ever becoming smart. Second, most species become extinct and do not reappear. There have been an estimated 500 million species of animal and plant life in the Earth's history; 99.8% of those are extinct. We can speculate that if humans disappeared, another intelligent species would evolve, but we cannot be sure.

In considering extraterrestrial life, we must avoid arguments that are anthropocentric, a term that means derivative of our own human experience. It is not safe to assume that intelligence must be associated with the human form (or primates, or any other specific lineage). It is even less safe to assume that alien life will take a human form (although this is the comfortable premise of much science fiction). In addition, we are not only interested in intelligence, but also in technology and the ability to communicate through space. To believe that aliens would understand the universe with our five senses is highly anthropocentric. Consider that on Earth, we have species that have evolved senses based on infrared radiation (snakes), sonar (bats), and magnetic fields (birds). Many animals communicate by chemical means, using pheromones. American scientist Edmund Wilson has estimated the information transfer rate of this method: for a single pheromone, the maximum rate is over 100 bits per second, the equivalent of 20 words of English text per second! In other words, species that we do not consider highly intelligent have evolved sophisticated modes of communication.


A bottlenose dolphin breaching in the bow wave of a boat

On Earth, we might note that it is possible to have intelligence without technology. Dolphins are land mammals that returned to the oceans millions of years ago. They have a similar brain mass to humans and a complex language that is still imperfectly understood by us. They exhibit highly cooperative social behavior, "farming" their food, playing, and rearing their young for a similar amount of time as humans do. There is no indication that dolphins have higher-level, abstract brain functions, but for us, the only important distinction is that technology is limited in an aquatic environment. Dolphins will never point telescopes at the stars and wonder if they are alone in the universe.

Intelligence might exist independently of carbon chemistry. Computers can be programmed to carry out many human functions. from flying a plane to playing world-class chess and Jeopardy. Of course, the ability to carry out calculations at blinding speed does not make a machine intelligent. Current computers are only as good as their programmers; they have no independent thoughts. However, we are within sight of a time when computers may be able to program themselves and improve their own functioning. Networks of many thousands of processors will process information in a scaled-down analogy of the human brain. Nobody knows what the limits of this trend will be. Perhaps in a cosmic setting intelligence can evolve from a biological phase to a computational phase.

It is possible to describe intelligence in terms of the storage and transmission of information. The information contained in the human genome is about 6 × 109 bits. The electrical activity of our brains is controlled by a thousand or so dendrites that project from each brain cell. Each time a brain cell "fires" an electrical contact is made and information is transmitted. So we can think of each connection as potentially a bit of information (electrical signal on or off, 1 or 0). With a trillion brain cells each connected to a thousand other brain cells, the total number of connections is 1012 × 103 = 1015! This is also the number of bits of information the brain could hold. Even if the brain is inefficient at storing information, this vast capability for information storage and processing exceeds anything in our technology. On Earth, life formed as a chemical network, and intelligence formed as an electrical network. It is an enormous challenge to think of the very different forms that life and intelligence might take across the universe. We are not sure enough of the nature and limits of intelligence to estimate the likelihood of intelligent life elsewhere in the universe.


Author: Chris Impey