Course finale and summary. We look back over where we've been the last eleven weeks, and bring together all of the main themes of this course on Life in the Universe. Recorded live on 2009 Dec 4 in Room 1005 Smith Laboratory on the Columbus campus of The Ohio State University.

How will life, the Universe, and everything end? This lecture looks at the evolution of our expanding Universe to project the prospects for life into the distant cosmological future. Recent observations show that we live in an infinite, accelerating universe. I will trace the evolution of the universe from the current age of stars into the future. The final state of the Universe will be cold, dark, and disordered, and ultimately inhospitable to life as we understand it or perhaps...

What is the future of life on Earth and in our Solar System? The Sun is the source of energy for life on the Earth, but it will not shine forever. This lecture looks at the impact of the various stages of the evolution of the Sun on the habitability of the Solar System, with particular emphasis on the continued habitability of the Earth. I will refer to state-of-the-art computer models of the Sun to get is properties at various stages in its past and future life. NOTE: Due to a recorder...

What does extraterrestrial life look like? This lecture explores current thinking about what extraterrestrial life might be like not by guessing their appearances, but instead applying lessons learned from our growing understanding of how evolution and biochemistry work on Earth. I will discuss Universal versus Parochial characteristics, Convergent Evolution, Radical Diversity, and other ideas from evolutionary biology that might inform how life might emerge on other worlds. We will then...

So, Where is Everybody? Interstellar colonization, in principle, is an exponential growth process that would fill the galaxy in a few million years even with a very modest star flight capability. This is a small fraction of the lifetime of the Milky Way Galaxy, so the Galaxy should be teaming with life. But, we so far have no compelling evidence of extraterrestrial visitations, alien artifacts, or any other evidences that the Galaxy is populated. Physicist and Nobel Laureate...

If we ever detect life elsewhere, how will we go visit? This lecture considers the challenges of interstellar travel and colonization. The problem is one of basic physics (the enormous energy requirements of star flight) coupled with the vast, irreducible distances between the stars. I will describe various starship concepts that use reasonable extrapolations of current technologies (nuclear propulsion and solar sails), ignoring for our discussions science-fiction exotica...

Is anybody out there? This lecture reviews the ideas behind SETI, the Search for Extra-Terrestrial Intelligence, an effort to find other intelligent communicating civilizations by tuning in on their radio or other electromagnetic communications. I will discuss the basic approaches being taken by various SETI efforts, and what we expect to find. In addition to listening, we have also been broadcasting, intentionally or otherwise, messages into space, and we have sent physical artifacts with...

How many intelligent, communicating civilizations live in our Galaxy? We have no idea. One way to approach the question and come up with quasi-quantitative estimates is the Drake Equation, first introduced by radio astronomy Frank Drake in the 1960s. I will use the Drake equation as an illustration of the issues related to the question of extraterrestrial intelligence, and to set the stage for future lectures on the likelihood of finding other intelligences in our Universe. Recorded live on...

Are there other Earths out there? Do they have life on them? This lecture looks at the search for ExoEarths - Earth-sized planets in the habitable zones of their parent stars, and what we might learn from measuring them. The ultimate goal of all planet searches is to find other Earth's, what the late Carl Sagan so poetically called the "pale blue dot" as seen from the depths of space. This lecture discusses what we might learn about such planets from studies of our own Earth,...

What are the properties of the 400+ exoplanets we have discovered so far? This lecture reviews the properties of exoplanets, and finds a couple of surprises: Jupiter-mass planets orbiting close to their parent stars, and Jupiter-mass planets in very elliptical orbits. Both seem to require some mechanism for migration: strong gravitational interactions with either the protoplanetary disk or other giant planets to cause the planets to move inward from their birth places beyond the "Ice...

Are there planets around other stars? This lecture reviews the methods used to hunt for exoplanets and the results thus far. I will describe direct imaging methods, indirect methods relying on the gravitational influence of the planet on its parent star, planetary transits in which a planet blocks part of its parent star's light, and gravitational microlensing. There has been an explosion in our knowledge of planets around other stars, from little or nothing in the early 1990s to more than...

What stars are near the Sun? Now that we have some idea of what we are looking for - rocky planets in the habitable zones of low-mass main-sequence stars - what are the prospects near the Sun? This lecture examines the hunting ground for planets, the nearby stars that make up the Solar Neighborhood. I will describe our nearest neighbor, the Proxima Centauri/Alpha Centauri triple system, and then look at the properties of our nearest stellar neighbors. What we will find is that G-type...

Which stars are the most hospitable for life? This lecture examines the factors affecting the habitability of stars, with a goal of understanding where we should search for life-bearing planets. We will do this by generalizing the idea of a Habitable Zone developed for the Sun back in Lecture 30. In this context, we find that the best places to search for life would be rocky planets in the habitable zones of low-mass main-sequence stars. There are a number of caveats we will discuss -...

What happens to a star when it runs out of hydrogen in its core? This lecture describes the post main-sequence evolution of stars. What happens depends on the star's mass. Low mass stars swell up into Red Giants, and eventually shed their envelopes and end their lives as white dwarf stars. High mass stars become Red Supergiants, and if large enough, end their lives in a spectacular supernova explosion that leaves behind a neutron star or black hole. The explosion itself creates massive...

Why do stars shine? How long do they shine? This lecture describes the physics of stars on the main sequence, describes the mass-luminosity relation of main sequence stars, introduces nuclear fusion power and the nuclear fusion lifetimes of stars. From this we gain an important insight into one of the criteria we might apply to the search for life around other stars: we want planets around low-mass main sequence stars that can shine more or less steadily for more that 500 Myr to 1...

What are the observed properties of stars? This lecture is a quick review of the basic observational properties of stars, introducing luminosity, spectral classification, the luminosity-radius-temperature relation, and the Hertzsprung-Russell (H-R) diagram. This sets up the empirical basis of subsequent lectures on the lives and deaths of stars. Recorded live on 2009 Nov 9 in Room 1005 Smith Laboratory on the Columbus campus of The Ohio State University.

Why is the Earth habitable today but Venus and Mars not? This lecture explores the question of planetary habitability from the perspective of the stability of liquid water on the surface of planetary bodies. We will see how the amount of sunlight and the greenhouse effect in the atmosphere combine to create a classic Goldilocks problem: whether or not a planetary surface has stable liquid water is a question of not being too hot or too cold. This defines the Habitable Zone for...

Among the 61 known moons of Saturn, two stand out: Enceladus and Titan. Giant Titan is the only moon in our Solar System with a substantial atmosphere, composed of nitrogen and methane, dense enough to maintain a weather cycle with methane analogous to the water cycle on Earth, even including great lakes of liquid methane and ethane at the poles. Enceladus has fountains of water vapor and ice particles that coat its surface in fresh ices, and indicates the presence of liquid water beneath its...

The four large Galilean Moons of Jupiter seem unlikely places to look for life; at first glance they should be cold, dead, icy worlds. Instead we find tremendous geological diversity, and two big surprises: volcanically-active Io, and icy Europa. Io is the most volcanically active world in the Solar System, heated by tides from Jupiter. Europa is even more surprising: its icy surface is young, with few impact craters and extensive signs of recent repaving by liquid water. Even more...

Is there life on Mars? We begin with a brief historical survey of the idea of inhabitable Mars, from Herschel to Lowell, and look at how the idea of Mars and Martians is deeply embedded in the popular culture. We then turn to spacecraft explorations of Mars, and how they have changed our view of the Red planet. We will discuss the on-going search of Martian life, past and present, particularly the Viking 1 and 2 experiments, the Allan Hills Meteorite controversy, Mars Methane, and...

For many, the most likely place in the Solar System to search for life beyond the Earth is Mars. This lecture describes the properties of Mars, a desert world with a thin, dry, cold carbon dioxide atmosphere. I will review evidence that has begun to point unequivocally to the conclusion that Mars had flowing and standing liquid water on its surface in the past, perhaps during the first billion years or so. If Mars had a warm, wet past, did life also get a start there? Recorded live on 2009...

Having completed our tour of the Solar System, we now turn to a discussion of the requirements for life, and where those requirements might be satisfied elsewhere in the Solar System. Some - energy, complex chemistry, and liquid water - seem obvious, but they are not the only possibilities or considerations. At the end, we will have a short list of possible places to look, some expected, others surprising. Recorded live on 2009 Oct 29 in Room 1005 Smith Laboratory on the Columbus campus of...

We turn our attention to the Giant Planets of the outer Solar System: the gas giants Jupiter and Saturn, and the ice giants Uranus and Neptune. We will review their structure and properties, and then examine their systems of moons, with special attention to the giant moons. While the Jovian planets themselves seem unlikely places to hunt for life in our Solar System, a few of their largest moons may be more promising than appears at first sight. We'll explore this further in...

We follow our tour of our Solar System with an in-depth comparison of the Terrestrial Planets. In particular, we want to contrast and compare their geological and atmospheric histories. This will inform our inquiry into whether or not we expect to find life on these worlds. Recorded live on 2009 Oct 27 in Room 1005 Smith Laboratory on the Columbus campus of The Ohio State University.