Lectures

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  1. Unveiling Cosmic Mysteries

  In our introductory lecture, we enter the fascinating world of black holes, wormholes, and Einstein’s legacy of general relativity, exploring why these objects captivate scientists and the public alike. We trace their history from John Michell’s 18th-century dark star hypothesis through Schwarzschild’s event horizon and Chandrasekhar’s pioneering work on stellar limits. Along the way, we consider the human stories of triumph and discrimination that shaped the field before connecting these foundations to modern discoveries and introducing key concepts such as Newton’s laws of gravitation, Einstein’s equivalence principle, and gravitational lensing.
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  2. Seeing the Invisible

  In lecture two, we learn how black holes, though invisible, can be detected through their interactions with stars and accretion discs. Examples such as Cygnus X-1 and the Event Horizon Telescope’s image of M87 reveal the key properties of black holes: mass, charge, and spin. We then introduce Einstein’s special relativity, examining the constancy of light’s speed and its consequences, including time dilation, length contraction, and mass-energy equivalence. We connect these principles to black holes and consider how fascinating concepts like Hawking radiation and the information paradox continue to challenge our understanding of physics and time.
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  3. When Gravity Bends Time

  In lecture three, we explore the evolution of gravitational theory from Newton’s law of universal gravitation through Einstein's general relativity, examining how mass curves space-time and the profound consequences this has for our understanding of the universe. We examine the equivalence principle, gravitational time dilation and redshift, and practical applications such as GPS. We then turn to black holes, exploring the Schwarzschild solution for the simplest black holes, event horizons, and the contrasting experiences of observers inside versus outside a black hole, including the phenomenon of spaghettification.
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  4. Anatomy of a Black Hole

  In lecture four, Dr. Keating details the structure and observable features of black holes, including the event horizon, photon sphere, ergosphere, and singularity, and how tidal forces and spaghettification depend on black hole mass. Together, we then turn to the Kerr solution, revealing how spin shrinks the event horizon, boosts energy-conversion efficiency, and helps explain the extraordinary luminosity of quasars. Finally, we trace how stellar evolution produces black holes, showing how a star’s initial mass determines its fate and linking stellar astrophysics with general relativity.
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  5. Observing Black Holes

  In lecture five, we analyze the mounting evidence for the existence of a supermassive black hole at the center of our Milky Way Galaxy, Sagittarius A*, examining how decades of infrared observations by Nobel laureates Andrea Ghez and Reinhard Genzel tracked stars orbiting an unseen massive object. We then connect these observations to the Event Horizon Telescope’s imaging of the black hole’s photon sphere shadow, showing how independent optical, infrared, and radio evidence converge to confirm its existence and properties. Finally, we examine how the detection of two distant black holes merging provided further confirmation of general relativity and opened a new way of observing the universe.
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  6. Wormholes & Quantum Mechanics

  In lecture six, Dr. Keating presents wormholes as theoretical constructs arising from general relativity, examining their structure, the immense challenges of creating and stabilizing them, and their portrayal in popular culture. He then introduces foundational principles of quantum mechanics, including wave-particle duality, Heisenberg’s uncertainty principle, superposition, and entanglement, as essential tools for understanding the frontier physics of black holes. The lecture concludes by identifying the lack of a quantum theory of gravity as a critical gap in modern physics, setting the stage for black hole thermodynamics and Hawking radiation.
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  7. Entropy & Thermodynamics

  In lecture seven, we study the profound connections between thermodynamics, quantum mechanics, and gravity at black hole event horizons. We trace the development of thermodynamics and Boltzmann’s concept of entropy, then examine Bekenstein and Hawking’s discovery that black holes possess entropy and temperature and emit Hawking radiation, eventually evaporating. We investigate the black hole information paradox—the unresolved question of whether information thrown into a black hole is truly destroyed. We conclude with Lee Smolin’s controversial theory of cosmic natural selection, in which black holes may seed new universes in a multiverse.
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  8. Journeys Through Space-time

  In our eighth and final lecture, Dr. Keating explores the physics behind the film Interstellar, examining the fictional black hole Gargantua, its extreme spin, the Kerr metric, ergosphere, and Penrose process, and how physicist Kip Thorne and the visual effects team brought these concepts to life. We then review the course journey from Newtonian gravity through relativity, black hole physics, stellar evolution, gravitational waves, and multi-messenger astronomy, highlighting the human stories behind these scientific breakthroughs. The lecture concludes with a Q&A exploring the connections between information, energy, and profound questions about the cosmos.