Free Course Image Astrophysics and Cosmology Course

Free online course Astrophysics and Cosmology Course

Duration of the online course: 1 hours and 24 minutes

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Boost your physics skills with this free online course in astrophysics and cosmology—stars, distances, and the expanding universe, plus practice questions.

In this free course, learn about

  • How stars form from collapsing interstellar clouds and what triggers collapse
  • Stellar evolution pathways by mass: main sequence, red giant, supergiant outcomes
  • Why some stars become white dwarfs and the mass limits that determine endpoints
  • Post–red giant stages for high-mass stars (e.g., supergiant, supernova, remnants)
  • Parallax method for stellar distances and the relation d = 1/p
  • Definition of a parsec and its link to 1 arcsecond parallax
  • Compute distances for given parallaxes (e.g., 1 arcsecond corresponds to 1 pc)
  • Using Doppler/redshift ideas in cosmology and what they indicate about motion
  • Hubble’s Law and what it implies about expansion of the Universe
  • Cosmic Microwave Background Radiation: what it is and why it matters
  • Applying astrophysics/cosmology concepts to A Level-style practice questions

About the free online course

Build a clear, exam-ready understanding of how the universe works, from the life cycle of stars to the evidence for cosmic expansion. This free online course is designed for learners who want to strengthen core physics knowledge in astrophysics and cosmology with explanations that connect key ideas into a coherent picture, rather than leaving you with disconnected facts.

You will explore how stars form when interstellar clouds collapse and what conditions can trigger that process. From there, you will follow stellar evolution through major stages and learn what ultimately determines a star’s final fate. By focusing on the physics behind outcomes such as white dwarfs and what can come after the red giant phase for very massive stars, you’ll gain intuition about how mass, pressure, temperature, and gravity shape a star’s journey.

On the cosmology side, the course helps you become confident with the measurements that allow astronomers to map the universe. You’ll understand how parallax is used to calculate distances, what a parsec actually means, and how the simple relationship between distance and parallax fits into real problem solving. You’ll also connect observational tools like Doppler effects with larger-scale ideas such as Hubble’s Law and the cosmic microwave background, building an evidence-based view of an expanding universe.

Throughout the course, short focused questions and practice-style problems reinforce what you learn so you can apply definitions and equations accurately under exam conditions. By the end, you should be able to explain stellar birth and evolution in physical terms, interpret basic astronomical distance measurements, and describe the observational foundations of modern cosmology with far more confidence.

Course content

  • Video class: A Level Physics Revision: All of Astrophysics (in under 25 minutes!) 24m
  • Exercise: What determines whether a star becomes a white dwarf?
  • Video class: A Level Physics: Star formation and evolution 10m
  • Exercise: What triggers the birth of a star from a collapsing interstellar cloud?
  • Video class: A Level Physics Revision: All of Cosmology | Parallax, parsecs, Doppler, CMBR, Hubble's Law 19m
  • Exercise: What is the definition of a parsec?
  • Video class: A Level Physics: parallax, the parsec, d=1/p 11m
  • Exercise: What is the distance to a star with a parallax of 1 arc second?
  • Video class: A Level Physics Revision: Astrophysics and Cosmology Practice Questions 17m
  • Exercise: Which stage follows the red giant phase for stars much more massive than the Sun?

This free course includes:

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1 hours and 24 minutes of online video course

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Digital certificate of course completion (Free)

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Exercises to train your knowledge

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100% free, from content to certificate

What is a parsec, and how is it calculated from parallax?

A parsec is the distance at which 1 AU subtends an angle of 1 arcsecond. Distance in parsecs is calculated as d = 1/p, where p is parallax in arcseconds.

What determines whether a star becomes a white dwarf or undergoes a supernova?

Its initial mass is the key factor. Low- and medium-mass stars shed their outer layers and leave white dwarfs, while very massive stars can explode as supernovae.

How do redshift and Hubble's law provide evidence for an expanding universe?

Light from distant galaxies is redshifted, showing they are moving away. Hubble's law shows that more distant galaxies generally recede faster, supporting cosmic expansion.

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