Physical Science - Module 1: Heavy Elements Formation

The process of creating new atomic nuclei from pre-existing nuclei.

The formation of elements inside stars through nuclear fusion, starting with lighter elements like Hydrogen and Helium.

The process by which the universe began from a tiny, dense, and hot point 13.8 billion years ago, leading to its expansion and cooling.

The creation of the first light elements like Hydrogen and Helium during the Big Bang.

A huge cloud of gas and dust in space. It is the starting point for star formation.

A dense region within a nebula where gravity begins to pull together gas and dust. It is the first stage of star formation.

A stage in a star's life where nuclear fusion starts at its core, converting Hydrogen into Helium.

A star's core fuses Helium into Carbon and Oxygen. It is an expanded and cooler stage compared to the main sequence.

A larger and hotter version of a red giant, formed by massive stars. It fuses heavier elements like Carbon and Oxygen.

The explosion of a massive star at the end of its life, releasing massive amounts of energy and heavy elements into space.

A collapsed core of a star after a supernova, being extremely dense and with a very strong gravitational pull.

A region in space where gravity is so strong that nothing, not even light, can escape. It can form after a massive star collapses.

The remnant of an average star after it has run out of fuel. It is a small and dense, cool object.

A hypothetical object formed from a white dwarf that has cooled down completely and no longer emits light or heat.

A process in a red giant star where three Helium-4 nuclei fuse to form Carbon.

A series of nuclear fusion reactions that happen in massive stars, converting Hydrogen into Helium through Carbon, Nitrogen, and Oxygen.

A process in red supergiant stars where heavier elements are created, building up from Carbon to Iron.

The way elements heavier than Iron are formed. A neutron is captured by a seed nucleus, increasing the atomic mass.

A slow process of neutron capture, where radioactive decay occurs between neutron captures, resulting in an increase in the number of protons.

A rapid process of neutron capture, where many neutrons are captured before radioactive decay can happen, resulting in a significant increase in atomic mass.

The formation of heavy elements like Iron and beyond, happening during the supernova explosion of massive stars.

A series of nuclear fusion reactions that occur in main sequence stars, converting Hydrogen into Helium through deuterium and Helium-3 intermediates.

The elements that formed during the Big Bang, like Hydrogen, Helium, and traces of Lithium and Beryllium.

The heavier elements formed through nuclear fusion and other processes in stars, such as Carbon, Oxygen, and Iron.

The fusion of two Helium-4 nuclei to form Beryllium-8, which then fuses with another Helium-4 nucleus to form Carbon-12.

A star's energy is derived from the process of nuclear fusion. This is how stars shine so brightly.

A star's final fate depends on its initial mass and composition. Stars with different compositions and masses have different lifecycles.

Stars can be classified by their mass and temperature. Massive stars are typically hotter and have shorter lifespans.

The death of a star can lead to the creation of new stars and planetary systems. Heavy elements released by supernovae can form new nebulae.