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M1\n- Explains that when the core temperature and density become high enough, hydrogen nuclei undergo nuclear fusion to form helium. M1\n- Explains that hydrostatic equilibrium is achieved when the outward radiation pressure (and gas pressure) from fusion perfectly balances the inward force of gravity. A1","marks":3,"order":0,"markingRubric":null,"tableImages":[],"explanation":{"methods":[{"id":"stellar_formation","label":"Follow stellar formation","steps":[{"type":"text","order":0,"title":"Identify the starting change","content":"The cloud is contracting under gravity. As particles move closer together, energy is transferred from the **gravitational potential energy store** to the **thermal energy store** of the gas and dust.\n\nThis makes the centre hotter and raises its pressure, producing a **protostar**. This full energy-transfer explanation earns **M1**.","highlights":[{"text":"undergoing gravitational contraction","location":"specification"}]},{"type":"text","order":1,"title":"Start nuclear fusion","content":"Continued contraction makes the protostar's core increasingly hot and dense. Once these conditions are high enough, **hydrogen nuclei fuse to form helium nuclei**.\n\nThis identifies the nuclear process required for **M1**.","highlights":[{"text":"transitions into a stable main sequence star","location":"specification"}]},{"type":"text","order":2,"title":"Establish equilibrium","content":"Fusion releases energy, producing outward **radiation pressure** and gas pressure. A stable main sequence star has **hydrostatic equilibrium** when these outward pressures exactly balance the inward force of gravity, so there is no overall tendency for the star to expand or contract.\n\nMaking the balance explicit earns **A1**.","highlights":[{"text":"explaining how hydrostatic equilibrium is established","location":"specification"}]}]}],"generatedAt":"2026-07-22T12:00:06.111Z","modelVersion":"gpt-5.6-terra+diagrams-1","explanationVersion":"v3"},"options":[]}],"options":[],"explanation":null,"firstAttemptFullMarks":null,"walkthroughVideo":null},{"id":"64129771-4d89-429f-9bfa-e207194597eb","revisionId":"2dea0d21-a274-42a9-9a59-fd758edc004f","questionNumber":null,"questionType":"LA","specification":"","difficulty":5,"difficultyBand":"medium","tier":null,"totalMarks":3,"sourceTitle":null,"calculatorUse":null,"isCalculation":false,"parts":[{"id":"1a288d21-09d2-4220-b232-97ed9ba4ae6e","label":null,"content":"Explain why a protostar stops contracting and reaches a stable state as a main sequence star.","markscheme":"- Gravitational contraction increases core temperature and density/pressure until hydrogen nuclei undergo nuclear fusion B1\n- This fusion reaction releases energy, creating an outward radiation (and gas) pressure B1\n- The outward pressure balances the inward gravitational force, preventing further collapse and establishing a stable state B1","marks":3,"order":0,"markingRubric":null,"tableImages":[],"explanation":{"methods":[{"id":"stellar_balance","label":"Stellar force balance","steps":[{"type":"text","order":1,"title":"Heat the core","content":"Gravity pulls the protostar's material inwards, so it contracts. This raises the core's temperature and density (and therefore its pressure) until hydrogen nuclei can undergo **nuclear fusion**: joining together to form heavier nuclei.\n\nThis cause-and-effect statement earns the first mark.","highlights":[{"text":"Explain why a protostar stops contracting and reaches a stable state as a main sequence star.","location":"specification"}]},{"type":"text","order":2,"title":"Release fusion energy","content":"Fusion releases energy from the core. This energy creates an outward **radiation and gas pressure** that pushes against the star's material.\n\nState both the energy release and the outward pressure for the second mark."},{"type":"text","order":3,"title":"Balance the forces","content":"The outward pressure balances the inward gravitational force. With no unbalanced inward force, the star stops collapsing and remains stable as a main sequence star.\n\nThat explicit balance and conclusion earns the final mark."}]}],"generatedAt":"2026-07-22T11:49:43.662Z","modelVersion":"gpt-5.6-terra+diagrams-1","explanationVersion":"v3"},"options":[]}],"options":[],"explanation":null,"firstAttemptFullMarks":null,"walkthroughVideo":null},{"id":"7ec56792-5043-4e4c-8cb7-1dd9174d5de9","revisionId":"31589c93-f69a-4e3a-a806-0981fa12fa4e","questionNumber":null,"questionType":"MC","specification":"An astrophysicist observes a massive main-sequence star with an initial mass of $30\\,M_{\\odot}$ (where $M_{\\odot}$ is the solar mass).\n\nWhich of the following correctly describes the main-sequence lifetime of this star compared to the Sun, and its eventual evolutionary remnant?","difficulty":8,"difficultyBand":"medium","tier":null,"totalMarks":1,"sourceTitle":null,"calculatorUse":null,"isCalculation":false,"parts":[],"options":[{"id":"5a3fbcbd-6faf-4c2e-8162-1b6ef8c8738a","content":"It has a shorter main-sequence lifetime than the Sun, and eventually collapses to form a black hole because its remaining core mass exceeds $3\\,M_{\\odot}$.","correct":true,"markscheme":"Correct. High-mass stars fuse fuel much faster, giving them shorter lifetimes. A $30\\,M_{\\odot}$ star undergoes a supernova and leaves behind a core mass $> 3\\,M_{\\odot}$, collapsing into a black hole.","order":0,"metadata":null},{"id":"84ad457a-9139-41c6-876c-392698264e5c","content":"It has a shorter main-sequence lifetime than the Sun, and eventually collapses to form a neutron star because its remaining core mass is between $1.4\\,M_{\\odot}$ and $3\\,M_{\\odot}$.","correct":false,"markscheme":"Incorrect. While the lifetime is indeed shorter, a star of $30\\,M_{\\odot}$ has a core remnant exceeding $3\\,M_{\\odot}$, which collapses into a black hole rather than a neutron star.","order":1,"metadata":null},{"id":"4004e315-5e72-4a1d-a858-f7d3a2c6b9c8","content":"It has a longer main-sequence lifetime than the Sun, and eventually collapses to form a black hole because its remaining core mass exceeds $3\\,M_{\\odot}$.","correct":false,"markscheme":"Incorrect. This assumes that more fuel leads to a longer lifetime, failing to account for the vastly higher fusion rate in high-mass stars.","order":2,"metadata":null},{"id":"584c3510-300b-4f5a-8b5e-f6b3c0af0d21","content":"It has a longer main-sequence lifetime than the Sun, and eventually collapses to form a neutron star because its remaining core mass is between $1.4\\,M_{\\odot}$ and $3\\,M_{\\odot}$.","correct":false,"markscheme":"Incorrect. This combines both errors: assuming more fuel leads to a longer lifetime, and incorrectly identifying the remnant as a neutron 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Stars","topicId":"210a9b55-b8b7-5b21-9cde-e0c5ac403c85","topicSidebar":"$L3c","topicSlug":"stellar-evolution-and-observing-the-universe","topicTitle":"7.3 Stars"}]}],"$L3d","$L3e"]}]

7.3 Stars

Question 5

7.3 Stars Questions

7.3 Stars

Question 5

7.3 Stars Questions