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A2 Level Astronomy and Cosmology

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2026

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1h 23m

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Release2026

Runtime1h 23m

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6 تبصرے

Millor_GhJul 2, 2026

Link to our latest notes and resources: https://drive.google.com/drive/u/2/folders/15FnZdp3NJ15WmXnkrSWgi5ltd5rUI9Bg 25 Astronomy and cosmology 25.1 Standard candles Candidates should be able to: 1 understand the term luminosity as the total power of radiation emitted by a star 2 recall and use the inverse square law for radiant flux intensity F in terms of the luminosity L of the source F = L/(4πd2 ) 3 understand that an object of known luminosity is called a standard candle 4 understand the use of standard candles to determine distances to galaxies 25.2 Stellar radii Candidates should be able to: 1 recall and use Wien’s displacement law λmax ∝ 1/T to estimate the peak surface temperature of a star 2 use the Stefan–Boltzmann law L = 4πσr 2 T4 3 use Wien’s displacement law and the Stefan–Boltzmann law to estimate the radius of a star 25.3 Hubble’s law and the Big Bang theory Candidates should be able to: 1 understand that the lines in the emission and absorption spectra from distant

@tufathiam364Jul 2, 2026

Link to our latest notes and resources: https://drive.google.com/drive/u/2/folders/15FnZdp3NJ15WmXnkrSWgi5ltd5rUI9Bg 25 Astronomy and cosmology 25.1 Standard candles Candidates should be able to: 1 understand the term luminosity as the total power of radiation emitted by a star 2 recall and use the inverse square law for radiant flux intensity F in terms of the luminosity L of the source F = L/(4πd2 ) 3 understand that an object of known luminosity is called a standard candle 4 understand the use of standard candles to determine distances to galaxies 25.2 Stellar radii Candidates should be able to: 1 recall and use Wien’s displacement law λmax ∝ 1/T to estimate the peak surface temperature of a star 2 use the Stefan–Boltzmann law L = 4πσr 2 T4 3 use Wien’s displacement law and the Stefan–Boltzmann law to estimate the radius of a star 25.3 Hubble’s law and the Big Bang theory Candidates should be able to: 1 understand that the lines in the emission and absorption spectra from distant

la meuf de tiktokJul 2, 2026

Link to our latest notes and resources: https://drive.google.com/drive/u/2/folders/15FnZdp3NJ15WmXnkrSWgi5ltd5rUI9Bg 25 Astronomy and cosmology 25.1 Standard candles Candidates should be able to: 1 understand the term luminosity as the total power of radiation emitted by a star 2 recall and use the inverse square law for radiant flux intensity F in terms of the luminosity L of the source F = L/(4πd2 ) 3 understand that an object of known luminosity is called a standard candle 4 understand the use of standard candles to determine distances to galaxies 25.2 Stellar radii Candidates should be able to: 1 recall and use Wien’s displacement law λmax ∝ 1/T to estimate the peak surface temperature of a star 2 use the Stefan–Boltzmann law L = 4πσr 2 T4 3 use Wien’s displacement law and the Stefan–Boltzmann law to estimate the radius of a star 25.3 Hubble’s law and the Big Bang theory Candidates should be able to: 1 understand that the lines in the emission and absorption spectra from distant

ibrahimbathily2020Jul 2, 2026

Link to our latest notes and resources: https://drive.google.com/drive/u/2/folders/15FnZdp3NJ15WmXnkrSWgi5ltd5rUI9Bg 25 Astronomy and cosmology 25.1 Standard candles Candidates should be able to: 1 understand the term luminosity as the total power of radiation emitted by a star 2 recall and use the inverse square law for radiant flux intensity F in terms of the luminosity L of the source F = L/(4πd2 ) 3 understand that an object of known luminosity is called a standard candle 4 understand the use of standard candles to determine distances to galaxies 25.2 Stellar radii Candidates should be able to: 1 recall and use Wien’s displacement law λmax ∝ 1/T to estimate the peak surface temperature of a star 2 use the Stefan–Boltzmann law L = 4πσr 2 T4 3 use Wien’s displacement law and the Stefan–Boltzmann law to estimate the radius of a star 25.3 Hubble’s law and the Big Bang theory Candidates should be able to: 1 understand that the lines in the emission and absorption spectra from distant

Abi Nas❤️❤️Jul 2, 2026

Link to our latest notes and resources: https://drive.google.com/drive/u/2/folders/15FnZdp3NJ15WmXnkrSWgi5ltd5rUI9Bg 25 Astronomy and cosmology 25.1 Standard candles Candidates should be able to: 1 understand the term luminosity as the total power of radiation emitted by a star 2 recall and use the inverse square law for radiant flux intensity F in terms of the luminosity L of the source F = L/(4πd2 ) 3 understand that an object of known luminosity is called a standard candle 4 understand the use of standard candles to determine distances to galaxies 25.2 Stellar radii Candidates should be able to: 1 recall and use Wien’s displacement law λmax ∝ 1/T to estimate the peak surface temperature of a star 2 use the Stefan–Boltzmann law L = 4πσr 2 T4 3 use Wien’s displacement law and the Stefan–Boltzmann law to estimate the radius of a star 25.3 Hubble’s law and the Big Bang theory Candidates should be able to: 1 understand that the lines in the emission and absorption spectra from distant

the._.B O N D._.007Jul 2, 2026

Link to our latest notes and resources: https://drive.google.com/drive/u/2/folders/15FnZdp3NJ15WmXnkrSWgi5ltd5rUI9Bg 25 Astronomy and cosmology 25.1 Standard candles Candidates should be able to: 1 understand the term luminosity as the total power of radiation emitted by a star 2 recall and use the inverse square law for radiant flux intensity F in terms of the luminosity L of the source F = L/(4πd2 ) 3 understand that an object of known luminosity is called a standard candle 4 understand the use of standard candles to determine distances to galaxies 25.2 Stellar radii Candidates should be able to: 1 recall and use Wien’s displacement law λmax ∝ 1/T to estimate the peak surface temperature of a star 2 use the Stefan–Boltzmann law L = 4πσr 2 T4 3 use Wien’s displacement law and the Stefan–Boltzmann law to estimate the radius of a star 25.3 Hubble’s law and the Big Bang theory Candidates should be able to: 1 understand that the lines in the emission and absorption spectra from distant