The Universe
22 flashcards to master The Universe
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The Milky Way galaxy is approximately 100,000 light-years in diameter. A spacecraft travels at a constant speed of 0.00002 light-years per year. Calculate how many years it would take this spacecraft to cross the diameter of the Milky Way.
Time = Distance / Speed
Time = 100,000 light-years / 0.00002 light-years/year
Time = 5,000,000,000 years
Therefore, it would take the spacecraft 5 billion years to cross the Milky Way's diameter. This calculation assumes a straight path and constant speed, which is a simplification.
State two facts about the Milky Way galaxy's place within the Universe.
1. The Milky Way is just one of many billions of galaxies that make up the Universe. This highlights the vast scale of the universe.
2. The diameter of the Milky Way is approximately 100,000 light-years. This provides a sense of the galaxy's scale.
Define redshift in the context of light from distant galaxies.
Redshift is the increase in the observed wavelength (or decrease in frequency) of electromagnetic radiation emitted from stars and galaxies as they recede from the observer. It indicates that the wavelength of light has been stretched, shifting it towards the red end of the spectrum.
State what causes the observed redshift of light from distant galaxies.
The observed redshift of light from distant galaxies is caused by the expansion of the universe, stretching the wavelength of light as it travels towards us. The further away a galaxy is, the faster it recedes and the greater the redshift.
The wavelength of a specific spectral line emitted by hydrogen on Earth is measured to be 656.3 nm. The same spectral line from a distant galaxy is observed to have a wavelength of 669.4 nm. Calculate the change in wavelength (Δλ).
Δλ = Observed wavelength - Rest wavelength
Δλ = 669.4 nm - 656.3 nm
Δλ = 13.1 nm
This calculation determines the shift in wavelength, which is a key indicator of redshift.
Light from distant galaxies exhibits redshift. State what this observation tells us about the motion of these galaxies relative to Earth.
Redshift indicates that the distant galaxies are moving away from the Earth. The greater the redshift, the faster the galaxy is receding. This is evidence for the expansion of the universe.
The wavelength of a specific spectral line from a distant galaxy is observed to be 660 nm. The same spectral line measured in a laboratory on Earth has a wavelength of 600 nm. Calculate the redshift (z) of the galaxy.
z = (observed wavelength - rest wavelength) / rest wavelength
z = (660 nm - 600 nm) / 600 nm
z = 60 nm / 600 nm
z = 0.1
The redshift (z) of the galaxy is 0.1. A positive redshift indicates that the galaxy is moving away from us.
State how the observation of redshift in the light from distant galaxies provides evidence for the Big Bang Theory.
Redshift indicates that galaxies are moving away from us. The greater the distance to a galaxy, the greater its redshift, meaning it is moving away faster. This observation supports the idea that the Universe is expanding from a single point (the Big Bang).
Define cosmic microwave background radiation (CMBR).
Cosmic microwave background radiation (CMBR) is the microwave radiation of a specific frequency observed at all points in space around us.
State two properties of cosmic microwave background radiation (CMBR).
1. It is microwave radiation.
2. It is observed at all points in space.
Explain how the Cosmic Microwave Background Radiation (CMBR) originated shortly after the formation of the Universe and why its wavelength has changed significantly since its creation.
Shortly after the Big Bang, the Universe was extremely hot and dense, filled with high-energy photons. As the Universe expanded, the wavelength of these photons stretched (redshifted) due to the expansion of space itself. This stretching reduced the energy of the photons, shifting them from shorter wavelengths (like gamma rays) to longer wavelengths in the microwave region of the electromagnetic spectrum. The CMBR is the residual radiation from this early stage, now observed as faint microwave radiation coming from all directions in the sky. This observed redshift is evidence for the expansion of the Universe.
State two properties of the Cosmic Microwave Background Radiation (CMBR) that support the Big Bang theory.
1. Uniformity: The CMBR is remarkably uniform in temperature (approximately 2.7 Kelvin) across the entire sky, suggesting a common origin in a very early, hot, and dense Universe. Small temperature fluctuations do exist, and these seed later galaxy formation.
2. Redshift: The CMBR's spectrum corresponds to that of a blackbody radiator that has been significantly redshifted. This redshift is interpreted as evidence for the expansion of the Universe since the CMBR was emitted, supporting the Big Bang model.
A spectral line from a distant galaxy has a wavelength of 660 nm when observed from Earth. The same line has a wavelength of 600 nm when measured in a laboratory. Calculate the speed at which the galaxy is moving away from the Earth, given that the speed of light is 3.0 x 10^8 m/s.
Formula: v = (Δλ / λ₀) * c
where:
v = velocity of the galaxy
Δλ = change in wavelength (observed - rest)
λ₀ = rest wavelength (laboratory measurement)
c = speed of light
Calculation:
Δλ = 660 nm - 600 nm = 60 nm
v = (60 nm / 600 nm) * (3.0 x 10^8 m/s)
v = (0.1) * (3.0 x 10^8 m/s)
v = 3.0 x 10^7 m/s
Answer: The galaxy is moving away at 3.0 x 10^7 m/s. This uses the redshift formula to calculate the recessional velocity.
State how the change in wavelength of starlight from distant galaxies, known as redshift, provides evidence that these galaxies are moving away from the Earth.
Redshift indicates that the observed wavelength of light from a galaxy is longer than its original wavelength. This increase in wavelength implies that the galaxy is moving away from Earth, analogous to the Doppler effect for sound. The greater the redshift, the faster the galaxy is receding.
A supernova in a distant galaxy has an observed brightness that is 1.2 x 10^-15 times the brightness of a similar supernova observed nearby at a distance of 10 Mpc. Calculate the distance to the distant galaxy in Mpc. Assume that the brightness of a supernova is inversely proportional to the square of the distance.
d = √(brightness_nearby / brightness_distant) * distance_nearby
d = √(1 / 1.2 x 10^-15) * 10 Mpc
d = √(8.33 x 10^14) * 10 Mpc
d = 9.13 x 10^7 * 10 Mpc
d = 9.13 x 10^8 Mpc (or 913 million Mpc)
Explanation: The brightness of a supernova decreases with the square of the distance. Therefore, the distance is proportional to the square root of the brightness ratio.
Explain how the observed brightness of a supernova can be used to determine the distance to a far galaxy.
Supernovae of type Ia have a known intrinsic (absolute) brightness. By comparing the observed (apparent) brightness of the supernova in the distant galaxy with its known intrinsic brightness, and applying the inverse square law for brightness, the distance to the galaxy can be estimated. The dimmer the supernova appears, the further away the galaxy is, assuming there is no intervening dust that would dim the supernova's light.
Define the Hubble constant, H₀. State the equation used to calculate it, defining all terms.
The Hubble constant (H₀) is the ratio of a galaxy's recessional velocity (v) to its distance (d) from Earth. Equation: H₀ = v / d, where v is the recessional velocity and d is the distance.
A galaxy is observed to be moving away from Earth at a speed of 2.2 x 10⁶ m/s. Its distance from Earth is estimated to be 3.0 x 10²³ m. Calculate the Hubble constant, H₀, in m/(s*m).
H₀ = v / d
H₀ = (2.2 x 10⁶ m/s) / (3.0 x 10²³ m)
H₀ = 7.3 x 10⁻¹⁸ s⁻¹
Calculate the recessional speed of a galaxy at a distance of 100 Mpc, given that the Hubble constant (H₀) is 2.2 × 10⁻¹⁸ s⁻¹ and 1 Mpc = 3.09 × 10²² m.
v = H₀d
v = (2.2 × 10⁻¹⁸ s⁻¹) × (100 Mpc × 3.09 × 10²² m/Mpc)
v = (2.2 × 10⁻¹⁸ s⁻¹) × (3.09 × 10²⁴ m)
v = 6.798 × 10⁶ m/s
v ≈ 6.8 × 10⁶ m/s
The recessional speed is calculated using Hubble's Law, which relates the recessional velocity of a galaxy to its distance. We converted Mpc to meters and then applied the formula.
Explain what the Hubble constant (H₀) represents in the context of the expanding universe.
The Hubble constant (H₀) represents the rate at which the universe is expanding. Specifically, it's the ratio of a galaxy's recessional velocity (how fast it's moving away from us) to its distance from us. A higher H₀ value implies a faster rate of expansion. Its units are typically expressed as per second (s⁻¹), representing expansion rate per unit distance. The current estimated value for H₀ is approximately 2.2 x 10⁻¹⁸ per second.
The Hubble constant, H₀, is a measure of the Universe's expansion rate. If H₀ is 2.3 x 10⁻¹⁸ s⁻¹, calculate an estimate for the age of the Universe in years. (1 year = 3.154 x 10⁷ seconds)
Age ≈ 1/H₀ = 1 / (2.3 x 10⁻¹⁸ s⁻¹) = 4.35 x 10¹⁷ s.
To convert to years: (4.35 x 10¹⁷ s) / (3.154 x 10⁷ s/year) = 1.38 x 10¹⁰ years.
Answer: 1.38 x 10¹⁰ years. This calculation estimates the time since the Big Bang, the point from which all matter is believed to have originated.
State how the estimated age of the Universe, calculated using the Hubble constant, provides evidence for the Big Bang theory.
The equation Age ≈ 1/H₀ estimates the time since the Universe began expanding. A finite, non-infinite age suggests the Universe started from a single point, supporting the idea that all matter was once concentrated in an extremely small volume, as proposed by the Big Bang theory. This estimated time aligns with independent estimates of the age of the oldest stars and galaxies.
Key Questions: The Universe
Define redshift in the context of light from distant galaxies.
Redshift is the increase in the observed wavelength (or decrease in frequency) of electromagnetic radiation emitted from stars and galaxies as they recede from the observer. It indicates that the wavelength of light has been stretched, shifting it towards the red end of the spectrum.
Define cosmic microwave background radiation (CMBR).
Cosmic microwave background radiation (CMBR) is the microwave radiation of a specific frequency observed at all points in space around us.
Define the Hubble constant, H₀. State the equation used to calculate it, defining all terms.
The Hubble constant (H₀) is the ratio of a galaxy's recessional velocity (v) to its distance (d) from Earth. Equation: H₀ = v / d, where v is the recessional velocity and d is the distance.
About The Universe (6.2.3)
These 22 flashcards cover everything you need to know about The Universe for your Cambridge IGCSE Physics (0625) exam. Each card is designed based on the official syllabus requirements.
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