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24:[["$","$L33",null,{"feature":"flashcards"}],"$L34",["$","$L35",null,{"href":"/a-level/physics/ocr/a/cosmology/flashcards","label":"Cosmology","subjectCode":"a_level_physics__ocr_a","surface":"flashcards"}],["$","$L36",null,{"runner":["$","div",null,{"className":"min-h-0 flex-1 overflow-hidden bg-background","children":["$","$L37",null,{"decks":[{"id":"797262de-a084-4642-a3d6-6f2e3403f6a1","title":"Cosmology Flashcards","topicId":"d1cad92d-e182-5433-836c-69872a50500d","topicSlug":"cosmology","cards":[{"id":"cd7077dd-062f-4a0a-b6bf-b1f9b070d541","cardType":"basic","points":1,"front":"Define the astronomical unit (AU).","back":"The mean distance between the Earth and the Sun.","mcqOptions":[{"text":"The mean distance between the Earth and the Sun.","correct":true,"explanation":"The astronomical unit is defined using the average separation of Earth and the Sun, providing a convenient distance scale for measurements within the Solar System."},{"text":"The mean distance between the Earth and the Moon.","correct":false,"explanation":"The mean Earth-Moon distance is about 384,400 km and is not an astronomical unit. An AU is the mean distance between Earth and the Sun."},{"text":"The mean distance between the Sun and Neptune.","correct":false,"explanation":"The Sun-Neptune separation is roughly 30 AU, so it cannot define one AU. One AU is the mean distance between Earth and the Sun."},{"text":"The mean radius of the Sun measured from its centre.","correct":false,"explanation":"The Sun’s radius measures the size of the Sun rather than an orbital distance. An AU is the mean distance between Earth and the Sun."}]},{"id":"8779c65d-a235-4891-b34c-266de147bafe","cardType":"cloze","points":null,"front":"The distance light travels in one year is 1 light-year, which is approximately $\\text{[...]}$.","back":"The distance light travels in one year is 1 light-year, which is approximately $\\boxed{9.46 \\times 10^{15}\\ \\text{m}}$.","mcqOptions":[{"text":"$$9.46 \\times 10^{15}\\ \\text{m}$","correct":true,"explanation":"Multiplying the speed of light, approximately $3.00 \\times 10^8\\ \\text{m s}^{-1}$, by the number of seconds in one year gives $9.46 \\times 10^{15}\\ \\text{m}$."},{"text":"$$9.46 \\times 10^{14}\\ \\text{m}$","correct":false,"explanation":"This is a factor of ten too small, typically from using the wrong power of ten for the seconds in a year. One light-year is $9.46 \\times 10^{15}\\ \\text{m}$."},{"text":"$$9.46 \\times 10^{16}\\ \\text{m}$","correct":false,"explanation":"This is a factor of ten too large, caused by increasing the exponent unnecessarily. Multiplying light speed by one year gives $9.46 \\times 10^{15}\\ \\text{m}$."},{"text":"$$1.50 \\times 10^{11}\\ \\text{m}$","correct":false,"explanation":"This confuses a light-year with the much smaller astronomical unit, which is about $1.50 \\times 10^{11}\\ \\text{m}$. A light-year is $9.46 \\times 10^{15}\\ \\text{m}$."}]},{"id":"c67e622f-7c47-411c-bf63-f0d6425d8577","cardType":"basic","points":1,"front":"Define a parsec (pc) in terms of angle.","back":"The distance at which 1 AU subtends an angle of 1 arcsecond.","mcqOptions":[{"text":"The distance at which 1 AU subtends an angle of 1 arcsecond.","correct":true,"explanation":"A parsec is defined geometrically as the distance from which a baseline of 1 AU has an angular size of exactly 1 arcsecond."},{"text":"The distance at which 1 AU subtends an angle of 1 arcminute.","correct":false,"explanation":"An arcminute is 60 arcseconds, so this angle would give a distance 60 times smaller than a parsec. The defining angle is 1 arcsecond."},{"text":"The distance at which 1 AU subtends an angle of 1 degree.","correct":false,"explanation":"One degree is 3600 arcseconds, making the corresponding distance far smaller than one parsec. A parsec uses 1 AU subtending 1 arcsecond."},{"text":"The distance at which 1 light-year subtends an angle of 1 arcsecond.","correct":false,"explanation":"This incorrectly replaces the 1 AU baseline with a light-year. A parsec is the distance at which 1 AU subtends an angle of 1 arcsecond."}]},{"id":"e32b619e-bb35-4d7a-8126-d9f597082a32","cardType":"basic","points":1,"front":"How many arcseconds are in 1 degree?","back":"3600","mcqOptions":[{"text":"3600","correct":true,"explanation":"Each degree contains 60 arcminutes and each arcminute contains 60 arcseconds, so one degree contains $60 \\times 60 = 3600$ arcseconds."},{"text":"60","correct":false,"explanation":"This gives only the number of arcminutes in one degree, overlooking the additional 60 arcseconds in every arcminute. The correct total is 3600."},{"text":"36000","correct":false,"explanation":"This results from multiplying by an extra factor of ten after converting through arcminutes. Since $60 \\times 60 = 3600$, one degree contains 3600 arcseconds."},{"text":"1800","correct":false,"explanation":"This is the number of arcseconds in half a degree, not a full degree. One degree contains $60 \\times 60 = 3600$ arcseconds."}]},{"id":"270fa662-b02f-4dc1-8361-874324b48002","cardType":"basic","points":1,"front":"What is the relationship between distance $d$ and parallax angle $p$?","back":"$$$d = \\frac{1}{p}$$ (where $d$ is in parsecs and $p$ is in arcseconds)","mcqOptions":[{"text":"$$$d = \\frac{1}{p}$$ (where $d$ is in parsecs and $p$ is in arcseconds)","correct":true,"explanation":"With distance measured in parsecs and parallax in arcseconds, distance is inversely proportional to parallax. A star with a parallax of 1 arcsecond is 1 parsec away."},{"text":"$$$d = p$$ (where $d$ is in parsecs and $p$ is in arcseconds)","correct":false,"explanation":"Distance is not directly proportional to parallax: more distant stars show smaller parallax angles. The correct inverse relationship is $d = 1/p$ for these units."},{"text":"$$$d = \\frac{1}{p^2}$$ (where $d$ is in parsecs and $p$ is in arcseconds)","correct":false,"explanation":"The inverse-square relationship applies to quantities such as intensity, not stellar parallax. Geometrically, distance is inversely proportional to angle, giving $d = 1/p$."},{"text":"$$$d = p^2$$ (where $d$ is in parsecs and $p$ is in arcseconds)","correct":false,"explanation":"Squaring the parallax incorrectly makes distance increase with the measured angular shift. In parsecs and arcseconds, the correct relationship is the reciprocal, $d = 1/p$."}]},{"id":"964adbe7-4ceb-4ad5-83b6-fe38c4b0810f","cardType":"basic","points":1,"front":"When calculating distance from stellar parallax, what is $p$ relative to the total angular shift?","back":"$$p$ is half the total angular shift.","mcqOptions":[{"text":"$$p$ is half the total angular shift.","correct":true,"explanation":"Observations six months apart show the star displaced to opposite sides of its mean position. The full shift is therefore $2p$, making $p$ half that shift."},{"text":"$$p$ is equal to the total angular shift.","correct":false,"explanation":"The total observed angular shift spans both sides of the star’s mean position and equals $2p$. Therefore, the parallax angle $p$ is half the total shift."},{"text":"$$p$ is twice the total angular shift.","correct":false,"explanation":"Doubling the total shift reverses the required relationship. Because the measured total displacement is $2p$, the parallax angle is half the total angular shift."},{"text":"$$p$ is one-quarter of the total angular shift.","correct":false,"explanation":"Quartering the total shift applies an extra, unjustified factor of two. The two extreme positions are separated by $2p$, so $p$ is half the total shift."}]},{"id":"1a2518b7-c93f-4e7d-b3b9-2fafde5d4c1c","cardType":"cloze","points":null,"front":"The Cosmological principle assumes the Universe is $\\text{[...]}$ (same structure everywhere) and $isotropic$ (looks the same in all directions).","back":"The Cosmological principle assumes the Universe is $\\boxed{homogeneous}$ (same structure everywhere) and $isotropic$ (looks the same in all directions).","mcqOptions":[{"text":"$$homogeneous$","correct":true,"explanation":"Homogeneity means that, on sufficiently large scales, matter has the same overall distribution and the Universe has the same general structure at every location."},{"text":"$$isotropic$","correct":false,"explanation":"Isotropy describes looking the same in every direction, not having the same large-scale structure everywhere. The term required for sameness from place to place is homogeneous."},{"text":"$$heterogeneous$","correct":false,"explanation":"A heterogeneous Universe would have fundamentally different large-scale structures in different places, contradicting the cosmological principle. The required description is homogeneous."},{"text":"$$anisotropic$","correct":false,"explanation":"An anisotropic Universe would look different in different directions and therefore violate the other part of the cosmological principle. Sameness of structure everywhere is described as homogeneous."}]},{"id":"0f8c1f86-6263-4ccd-9b46-fd309e871c04","cardType":"cloze","points":null,"front":"The Cosmological principle assumes the Universe is $homogeneous$ (same structure everywhere) and $\\text{[...]}$ (looks the same in all directions).","back":"The Cosmological principle assumes the Universe is $homogeneous$ (same structure everywhere) and $\\boxed{isotropic}$ (looks the same in all directions).","mcqOptions":[{"text":"$$isotropic$","correct":true,"explanation":"Isotropy means that, on sufficiently large scales, the Universe has the same general appearance in every direction from a given observation point."},{"text":"$$homogeneous$","correct":false,"explanation":"Homogeneity means having the same large-scale structure in different places, rather than looking the same in every direction. The directional property required here is isotropic."},{"text":"$$anisotropic$","correct":false,"explanation":"Anisotropic means looking different in different directions, which is the opposite of the cosmological principle’s directional assumption. The Universe is assumed to be isotropic."},{"text":"$$heterogeneous$","correct":false,"explanation":"Heterogeneous describes variation in large-scale structure from place to place, not sameness in all viewing directions. The required directional property is isotropic."}]},{"id":"255a5975-ab7a-4dd9-ba6d-4dba59a64869","cardType":"basic","points":1,"front":"What does redshift in a galaxy's spectrum indicate about its motion?","back":"The galaxy is moving away from the observer.","mcqOptions":[{"text":"The galaxy is moving away from the observer.","correct":true,"explanation":"Redshift means the observed wavelengths are longer than the emitted wavelengths. This Doppler shift occurs when the galaxy is receding from the observer."},{"text":"The galaxy is moving towards the observer.","correct":false,"explanation":"A galaxy moving towards the observer produces a blueshift, in which its observed spectral wavelengths become shorter. Redshift instead indicates that the galaxy is moving away."},{"text":"The galaxy is moving sideways relative to the observer.","correct":false,"explanation":"Transverse motion alone does not produce the classical wavelength increase described here. Redshift indicates a component of velocity directed away from the observer."},{"text":"The galaxy is stationary relative to the observer.","correct":false,"explanation":"Being stationary would leave the spectral lines at their laboratory wavelengths, apart from non-motion effects. A Doppler redshift indicates that the galaxy is moving away."}]},{"id":"b3986e80-008d-452e-803e-f932f29a1df3","cardType":"basic","points":1,"front":"State the Doppler equation relating wavelength shift and recessional speed ($v \\ll c$).","back":"$$$\\frac{\\Delta \\lambda}{\\lambda} \\approx \\frac{v}{c}$$","mcqOptions":[{"text":"$$$\\frac{\\Delta \\lambda}{\\lambda} \\approx \\frac{v}{c}$$","correct":true,"explanation":"For recessional speeds much smaller than the speed of light, the fractional increase in wavelength is approximately equal to the ratio of recessional speed to light speed."},{"text":"$$$\\frac{\\Delta \\lambda}{\\lambda} \\approx \\frac{c}{v}$$","correct":false,"explanation":"This reverses the speed ratio. The non-relativistic Doppler relation equates the fractional wavelength shift to $v/c$, not $c/v$."},{"text":"$$$\\frac{\\Delta \\lambda}{\\Delta v} \\approx \\frac{v}{c}$$","correct":false,"explanation":"This uses the shifted wavelength in the denominator rather than the original wavelength. The required fractional shift is $\\Delta\\lambda/\\lambda \\approx v/c$."},{"text":"$$$\\frac{\\Delta \\lambda}{\\lambda} \\approx \\frac{v^2}{c^2}$$","correct":false,"explanation":"This incorrectly squares the velocity ratio. At speeds much smaller than $c$, the fractional wavelength shift is proportional directly to $v/c$."}]},{"id":"48e48174-50a3-42ee-94b9-c8a5233e1011","cardType":"basic","points":1,"front":"State Hubble's Law.","back":"The recessional speed $v$ of a galaxy is proportional to its distance $d$:

$$v \\approx H_0 d$$

","mcqOptions":[{"text":"The recessional speed $v$ of a galaxy is proportional to its distance $d$:

$$v \\approx H_0 d$$

","correct":true,"explanation":"Hubble's Law states that more distant galaxies recede faster. The proportionality constant $H_0$ links a galaxy's distance to its recessional speed."},{"text":"The recessional speed $v$ of a galaxy is inversely proportional to its distance $d$:

$$v \\approx \\frac{H_0}{d}$$

","correct":false,"explanation":"This gives an inverse relationship, incorrectly predicting that more distant galaxies recede more slowly. Hubble's Law states $v \\approx H_0d$, so speed is directly proportional to distance."},{"text":"The recessional speed $v$ of a galaxy is proportional to its distance $d$:

$$v \\approx \\frac{d}{H_0}$$

","correct":false,"explanation":"This reverses the roles of distance and the Hubble constant and is dimensionally inconsistent. Hubble's Law is $v \\approx H_0d$."},{"text":"The recessional speed $v$ of a galaxy is proportional to the square of its distance $d$:

$$v \\approx H_0 d^2$$

","correct":false,"explanation":"Hubble's Law is a linear relationship, not a square-law relationship. Recessional speed satisfies $v \\approx H_0d$, making it directly proportional to distance."}]},{"id":"923f2bed-ac2c-46be-aab8-47f6d54636ba","cardType":"basic","points":1,"front":"In a graph of recessional speed $v$ against distance $d$, what represents the Hubble constant?","back":"The gradient of the line of best fit.","mcqOptions":[{"text":"The gradient of the line of best fit.","correct":true,"explanation":"On a graph with $v$ on the vertical axis and $d$ on the horizontal axis, the gradient is $v/d$, which equals $H_0$."},{"text":"The vertical intercept of the line of best fit.","correct":false,"explanation":"The intercept represents the predicted recessional speed at zero distance, not the proportionality constant. The Hubble constant is the gradient of the best-fit line."},{"text":"The area beneath the line of best fit.","correct":false,"explanation":"The area beneath a speed-distance graph has no role in Hubble's Law. Since $v=H_0d$, the Hubble constant is the gradient."},{"text":"The scatter around the line of best fit.","correct":false,"explanation":"Scatter indicates observational uncertainty or peculiar velocities rather than the expansion rate itself. The Hubble constant is represented by the gradient of the best-fit line."}]},{"id":"5c37a09e-7ae2-4c2c-b59c-d825a372f2c7","cardType":"basic","points":1,"front":"What is the SI unit for the Hubble constant?","back":"$$$\\text{s}^{-1}$$","mcqOptions":[{"text":"$$$\\text{s}^{-1}$$","correct":true,"explanation":"From $v=H_0d$, the units of $H_0$ are velocity divided by distance: $(\\text{m s}^{-1})/\\text{m}=\\text{s}^{-1}$."},{"text":"$$$\\text{s}$$","correct":false,"explanation":"Seconds measure time, but the Hubble constant is an inverse timescale. Dividing velocity by distance gives the SI unit $\\text{s}^{-1}$."},{"text":"$$$\\text{m s}^{-1}$$","correct":false,"explanation":"Metres per second are units of velocity, not the Hubble constant. In $H_0=v/d$, the metres cancel, leaving $\\text{s}^{-1}$."},{"text":"$$$\\text{m}^{-1}$$","correct":false,"explanation":"Inverse metres describe spatial frequency rather than expansion rate. Dividing velocity by distance cancels the length dimension and gives $\\text{s}^{-1}$."}]},{"id":"0b410f48-103e-4ad0-8471-e447e91053aa","cardType":"basic","points":1,"front":"How is the age of the Universe estimated using the Hubble constant ($H_0$)?","back":"$$$t \\approx \\frac{1}{H_0}$$","mcqOptions":[{"text":"$$$t \\approx \\frac{1}{H_0}$$","correct":true,"explanation":"The Hubble constant has dimensions of inverse time, so its reciprocal provides a characteristic expansion time and hence an approximate age of the Universe."},{"text":"$$$t \\approx H_0$$","correct":false,"explanation":"Using $H_0$ directly confuses an inverse timescale with a time. The approximate age is obtained by taking its reciprocal: $t\\approx1/H_0$."},{"text":"$$$t \\approx H_0^2$$","correct":false,"explanation":"Squaring the Hubble constant produces dimensions of inverse time squared, so this cannot represent an age. The required estimate is $t\\approx1/H_0$."},{"text":"$$$t \\approx \\frac{1}{H_0^2}$$","correct":false,"explanation":"This gives a squared timescale and therefore has the wrong dimensions for age. The Hubble time is the simple reciprocal, $t\\approx1/H_0$."}]},{"id":"f9044067-45a9-48a8-b4cf-aafb760c5d6f","cardType":"basic","points":1,"front":"According to the Big Bang theory, what was the initial state of the Universe?","back":"Extremely hot and dense.","mcqOptions":[{"text":"Extremely hot and dense.","correct":true,"explanation":"The Big Bang model describes the early Universe as having an extremely high temperature and density, followed by expansion and cooling over cosmic time."},{"text":"Extremely cold and dense.","correct":false,"explanation":"The early Universe was hot rather than cold because matter and radiation had enormous energy density. It was also extremely dense before expansion."},{"text":"Extremely hot and diffuse.","correct":false,"explanation":"The early Universe was dense rather than diffuse, with matter and energy concentrated into a much smaller volume. It was also extremely hot."},{"text":"Extremely cold and diffuse.","correct":false,"explanation":"Cold and diffuse describe the later Universe more closely, after extensive expansion and cooling. The initial Universe was extremely hot and dense."}]},{"id":"108c3630-9c74-49d7-8e11-1d6b5994422d","cardType":"cloze","points":null,"front":"The cosmic microwave background radiation (CMB) corresponds to a temperature of approximately $\\text{[...]}$.","back":"The cosmic microwave background radiation (CMB) corresponds to a temperature of approximately $\\boxed{2.7\\ \\text{K}}$.","mcqOptions":[{"text":"$$2.7\\ \\text{K}$","correct":true,"explanation":"The CMB has a near-perfect black-body spectrum corresponding to about $2.7\\ \\text{K}$, showing that radiation from the early Universe has cooled through cosmic expansion."},{"text":"$$27\\ \\text{K}$","correct":false,"explanation":"This factor-of-ten overestimate confuses the CMB with a much warmer black body. Its measured spectrum corresponds to approximately $2.7\\ \\text{K}$."},{"text":"$$270\\ \\text{K}$","correct":false,"explanation":"This factor-of-100 overestimate is near room-temperature scales, not the microwave background. The CMB's black-body temperature is approximately $2.7\\ \\text{K}$."},{"text":"$$0.27\\ \\text{K}$","correct":false,"explanation":"This factor-of-ten underestimate would place the radiation even closer to absolute zero than observations show. The measured CMB temperature is approximately $2.7\\ \\text{K}$."}]},{"id":"e9d89c65-ca24-46b2-afe3-ff724a1ffd2b","cardType":"basic","points":2,"front":"Why is the CMB radiation evidence for the Big Bang?","back":"It is leftover radiation from the early hot Universe, stretched to microwave wavelengths as space expanded.","mcqOptions":[{"text":"It is leftover radiation from the early hot Universe, stretched to microwave wavelengths as space expanded.","correct":true,"explanation":"The early Universe was hot and filled with thermal radiation. Expansion stretched this radiation to longer wavelengths, producing the nearly uniform microwave background observed throughout space today."},{"text":"It is radiation emitted by the first stars, scattered to microwave wavelengths by intergalactic dust.","correct":false,"explanation":"Starlight contributes to other background radiation but did not produce the CMB. The correct explanation is that the CMB is early-Universe radiation stretched to microwave wavelengths by cosmic expansion."},{"text":"It is radiation produced by dark matter, converted to microwave wavelengths as galaxies formed.","correct":false,"explanation":"The CMB is not generated continuously by dark matter, which does not emit electromagnetic radiation. It is remnant thermal radiation from the hot early Universe, redshifted as space expanded."},{"text":"It is leftover radiation from the early hot Universe, shortened to gamma-ray wavelengths as space expanded.","correct":false,"explanation":"Expansion increases electromagnetic wavelengths rather than shortening them. Radiation from the hot early Universe was stretched into the microwave region, which is why it is observed as the CMB."}]},{"id":"85b532fc-eb64-4481-a1f0-ddc1f6c34da9","cardType":"basic","points":2,"front":"Why does galactic redshift support the Big Bang model?","back":"It shows the Universe is expanding, implying it was smaller and denser in the past.","mcqOptions":[{"text":"It shows the Universe is expanding, implying it was smaller and denser in the past.","correct":true,"explanation":"Light from most distant galaxies is shifted towards longer wavelengths, showing that they are receding. Reversing this expansion implies that the Universe was once smaller, hotter and denser."},{"text":"It shows the Universe is contracting, implying it was larger and less dense in the past.","correct":false,"explanation":"Redshift indicates that distant galaxies are generally receding, not approaching one another. The resulting expansion implies that the Universe was smaller and denser at earlier times."},{"text":"It shows the galaxies orbit a centre, implying the Universe rotates as a single system.","correct":false,"explanation":"Galactic redshift follows a large-scale pattern of recession rather than merely showing orbital motion around a central point. This pattern demonstrates cosmic expansion from an earlier, denser state."},{"text":"It shows the galaxies move randomly, implying there was no denser state in the past.","correct":false,"explanation":"Redshifts increase systematically with galactic distance, so they do not represent purely random motion. This relationship shows that space is expanding and points to a smaller, denser past."}]},{"id":"f5d205e9-2074-426a-8e60-6abaaf04ca39","cardType":"basic","points":1,"front":"What is the defining characteristic of dark matter?","back":"It has gravitational effects but does not emit or absorb electromagnetic radiation.","mcqOptions":[{"text":"It has gravitational effects but does not emit or absorb electromagnetic radiation.","correct":true,"explanation":"Dark matter is inferred from gravitational phenomena such as galaxy rotation and gravitational lensing. It is called dark because it neither emits nor absorbs detectable electromagnetic radiation."},{"text":"It has gravitational effects and emits large amounts of visible electromagnetic radiation.","correct":false,"explanation":"Emitting visible light would make matter electromagnetically detectable and therefore not dark. Dark matter is instead identified through its gravitational effects despite not emitting or absorbing electromagnetic radiation."},{"text":"It has electromagnetic effects but does not exert gravitational forces on ordinary matter.","correct":false,"explanation":"Dark matter is not defined by electromagnetic interactions, which would make it directly detectable through radiation. Its defining evidence comes from gravity, while it does not emit or absorb electromagnetic radiation."},{"text":"It has light-absorbing effects but does not contribute to the gravitational fields of galaxies.","correct":false,"explanation":"Absorbing light would create observable electromagnetic signatures, while an absence of gravity would not explain galaxy rotation or lensing. Dark matter has gravitational effects but does not absorb or emit radiation."}]},{"id":"84edc1d4-5140-4f10-9818-3025702657a9","cardType":"basic","points":1,"front":"What is the role of dark energy in the Universe?","back":"It is responsible for the accelerated expansion of the Universe.","mcqOptions":[{"text":"It is responsible for the accelerated expansion of the Universe.","correct":true,"explanation":"Observations of distant Type Ia supernovae indicate that cosmic expansion is speeding up. Dark energy is the name given to the component responsible for this accelerated expansion."},{"text":"It is responsible for the decelerated expansion of the Universe.","correct":false,"explanation":"Gravity from matter tends to slow cosmic expansion rather than explaining its observed acceleration. Dark energy is introduced specifically to account for the accelerating expansion of the Universe."},{"text":"It is responsible for the rapid rotation of galaxies.","correct":false,"explanation":"Unseen mass within and around galaxies explains unexpectedly fast galactic rotation, but that is attributed to dark matter. Dark energy instead accounts for accelerated cosmic expansion."},{"text":"It is responsible for the formation of light elements in the Universe.","correct":false,"explanation":"Nuclear reactions during Big Bang nucleosynthesis produced the early light elements; dark energy did not. Its cosmological role is to drive the Universe’s accelerated expansion."}]},{"id":"ad3e3b45-8f11-4725-9a19-aa960759c52f","cardType":"cloze","points":null,"front":"The approximate composition of the Universe is 5% ordinary matter, $\\text{[...]}$ dark matter, and $70\\%$ dark energy.","back":"The approximate composition of the Universe is 5% ordinary matter, $\\boxed{25\\%}$ dark matter, and $70\\%$ dark energy.","mcqOptions":[{"text":"$$25\\%$","correct":true,"explanation":"Current cosmological measurements indicate that dark matter contributes approximately 25% of the Universe’s total mass-energy content, alongside about 5% ordinary matter and 70% dark energy."},{"text":"$$5\\%$","correct":false,"explanation":"This confuses dark matter with ordinary baryonic matter, which contributes only about 5%. Dark matter accounts for approximately $25\\%$, allowing the three listed components to total 100%."},{"text":"$$70\\%$","correct":false,"explanation":"This swaps the approximate proportions of dark matter and dark energy. Dark energy contributes about 70%, whereas dark matter contributes approximately $25\\%$ of the Universe’s content."},{"text":"$$30\\%$","correct":false,"explanation":"This likely subtracts only the 70% dark-energy share and overlooks the 5% ordinary-matter share. The remaining dark-matter proportion is approximately $25\\%$, not 30%."}]},{"id":"2437d0b2-2401-4fb6-ac1a-364646cb6241","cardType":"cloze","points":null,"front":"The approximate composition of the Universe is 5% ordinary matter, $25\\%$ dark matter, and $\\text{[...]}$ dark energy.","back":"The approximate composition of the Universe is 5% ordinary matter, $25\\%$ dark matter, and $\\boxed{70\\%}$ dark energy.","mcqOptions":[{"text":"$$70\\%$","correct":true,"explanation":"Dark energy makes up approximately 70% of the Universe’s total mass-energy content. Together with about 25% dark matter and 5% ordinary matter, this totals 100%."},{"text":"$$25\\%$","correct":false,"explanation":"This swaps the proportions assigned to dark energy and dark matter. Dark matter accounts for about 25%, while dark energy is the dominant component at approximately $70\\%$."},{"text":"$$5\\%$","correct":false,"explanation":"This confuses dark energy with ordinary matter, which contributes about 5% of the total. Observational evidence indicates that dark energy contributes approximately $70\\%$."},{"text":"$$75\\%$","correct":false,"explanation":"This subtracts the 25% dark-matter share from 100% but overlooks the additional 5% of ordinary matter. Accounting for both leaves approximately $70\\%$ dark energy."}]}]}],"examCountdown":{"examDate":"2027-05-21","paperLabel":"Paper 1"},"heading":"Cosmology","title":"Cosmology Flashcards","topbar":{"backHref":"/a-level/physics/ocr/a/flashcards"},"topicSidebar":"$L38"}]}],"topicId":"d1cad92d-e182-5433-836c-69872a50500d","walled":"$L39"}],"$L3a","$L3b"]