dkoterwa/mlqa_filtered huggingface dataset:
Humans play a key role in the biosphere, with the large human population dominating many of Earth's ecosystems. This has resulted in a widespread, ongoing mass extinction of other species during the present geological epoch, now known as the Holocene extinction. The large-scale loss of species caused by human influence since the 1950s has been called a biotic crisis, with an estimated 10% of the total species lost as of 2007. At current rates, about 30% of species are at risk of extinction in the next hundred years. The Holocene extinction event is the result of habitat destruction, the widespread distribution of invasive species, hunting, and climate change. In the present day, human activity has had a significant impact on the surface of the planet. More than a third of the land surface has been modified by human actions, and humans use about 20% of global primary production. The concentration of carbon dioxide in the atmosphere has increased by close to 30% since the start of the Industrial Revolution.The consequences of a persistent biotic crisis have been predicted to last for at least five million years. It could result in a decline in biodiversity and homogenization of biotas, accompanied by a proliferation of species that are opportunistic, such as pests and weeds. Novel species may also emerge; in particular taxa that prosper in human-dominated ecosystems may rapidly diversify into many new species. Microbes are likely to benefit from the increase in nutrient-enriched environmental niches. No new species of existing large vertebrates are likely to arise and food chains will probably be shortened.There are multiple scenarios for known risks that can have a global impact on the planet. From the perspective of humanity, these can be subdivided into survivable risks and terminal risks. Risks that humanity pose to itself include climate change, the misuse of nanotechnology, a nuclear holocaust, warfare with a programmed superintelligence, a genetically engineered disease, or a disaster caused by a physics experiment. Similarly, several natural events may pose a doomsday threat, including a highly virulent disease, the impact of an asteroid or comet, runaway greenhouse effect, and resource depletion. There may also be the possibility of an infestation by an extraterrestrial lifeform. The actual odds of these scenarios occurring are difficult if not impossible to deduce.Should the human race become extinct, then the various features assembled by humanity will begin to decay. The largest structures have an estimated decay half-life of about 1,000 years. The last surviving structures would most likely be open pit mines, large landfills, major highways, wide canal cuts, and earth-fill flank dams. A few massive stone monuments like the pyramids at the Giza Necropolis or the sculptures at Mount Rushmore may still survive in some form after a million years.

Question: If  there were no more humans on earth, what would be left to drive on?
Answer: major highways
Once the Sun changes from burning hydrogen at its core to burning hydrogen around its shell, the core will start to contract and the outer envelope will expand. The total luminosity will steadily increase over the following billion years until it reaches 2,730 times the Sun's current luminosity at the age of 12.167 billion years. Most of Earth's atmosphere will be lost to space and its surface will consist of a lava ocean with floating continents of metals and metal oxides as well as icebergs of refractory materials, with its surface temperature reaching more than 2,400 K (2,130 °C; 3,860 °F). The Sun will experience more rapid mass loss, with about 33% of its total mass shed with the solar wind. The loss of mass will mean that the orbits of the planets will expand. The orbital distance of the Earth will increase to at most 150% of its current value.The most rapid part of the Sun's expansion into a red giant will occur during the final stages, when the Sun will be about 12 billion years old. It is likely to expand to swallow both Mercury and Venus, reaching a maximum radius of 1.2 AU (180,000,000 km). The Earth will interact tidally with the Sun's outer atmosphere, which would serve to decrease Earth's orbital radius. Drag from the chromosphere of the Sun would also reduce the Earth's orbit. These effects will act to counterbalance the effect of mass loss by the Sun, and the Earth will probably be engulfed by the Sun.The drag from the solar atmosphere may cause the orbit of the Moon to decay. Once the orbit of the Moon closes to a distance of 18,470 km (11,480 mi), it will cross the Earth's Roche limit. This means that tidal interaction with the Earth would break apart the Moon, turning it into a ring system. Most of the orbiting ring will then begin to decay, and the debris will impact the Earth. Hence, even if the Earth is not swallowed up by the Sun, the planet may be left moonless. The ablation and vaporization caused by its fall on a decaying trajectory towards the Sun may remove Earth's mantle, leaving just its core, which will finally be destroyed after at most 200 years. Following this event, Earth's sole legacy will be a very slight increase (0.01%) of the solar metallicity.§IIC

Question: What burns hydrogen and has a shell and a core?
Answer: Sun

Question: What two bodies will be swallowed?
Answer: Mercury and Venus
34He → 12C + γ + 7.2 MeVIn massive stars, heavier elements can also be burned in a contracting core through the neon-burning process and oxygen-burning process. The final stage in the stellar nucleosynthesis process is the silicon-burning process that results in the production of the stable isotope iron-56, an endothermic process that consumes energy, and so further energy can only be produced through gravitational collapse.The example below shows the amount of time required for a star of 20 M☉ to consume all of its nuclear fuel. As an O-class main sequence star, it would be 8 times the solar radius and 62,000 times the Sun's luminosity.

Question: What processes can be used to burn heavier elements in a contracting core?
Answer: neon-burning process and oxygen-burning process
A variety of nuclear fusion reactions take place in the cores of stars, that depend upon their mass and composition. When nuclei fuse, the mass of the fused product is less than the mass of the original parts. This lost mass is converted to electromagnetic energy, according to the mass–energy equivalence relationship E = mc2.The hydrogen fusion process is temperature-sensitive, so a moderate increase in the core temperature will result in a significant increase in the fusion rate. As a result, the core temperature of main sequence stars only varies from 4 million kelvin for a small M-class star to 40 million kelvin for a massive O-class star.In the Sun, with a 10-million-kelvin core, hydrogen fuses to form helium in the proton–proton chain reaction:

Question: What element combines to make helium in the process?
Answer: hydrogen
Besides mass, the elements heavier than helium can play a significant role in the evolution of stars. Astronomers label all elements heavier than helium "metals", and call the chemical concentration of these elements in a star, its metallicity. A star's metallicity can influence the time the star takes to burn its fuel, and controls the formation of its magnetic fields, which affects the strength of its stellar wind. Older, population II stars have substantially less metallicity than the younger, population I stars due to the composition of the molecular clouds from which they formed. Over time, such clouds become increasingly enriched in heavier elements as older stars die and shed portions of their atmospheres.

Question: What happens to the clouds of younger population I stars over time?
Answer: become increasingly enriched in heavier elements
Circa 1600, the names of the constellations were used to name the stars in the corresponding regions of the sky. The German astronomer Johann Bayer created a series of star maps and applied Greek letters as designations to the stars in each constellation. Later a numbering system based on the star's right ascension was invented and added to John Flamsteed's star catalogue in his book "Historia coelestis Britannica" (the 1712 edition), whereby this numbering system came to be called Flamsteed designation or Flamsteed numbering.The only internationally recognized authority for naming celestial bodies is the International Astronomical Union (IAU). The International Astronomical Union maintains the Working Group on Star Names (WGSN) which catalogs and standardizes proper names for stars. A number of private companies sell names of stars, which the British Library calls an unregulated commercial enterprise. The IAU has disassociated itself from this commercial practice, and these names are neither recognized by the IAU, professional astronomers, nor the amateur astronomy community. One such star-naming company is the International Star Registry, which, during the 1980s, was accused of deceptive practice for making it appear that the assigned name was official. This now-discontinued ISR practice was informally labeled a scam and a fraud, and the New York City Department of Consumer Affairs issued a violation against ISR for engaging in a deceptive trade practice.

Question: The International Star Registry is now labeled as what?
Answer: scam and a fraud
For at least a portion of its life, a star shines due to thermonuclear fusion of hydrogen into helium in its core, releasing energy that traverses the star's interior and then radiates into outer space. Almost all naturally occurring elements heavier than helium are created by stellar nucleosynthesis during the star's lifetime, and for some stars by supernova nucleosynthesis when it explodes. Near the end of its life, a star can also contain degenerate matter. Astronomers can determine the mass, age, metallicity (chemical composition), and many other properties of a star by observing its motion through space, its luminosity, and spectrum respectively. The total mass of a star is the main factor that determines its evolution and eventual fate. Other characteristics of a star, including diameter and temperature, change over its life, while the star's environment affects its rotation and movement. A plot of the temperature of many stars against their luminosities produces a plot known as a Hertzsprung–Russell diagram (H–R diagram). Plotting a particular star on that diagram allows the age and evolutionary state of that star to be determined.

Question: What primary piece of information determines the evolution and fate of a star?
Answer: total mass
Radial velocity is measured by the doppler shift of the star's spectral lines, and is given in units of km/s. The proper motion of a star, its parallax, is determined by precise astrometric measurements in units of milli-arc seconds (mas) per year. With knowledge of the star's parallax and its distance, the proper motion velocity can be calculated. Together with the radial velocity, the total velocity can be calculated. Stars with high rates of proper motion are likely to be relatively close to the Sun, making them good candidates for parallax measurements.When both rates of movement are known, the space velocity of the star relative to the Sun or the galaxy can be computed. Among nearby stars, it has been found that younger population I stars have generally lower velocities than older, population II stars. The latter have elliptical orbits that are inclined to the plane of the galaxy. A comparison of the kinematics of nearby stars has allowed astronomers to trace their origin to common points in giant molecular clouds, and are referred to as stellar associations.

Question: How can you determine how close a star is to the Sun?
Answer: rates of proper motion
The first direct measurement of the distance to a star (61 Cygni at 11.4 light-years) was made in 1838 by Friedrich Bessel using the parallax technique. Parallax measurements demonstrated the vast separation of the stars in the heavens. Observation of double stars gained increasing importance during the 19th century. In 1834, Friedrich Bessel observed changes in the proper motion of the star Sirius and inferred a hidden companion. Edward Pickering discovered the first spectroscopic binary in 1899 when he observed the periodic splitting of the spectral lines of the star Mizar in a 104-day period. Detailed observations of many binary star systems were collected by astronomers such as Friedrich Georg Wilhelm von Struve and S. W. Burnham, allowing the masses of stars to be determined from computation of orbital elements. The first solution to the problem of deriving an orbit of binary stars from telescope observations was made by Felix Savary in 1827.

Question: When did Bessl found hidden companion of Sirius star?
Answer: 1834
The luminosity of a star is the amount of light and other forms of radiant energy it radiates per unit of time. It has units of power. The luminosity of a star is determined by its radius and surface temperature. Many stars do not radiate uniformly across their entire surface. The rapidly rotating star Vega, for example, has a higher energy flux (power per unit area) at its poles than along its equator.Patches of the star's surface with a lower temperature and luminosity than average are known as starspots. Small, dwarf stars such as our Sun generally have essentially featureless disks with only small starspots.  Giant stars have much larger, more obvious starspots, and

Question: Which measurements are used to calculate the luminosity?
Answer: radius and surface temperature
The magnetic field of a star is generated within regions of the interior where convective circulation occurs. This movement of conductive plasma functions like a dynamo, wherein the movement of electrical charges induce magnetic fields, as does a mechanical dynamo. Those magnetic fields have a great range that extend throughout and beyond the star. The strength of the magnetic field varies with the mass and composition of the star, and the amount of magnetic surface activity depends upon the star's rate of rotation. This surface activity produces starspots, which are regions of strong magnetic fields and lower than normal surface temperatures. Coronal loops are arching magnetic field flux lines that rise from a star's surface into the star's outer atmosphere, its corona. The coronal loops can be seen due to the plasma they conduct along their length. Stellar flares are bursts of high-energy particles that are emitted due to the same magnetic activity.Young, rapidly rotating stars tend to have high levels of surface activity because of their magnetic field. The magnetic field can act upon a star's stellar wind, functioning as a brake to gradually slow the rate of rotation with time. Thus, older stars such as the Sun have a much slower rate of rotation and a lower level of surface activity. The activity levels of slowly rotating stars tend to vary in a cyclical manner and can shut down altogether for periods of time. During

Question: how does the brake function?
Answer: gradually slow the rate of rotation with time
The rotation rate of stars can be determined through spectroscopic measurement, or more exactly determined by tracking their starspots. Young stars can have a rotation greater than 100 km/s at the equator. The B-class star Achernar, for example, has an equatorial velocity of about 225 km/s or greater, causing its equator to bulge outward and giving it an equatorial diameter that is more than 50% greater than between the poles. This rate of rotation is just below the critical velocity of 300 km/s at which speed the star would break apart. By contrast, the Sun rotates once every 25–35 days depending on latitude, with an equatorial velocity of 1.93 km/s. A main sequence star's magnetic field and the stellar wind serve to slow its rotation by a significant amount as it evolves on the main sequence.Degenerate stars have contracted into a compact mass, resulting in a rapid rate of rotation. However they have relatively low rates of rotation compared to what would be expected by conservation of angular momentum—the tendency of a rotating body to compensate for a contraction in size by increasing its rate of spin. A large portion of the star's angular momentum is dissipated as a result of mass loss through the stellar wind. In spite of this, the rate of rotation for a pulsar can be very rapid. The pulsar at the heart of the Crab nebula, for example, rotates 30 times per second. The rotation rate of the pulsar will gradually slow due to the emission of radiation.

Question: When a large body is in rotation, how does it deal with the contraction in its size?
Answer: increasing its rate of spin

Question: What results in the rapid rotation rate of degenerate stars?
Answer: Degenerate stars
galaxy). But some stars have been observed in the M100 galaxy of the Virgo Cluster, about 100 million light years from the Earth.

Question: how many light years can you observe some stars from earth?
Answer: 100 million
King Pōmare II of Tahiti was forced to flee to Mo'orea in 1803; he and his subjects were converted to Protestantism in 1812. French Catholic missionaries arrived on Tahiti in 1834; their expulsion in 1836 caused France to send a gunboat in 1838. In 1842, Tahiti and Tahuata were declared a French protectorate, to allow Catholic missionaries to work undisturbed. The capital of Papeetē was founded in 1843. In 1880, France annexed Tahiti, changing the status from that of a protectorate to that of a colony. The island groups were not officially united until the establishment of the French protectorate in 1889.After France declared a protectorate over Tahiti in 1840, the British and French signed the Jarnac Convention in 1847, declaring that the kingdoms of Raiatea, Huahine and Bora Bora were to remain independent from either powers and that no single chief was to be allowed to reign over the entire archipelago. France eventually broke the agreement, and the islands were annexed and became a colony in 1888 (eight years after the Windward Islands) after many native resistances and conflicts called the Leewards War, lasting until 1897.In the 1880s, France claimed the Tuamotu Archipelago, which formerly belonged to the Pōmare Dynasty, without formally annexing it. Having declared a protectorate over Tahuata in 1842, the French regarded the entire Marquesas Islands as French. In 1885, France appointed a governor and established a general council, thus giving it the proper administration for a colony. The islands of Rimatara and Rūrutu unsuccessfully lobbied for British protection in 1888, so in 1889 they were annexed by France. Postage stamps were first issued in the colony in 1892. The first official name for the colony was Établissements de l'Océanie (Establishments in Oceania); in 1903 the general council was changed to an advisory council and the colony's name was changed to Établissements Français de l'Océanie (French Establishments in Oceania).In 1940, the administration of French Polynesia recognised the Free French Forces and many Polynesians served in World War II. Unknown at the time to the French and Polynesians, the Konoe Cabinet in Imperial Japan on 16 September 1940 included French Polynesia among the many territories which were to become Japanese possessions, as part of the "Eastern Pacific Government-General" in the post-war world. However, in the course of the war in the Pacific the Japanese were not able to launch an actual invasion of the French islands.

Question: What happened as a result of King Pomare II and his followers when they escaped to Mo'orea?
Answer: converted to Protestantism
Scientists believe the Great Polynesian Migration happened around 1500 BC as Austronesian people went on a journey using celestial navigation to find islands in the South Pacific Ocean. The first islands of French Polynesia to be settled were the Marquesas Islands in about 200 BC. The Polynesians later ventured southwest and discovered the Society Islands around AD 300.European encounters began in 1521 when Portuguese explorer Ferdinand Magellan, sailing at the service of the Spanish Crown, sighted Puka-Puka in the Tuāmotu-Gambier Archipelago. In 1606 another Spanish expedition under Pedro Fernandes de Queirós sailed through Polynesia sighting an inhabited island on 10 February which they called Sagitaria (or Sagittaria), probably the island of Rekareka to the southeast of Tahiti.Over a century later, British explorer Samuel Wallis visited Tahiti in 1767. French explorer Louis Antoine de Bougainville also visited Tahiti in 1768, while British explorer James Cook arrived in 1769.  In 1772, the Spanish Viceroy of Peru Don Manuel de Amat ordered a number of expeditions to Tahiti under the command of Domingo de Bonechea who was the first European to explore all of the main islands beyond Tahiti. A short-lived Spanish settlement was created in 1774, and for a time some maps bore the name Isla de Amat after Viceroy Amat. In 1772, Dutchman Jakob Roggeveen came across Bora Bora in the Society Islands. Christian missions began with Spanish priests who stayed in Tahiti for a year. Protestants from the London Missionary Society settled permanently in Polynesia in 1797.

Question: When did Bougainville visit Tahiti?
Answer: 1768
The legal tender of French Polynesia is the CFP Franc which has a fixed exchange rate with the Euro. The nominal gross domestic product (or GDP) of French Polynesia in 2014 was 5.623 billion U.S. dollars at market local prices, the sixth-largest economy in Oceania after Australia, New Zealand, Hawaii, New Caledonia, and Papua New Guinea. The GDP per capita was $20,098 in 2014 (at market exchange rates, not at PPP), lower than in Hawaii, Australia, New Zealand, and New Caledonia, but higher than all the independent insular states of Oceania. Both per capita and total figures were significantly lower than those recorded before the financial crisis of 2007–08.French Polynesia has a moderately developed economy, which is dependent on imported goods, tourism, and the financial assistance of mainland France. Tourist facilities are well developed and are available on the major islands. Main agricultural productions are coconuts (copra), vegetables and fruits. French Polynesia exports noni juice, a high quality vanilla, and the famous black Tahitian pearls which accounted for 55% of exports (in value) in 2008.French Polynesia's seafloor contains rich deposits of nickel, cobalt, manganese, and copper that are not exploited.In 2008, French Polynesia's imports amounted to 2.2 billion U.S. dollars and exports amounted to 0.2 billion U.S. dollars.

Question: What is also available on major islands and are well developed?
Answer: Tourist facilities
Total population at the August 2017 census was 275,918 inhabitants. At the 2017 census, 68.7% of the population of French Polynesia lived on the island of Tahiti alone. The urban area of Papeete, the capital city, has 136,771 inhabitants (2017 census).

Question: In what year did Papeete have 136,771 people?
Answer: 2017
Despite the great quantity and excellent quality of the fossil material, Plateosaurus was for a long time one of the most misunderstood dinosaurs. Some researchers proposed theories that were later shown to conflict with geological and palaeontological evidence, but have become the paradigm of public opinion. Since 1980 the taxonomy (relationships), taphonomy (how the animals became embedded and fossilised), biomechanics (how their skeletons worked), and palaeobiology (life circumstances) of Plateosaurus have been re-studied in detail, altering the interpretation of the animal's biology, posture and behaviour.

Question: What did researchers propose that was later conflicted with evidence?
Answer: theories