Siam0703/SQuAD-EN-Passage-to-Question huggingface dataset:
Neptune's mass of 1.0243×1026 kg, is intermediate between Earth and the larger gas giants: it is 17 times that of Earth but just 1/19th that of Jupiter.[d] Its gravity at 1 bar is 11.15 m/s2, 1.14 times the surface gravity of Earth, and surpassed only by Jupiter. Neptune's equatorial radius of 24,764 km is nearly four times that of Earth. Neptune, like Uranus, is an ice giant, a subclass of giant planet, due to their smaller size and higher concentrations of volatiles relative to Jupiter and Saturn. In the search for extrasolar planets, Neptune has been used as a metonym: discovered bodies of similar mass are often referred to as "Neptunes", just as scientists refer to various extrasolar bodies as "Jupiters".

Questions:
What is Neptune's mass?
How much more mass does Neptune have compared to Earth?
What is Neptune's gravity at 1 bar?
What is Neptune's equatorial radius?
What is Neptune referred to due to it's size and concentration of volatiles?
The mantle is equivalent to 10 to 15 Earth masses and is rich in water, ammonia and methane. As is customary in planetary science, this mixture is referred to as icy even though it is a hot, dense fluid. This fluid, which has a high electrical conductivity, is sometimes called a water–ammonia ocean. The mantle may consist of a layer of ionic water in which the water molecules break down into a soup of hydrogen and oxygen ions, and deeper down superionic water in which the oxygen crystallises but the hydrogen ions float around freely within the oxygen lattice. At a depth of 7000 km, the conditions may be such that methane decomposes into diamond crystals that rain downwards like hailstones. Very-high-pressure experiments at the Lawrence Livermore National Laboratory suggest that the base of the mantle may comprise an ocean of liquid carbon with floating solid 'diamonds'.

Questions:
What is Neptune's mantle rich in?
What is the hot, dense fluid in Neptune referred to as?
What does the fluid in Neptune have a high conductivity of?
How deep does Neptune's water-ammonia ocean go?
What rains on Neptune?
At high altitudes, Neptune's atmosphere is 80% hydrogen and 19% helium. A trace amount of methane is also present. Prominent absorption bands of methane exist at wavelengths above 600 nm, in the red and infrared portion of the spectrum. As with Uranus, this absorption of red light by the atmospheric methane is part of what gives Neptune its blue hue, although Neptune's vivid azure differs from Uranus's milder cyan. Because Neptune's atmospheric methane content is similar to that of Uranus, some unknown atmospheric constituent is thought to contribute to Neptune's colour.

Questions:
What is Neptune's atmosphere made of?
Where are absorption bands of methane on Neptune?
What gives Neptune it's blue hue?
What planet also gets it's color from atmospheric constituent?
What color is Uranus, compared to Neptune?
Models suggest that Neptune's troposphere is banded by clouds of varying compositions depending on altitude. The upper-level clouds lie at pressures below one bar, where the temperature is suitable for methane to condense. For pressures between one and five bars (100 and 500 kPa), clouds of ammonia and hydrogen sulfide are thought to form. Above a pressure of five bars, the clouds may consist of ammonia, ammonium sulfide, hydrogen sulfide and water. Deeper clouds of water ice should be found at pressures of about 50 bars (5.0 MPa), where the temperature reaches 273 K (0 °C). Underneath, clouds of ammonia and hydrogen sulfide may be found.

Questions:
What is Neptune's clouds competition variants dependent on?
Which clouds on Neptune are suitable for methane to condense?
What clouds form between one and five bars on Neptune?
On Neptune, what do clouds above five bars consist of?
What is the temperature on Neptune's clouds that are at 50 bars?
High-altitude clouds on Neptune have been observed casting shadows on the opaque cloud deck below. There are also high-altitude cloud bands that wrap around the planet at constant latitude. These circumferential bands have widths of 50–150 km and lie about 50–110 km above the cloud deck. These altitudes are in the layer where weather occurs, the troposphere. Weather does not occur in the higher stratosphere or thermosphere. Unlike Uranus, Neptune's composition has a higher volume of ocean, whereas Uranus has a smaller mantle.

Questions:
On Neptune, which clouds cast shadows on the cloud deck below it?
What are the widths of the cloud bands on Neptune?
Where are the high altitude bands of clouds on Neptune?
What does Neptune have more of compared to Uranus?
Where on Neptune does weather not occur?
For reasons that remain obscure, the planet's thermosphere is at an anomalously high temperature of about 750 K. The planet is too far from the Sun for this heat to be generated by ultraviolet radiation. One candidate for a heating mechanism is atmospheric interaction with ions in the planet's magnetic field. Other candidates are gravity waves from the interior that dissipate in the atmosphere. The thermosphere contains traces of carbon dioxide and water, which may have been deposited from external sources such as meteorites and dust.

Questions:
What is Neptune's temperature in the thermosphere?
What would interact with Neptune's magnetic field to make it warm?
Where would gravity waves in Neptune's interior dissipate?
What does Neptune's thermosphere containers traces of?
Neptune also resembles Uranus in its magnetosphere, with a magnetic field strongly tilted relative to its rotational axis at 47° and offset at least 0.55 radii, or about 13500 km from the planet's physical centre. Before Voyager 2's arrival at Neptune, it was hypothesised that Uranus's tilted magnetosphere was the result of its sideways rotation. In comparing the magnetic fields of the two planets, scientists now think the extreme orientation may be characteristic of flows in the planets' interiors. This field may be generated by convective fluid motions in a thin spherical shell of electrically conducting liquids (probably a combination of ammonia, methane and water) resulting in a dynamo action.

Questions:
What is the rotational axis of Neptune's magnetic field?
Where is Neptune's magnetic field offset from the physical centre?
What planet besides Neptune has a sideways rotation?
What might cause Neptune's extreme orientation?
What fluids are in Neptune's interior?
The dipole component of the magnetic field at the magnetic equator of Neptune is about 14 microteslas (0.14 G). The dipole magnetic moment of Neptune is about 2.2 × 1017 T·m3 (14 μT·RN3, where RN is the radius of Neptune). Neptune's magnetic field has a complex geometry that includes relatively large contributions from non-dipolar components, including a strong quadrupole moment that may exceed the dipole moment in strength. By contrast, Earth, Jupiter and Saturn have only relatively small quadrupole moments, and their fields are less tilted from the polar axis. The large quadrupole moment of Neptune may be the result of offset from the planet's centre and geometrical constraints of the field's dynamo generator.

Questions:
What is Neptune's dipole magnetic moment?
What is one of Neptune's non-dipolar component what may exceed the dipole moment in strength?
Which three planets have small quadrupole moments compared to Neptune?
Besides the geometrical constraints of Neptune's dynamo generator, what is another result of the quadrupole moment?
What is the dipole component of the magnetic field at the magnetic equator of neptune?
Neptune has a planetary ring system, though one much less substantial than that of Saturn. The rings may consist of ice particles coated with silicates or carbon-based material, which most likely gives them a reddish hue. The three main rings are the narrow Adams Ring, 63,000 km from the centre of Neptune, the Le Verrier Ring, at 53,000 km, and the broader, fainter Galle Ring, at 42,000 km. A faint outward extension to the Le Verrier Ring has been named Lassell; it is bounded at its outer edge by the Arago Ring at 57,000 km.

Questions:
What system, like Saturn, does Neptune have?
What might Neptune's rings consist of?
What might the ice particles of Neptune's rings be coated with?
Where is Adams ring from the center of Neptune?
Where is the La Verrier ring from the center of Neptune?
Neptune's weather is characterised by extremely dynamic storm systems, with winds reaching speeds of almost 600 m/s (2,200 km/h; 1,300 mph)—nearly reaching supersonic flow. More typically, by tracking the motion of persistent clouds, wind speeds have been shown to vary from 20 m/s in the easterly direction to 325 m/s westward. At the cloud tops, the prevailing winds range in speed from 400 m/s along the equator to 250 m/s at the poles. Most of the winds on Neptune move in a direction opposite the planet's rotation. The general pattern of winds showed prograde rotation at high latitudes vs. retrograde rotation at lower latitudes. The difference in flow direction is thought to be a "skin effect" and not due to any deeper atmospheric processes. At 70° S latitude, a high-speed jet travels at a speed of 300 m/s.

Questions:
What dynamic weather does Neptune have?
What does Neptune's wind speeds reach?
What is the high wind speed on Neptune's cloud tops?
Which direction does Neptune's winds move relevant to the plant's rotation?
What is the effect called that describes the flow direction on Neptune?
In 2007, it was discovered that the upper troposphere of Neptune's south pole was about 10 K warmer than the rest of its atmosphere, which averages approximately 73 K (−200 °C). The temperature differential is enough to let methane, which elsewhere is frozen in the troposphere, escape into the stratosphere near the pole. The relative "hot spot" is due to Neptune's axial tilt, which has exposed the south pole to the Sun for the last quarter of Neptune's year, or roughly 40 Earth years. As Neptune slowly moves towards the opposite side of the Sun, the south pole will be darkened and the north pole illuminated, causing the methane release to shift to the north pole.

Questions:
How much warmer is Neptune's south pole to the rest of it's atmosphere?
Where does methane in the south pole escape to on Neptune?
What is the average temperature of Neptune's south pole?
How many earth years is Neptune's south pole exposed to the sun?
To which pole will Neptune's methane shift to as it moves to the opposite side of the sun?
The Scooter is another storm, a white cloud group farther south than the Great Dark Spot. This nickname first arose during the months leading up to the Voyager 2 encounter in 1989, when they were observed moving at speeds faster than the Great Dark Spot (and images acquired later would subsequently reveal the presence of clouds moving even faster than those that had initially been detected by Voyager 2). The Small Dark Spot is a southern cyclonic storm, the second-most-intense storm observed during the 1989 encounter. It was initially completely dark, but as Voyager 2 approached the planet, a bright core developed and can be seen in most of the highest-resolution images.

Questions:
What white cloud group on Neptune is farther south than the dark great spot?
When was The Scooter on Neptune observed?
What type of storm is The Scooter on Neptune?
What detected the storms on Neptune?
What is the second most intense storm on Neptune?
Neptune's dark spots are thought to occur in the troposphere at lower altitudes than the brighter cloud features, so they appear as holes in the upper cloud decks. As they are stable features that can persist for several months, they are thought to be vortex structures. Often associated with dark spots are brighter, persistent methane clouds that form around the tropopause layer. The persistence of companion clouds shows that some former dark spots may continue to exist as cyclones even though they are no longer visible as a dark feature. Dark spots may dissipate when they migrate too close to the equator or possibly through some other unknown mechanism.

Questions:
Where are Neptune's dark spots thought to occur?
What do Neptune's dark spots appear as in the cloud decks?
Since Neptune's dark spots persist for several months, what are they thought to be?
What on Neptune are associated with dark spots that are brighter?
When Neptune's dark spots migrate too close to the equator, what do they do?
Neptune's more varied weather when compared to Uranus is due in part to its higher internal heating. Although Neptune lies over 50% further from the Sun than Uranus, and receives only 40% its amount of sunlight, the two planets' surface temperatures are roughly equal. The upper regions of Neptune's troposphere reach a low temperature of 51.8 K (−221.3 °C). At a depth where the atmospheric pressure equals 1 bar (100 kPa), the temperature is 72.00 K (−201.15 °C). Deeper inside the layers of gas, the temperature rises steadily. As with Uranus, the source of this heating is unknown, but the discrepancy is larger: Uranus only radiates 1.1 times as much energy as it receives from the Sun; whereas Neptune radiates about 2.61 times as much energy as it receives from the Sun. Neptune is the farthest planet from the Sun, yet its internal energy is sufficient to drive the fastest planetary winds seen in the Solar System. Depending on the thermal properties of its interior, the heat left over from Neptune's formation may be sufficient to explain its current heat flow, though it is more difficult to simultaneously explain Uranus's lack of internal heat while preserving the apparent similarity between the two planets.

Questions:
Why might Neptune have more varied weather than Uranus?
How much farther is Neptune from the Sun than Uranus?
How much percentage of the sun does Neptune get compared to Uranus?
How much more energy does Neptune radiate than it receives?
The current heat flow on Neptune might be explained by what?
On 11 July 2011, Neptune completed its first full barycentric orbit since its discovery in 1846, although it did not appear at its exact discovery position in the sky, because Earth was in a different location in its 365.26-day orbit. Because of the motion of the Sun in relation to the barycentre of the Solar System, on 11 July Neptune was also not at its exact discovery position in relation to the Sun; if the more common heliocentric coordinate system is used, the discovery longitude was reached on 12 July 2011.

Questions:
When did Neptune complete it's first barycentric orbit since it's discovery?
What is the Earth's orbit?
Why didn't Neptune appear to be in it's exact discover position?
Using the heliocentric coordinate system, when did Neptune reach the discovery longitude?
Neptune's orbit has a profound impact on the region directly beyond it, known as the Kuiper belt. The Kuiper belt is a ring of small icy worlds, similar to the asteroid belt but far larger, extending from Neptune's orbit at 30 AU out to about 55 AU from the Sun. Much in the same way that Jupiter's gravity dominates the asteroid belt, shaping its structure, so Neptune's gravity dominates the Kuiper belt. Over the age of the Solar System, certain regions of the Kuiper belt became destabilised by Neptune's gravity, creating gaps in the Kuiper belt's structure. The region between 40 and 42 AU is an example.

Questions:
What is the region behind Neptune called?
What does the Kuiper belt consist of?
Where is the Kuiper belt relative to Neptune?
What dominates the Kuiper belt?
What did Neptune's gravity do to Kuiper belt?
There do exist orbits within these empty regions where objects can survive for the age of the Solar System. These resonances occur when Neptune's orbital period is a precise fraction of that of the object, such as 1:2, or 3:4. If, say, an object orbits the Sun once for every two Neptune orbits, it will only complete half an orbit by the time Neptune returns to its original position. The most heavily populated resonance in the Kuiper belt, with over 200 known objects, is the 2:3 resonance. Objects in this resonance complete 2 orbits for every 3 of Neptune, and are known as plutinos because the largest of the known Kuiper belt objects, Pluto, is among them. Although Pluto crosses Neptune's orbit regularly, the 2:3 resonance ensures they can never collide. The 3:4, 3:5, 4:7 and 2:5 resonances are less populated.

Questions:
What is the fraction of the most heavily populated resonance in the Kuiper belt?
What is the best known, and largest, object in the Kuiper belt?
How many known objects is in the most populated resonance of the Kuiper belt?
What is the resonance of Pluto in the Kuiper belt?
Which resonances are less populated in the Kuiper belt?
The formation of the ice giants, Neptune and Uranus, has proven difficult to model precisely. Current models suggest that the matter density in the outer regions of the Solar System was too low to account for the formation of such large bodies from the traditionally accepted method of core accretion, and various hypotheses have been advanced to explain their formation. One is that the ice giants were not formed by core accretion but from instabilities within the original protoplanetary disc and later had their atmospheres blasted away by radiation from a nearby massive OB star.

Questions:
What could have blasted Neptune and Uranus's atmosphere with radiation, aiding in creation?
What is too low to account for the formation of Neptune?
If Neptune was formed from instabilities within the original protoplanetary disc, what was it not formed by?
Neptune has 14 known moons. Triton is the largest Neptunian moon, comprising more than 99.5% of the mass in orbit around Neptune,[e] and it is the only one massive enough to be spheroidal. Triton was discovered by William Lassell just 17 days after the discovery of Neptune itself. Unlike all other large planetary moons in the Solar System, Triton has a retrograde orbit, indicating that it was captured rather than forming in place; it was probably once a dwarf planet in the Kuiper belt. It is close enough to Neptune to be locked into a synchronous rotation, and it is slowly spiralling inward because of tidal acceleration. It will eventually be torn apart, in about 3.6 billion years, when it reaches the Roche limit. In 1989, Triton was the coldest object that had yet been measured in the Solar System, with estimated temperatures of 38 K (−235 °C).

Questions:
How many moons does Neptune have?
What is Neptune's largest moon?
Who discovered Triton?
What orbit does Triton have around Neptune?
What does Triton's orbit suggest about it's relation to Neptune?
From July to September 1989, Voyager 2 discovered six moons of Neptune. Of these, the irregularly shaped Proteus is notable for being as large as a body of its density can be without being pulled into a spherical shape by its own gravity. Although the second-most-massive Neptunian moon, it is only 0.25% the mass of Triton. Neptune's innermost four moons—Naiad, Thalassa, Despina and Galatea—orbit close enough to be within Neptune's rings. The next-farthest out, Larissa, was originally discovered in 1981 when it had occulted a star. This occultation had been attributed to ring arcs, but when Voyager 2 observed Neptune in 1989, Larissa was found to have caused it. Five new irregular moons discovered between 2002 and 2003 were announced in 2004. A new moon and the smallest yet, S/2004 N 1, was found in 2013. Because Neptune was the Roman god of the sea, Neptune's moons have been named after lesser sea gods.

Questions:
What discovered six moons of Neptune in 1989?
What is the second most massive Neptunian moon?
What is notable about the moon Proteus?
Which are Neptune's four innermost moons?
When was Neptune's moon Larissa discovered?
The key advantage of the four-rail system is that neither running rail carries any current. This scheme was introduced because of the problems of return currents, intended to be carried by the earthed (grounded) running rail, flowing through the iron tunnel linings instead. This can cause electrolytic damage and even arcing if the tunnel segments are not electrically bonded together. The problem was exacerbated because the return current also had a tendency to flow through nearby iron pipes forming the water and gas mains. Some of these, particularly Victorian mains that predated London's underground railways, were not constructed to carry currents and had no adequate electrical bonding between pipe segments. The four-rail system solves the problem. Although the supply has an artificially created earth point, this connection is derived by using resistors which ensures that stray earth currents are kept to manageable levels. Power-only rails can be mounted on strongly insulating ceramic chairs to minimise current leak, but this is not possible for running rails which have to be seated on stronger metal chairs to carry the weight of trains. However, elastomeric rubber pads placed between the rails and chairs can now solve part of the problem by insulating the running rails from the current return should there be a leakage through the running rails.

Questions:
What danger can return currents cause?
How are stray earth currents kept to a manageable levels?
What insures minimal current leak during power rails instalation?
How did return current effect water and gas in iron pipes?
What is the crucial advantage of four-rail system?
Newly electrified lines often show a "sparks effect", whereby electrification in passenger rail systems leads to significant jumps in patronage / revenue. The reasons may include electric trains being seen as more modern and attractive to ride, faster and smoother service, and the fact that electrification often goes hand in hand with a general infrastructure and rolling stock overhaul / replacement, which leads to better service quality (in a way that theoretically could also be achieved by doing similar upgrades yet without electrification). Whatever the causes of the sparks effect, it is well established for numerous routes that have electrified over decades.

Questions:
What can be seen in the newly electrified lines?
What can electrification of modern trains effect?
How can better service quality be achieved?
As civil wars engulfed several Central American countries in the 1980s, hundreds of thousands of Salvadorans fled their country and came to the United States. Between 1980 and 1990, the Salvadoran immigrant population in the United States increased nearly fivefold from 94,000 to 465,000. The number of Salvadoran immigrants in the United States continued to grow in the 1990s and 2000s as a result of family reunification and new arrivals fleeing a series of natural disasters that hit El Salvador, including earthquakes and hurricanes. By 2008, there were about 1.1 million Salvadoran immigrants in the United States.

Questions:
Why did Central Americans flee to the U.S.?
When did Salvadorans flee
Are the Salvadorans a large population in the U.S.?
Is the  Salvadoran population still growing?
How many  Salvadorans  are in America now?
Until the 20th century, there was no clear record of the number of Venezuelans who emigrated to the United States. Between the 18th and early 19th centuries, there were many European immigrants who went to Venezuela, only to later migrate to the United States along with their children and grandchildren who born and/or grew up in Venezuela speaking Spanish. From 1910 to 1930, it is estimated that over 4,000 South Americans each year emigrated to the United States; however, there are few specific figures indicating these statistics. Many Venezuelans settled in the United States with hopes of receiving a better education, only to remain in there following graduation. They are frequently joined by relatives. However, since the early 1980s, the reasons for Venezuelan emigration have changed to include hopes of earning a higher salary and due to the economic fluctuations in Venezuela which also promoted an important migration of Venezuelan professionals to the US.

Questions:
When did the Venezuelans emigrate to the united states?
Does Venezuela have immigrates from other countries?
Why did Venezuelans come to America?
Do Venezuelans still come to America for the same reasons as they did before?