romikgosai/squad_modified_2 huggingface dataset:
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.

Q1: What is Neptune's atmosphere made of?
A1: 80% hydrogen and 19% helium
Q2: Where are absorption bands of methane on Neptune?
A2: wavelengths above 600 nm
Q3: What gives Neptune it's blue hue?
A3: absorption of red light by the atmospheric methane
Q4: What planet also gets it's color from atmospheric constituent?
A4: Uranus
Q5: What color is Uranus, compared to Neptune?
A5: cyan
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.

Q1: What is Neptune's clouds competition variants dependent on?
A1: altitude
Q2: Which clouds on Neptune are suitable for methane to condense?
A2: upper-level
Q3: What clouds form between one and five bars on Neptune?
A3: ammonia and hydrogen sulfide
Q4: On Neptune, what do clouds above five bars consist of?
A4: ammonia, ammonium sulfide, hydrogen sulfide and water
Q5: What is the temperature on Neptune's clouds that are at 50 bars?
A5: 273 K (0 °C)
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.

Q1: On Neptune, which clouds cast shadows on the cloud deck below it?
A1: High-altitude clouds
Q2: What are the widths of the cloud bands on Neptune?
A2: 50–150 km
Q3: Where are the high altitude bands of clouds on Neptune?
A3: 50–110 km above the cloud deck.
Q4: What does Neptune have more of compared to Uranus?
A4: volume of ocean
Q5: Where on Neptune does weather not occur?
A5: higher stratosphere or thermosphere
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.

Q1: What is Neptune's temperature in the thermosphere?
A1: 750 K
Q2: What would interact with Neptune's magnetic field to make it warm?
A2: atmospheric interaction with ions
Q3: Where would gravity waves in Neptune's interior dissipate?
A3: in the atmosphere
Q4: What does Neptune's thermosphere containers traces of?
A4: carbon dioxide and water
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.

Q1: What is the rotational axis of Neptune's magnetic field?
A1: 47°
Q2: Where is Neptune's magnetic field offset from the physical centre?
A2: 0.55 radii
Q3: What planet besides Neptune has a sideways rotation?
A3: Uranus's
Q4: What might cause Neptune's extreme orientation?
A4: flows in the planets' interiors
Q5: What fluids are in Neptune's interior?
A5: ammonia, methane and water
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.

Q1: What is Neptune's dipole magnetic moment?
A1: 2.2 × 1017 T·m3
Q2: What is one of Neptune's non-dipolar component what may exceed the dipole moment in strength?
A2: strong quadrupole moment
Q3: Which three planets have small quadrupole moments compared to Neptune?
A3: Earth, Jupiter and Saturn
Q4: Besides the geometrical constraints of Neptune's dynamo generator, what is another result of the quadrupole moment?
A4: the planet's centre
Q5: What is the dipole component of the magnetic field at the magnetic equator of neptune?
A5: 14 microteslas (0.14 G)
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.

Q1: What system, like Saturn, does Neptune have?
A1: planetary ring system
Q2: What might Neptune's rings consist of?
A2: ice particles
Q3: What might the ice particles of Neptune's rings be coated with?
A3: silicates or carbon-based material
Q4: Where is Adams ring from the center of Neptune?
A4: 63,000 km
Q5: Where is the La Verrier ring from the center of Neptune?
A5: 53,000 km
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.

Q1: What dynamic weather does Neptune have?
A1: storm
Q2: What does Neptune's wind speeds reach?
A2: 600 m/s (2,200 km/h; 1,300 mph)
Q3: What is the high wind speed on Neptune's cloud tops?
A3: 400 m/s
Q4: Which direction does Neptune's winds move relevant to the plant's rotation?
A4: opposite
Q5: What is the effect called that describes the flow direction on Neptune?
A5: skin effect
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.

Q1: How much warmer is Neptune's south pole to the rest of it's atmosphere?
A1: 10 K
Q2: Where does methane in the south pole escape to on Neptune?
A2: the stratosphere near the pole.
Q3: What is the average temperature of Neptune's south pole?
A3: 73 K (−200 °C).
Q4: How many earth years is Neptune's south pole exposed to the sun?
A4: 40
Q5: To which pole will Neptune's methane shift to as it moves to the opposite side of the sun?
A5: north pole
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.

Q1: What white cloud group on Neptune is farther south than the dark great spot?
A1: The Scooter
Q2: When was The Scooter on Neptune observed?
A2: 1989
Q3: What type of storm is The Scooter on Neptune?
A3: southern cyclonic storm
Q4: What detected the storms on Neptune?
A4: Voyager 2)
Q5: What is the second most intense storm on Neptune?
A5: The Small Dark Spot
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.

Q1: Where are Neptune's dark spots thought to occur?
A1: in the troposphere
Q2: What do Neptune's dark spots appear as in the cloud decks?
A2: holes
Q3: Since Neptune's dark spots persist for several months, what are they thought to be?
A3: vortex structures
Q4: What on Neptune are associated with dark spots that are brighter?
A4: methane clouds
Q5: When Neptune's dark spots migrate too close to the equator, what do they do?
A5: dissipate
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.

Q1: Why might Neptune have more varied weather than Uranus?
A1: higher internal heating
Q2: How much farther is Neptune from the Sun than Uranus?
A2: 50%
Q3: How much percentage of the sun does Neptune get compared to Uranus?
A3: 40%
Q4: How much more energy does Neptune radiate than it receives?
A4: 2.61
Q5: The current heat flow on Neptune might be explained by what?
A5: heat left over from Neptune's formation
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.

Q1: When did Neptune complete it's first barycentric orbit since it's discovery?
A1: 11 July 2011
Q2: What is the Earth's orbit?
A2: 365.26-day
Q3: Why didn't Neptune appear to be in it's exact discover position?
A3: Earth was in a different location
Q4: Using the heliocentric coordinate system, when did Neptune reach the discovery longitude?
A4: 12 July 2011
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.

Q1: What is the region behind Neptune called?
A1: Kuiper belt
Q2: What does the Kuiper belt consist of?
A2: small icy worlds
Q3: Where is the Kuiper belt relative to Neptune?
A3: 30 AU out to about 55 AU from the Sun
Q4: What dominates the Kuiper belt?
A4: Neptune's gravity
Q5: What did Neptune's gravity do to Kuiper belt?
A5: gaps in the Kuiper belt's structure
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.

Q1: What is the fraction of the most heavily populated resonance in the Kuiper belt?
A1: 2:3 resonance
Q2: What is the best known, and largest, object in the Kuiper belt?
A2: Pluto
Q3: How many known objects is in the most populated resonance of the Kuiper belt?
A3: 200
Q4: What is the resonance of Pluto in the Kuiper belt?
A4: 2:3
Q5: Which resonances are less populated in the Kuiper belt?
A5: 3:4, 3:5, 4:7 and 2:5
Neptune has a number of known trojan objects occupying both the Sun–Neptune L4 and L5 Lagrangian points—gravitationally stable regions leading and trailing Neptune in its orbit, respectively. Neptune trojans can be viewed as being in a 1:1 resonance with Neptune. Some Neptune trojans are remarkably stable in their orbits, and are likely to have formed alongside Neptune rather than being captured. The first and so far only object identified as associated with Neptune's trailing L5 Lagrangian point is 2008 LC18. Neptune also has a temporary quasi-satellite, (309239) 2007 RW10. The object has been a quasi-satellite of Neptune for about 12,500 years and it will remain in that dynamical state for another 12,500 years.

Q1: What is the resonance of Neptune trojans?
A1: 1:1
Q2: Where did most Neptune trojans form?
A2: alongside Neptune
Q3: What is the only object identified with Neptune's trailing L5 Lagrangian point?
A3: 2008 LC18
Q4: What is Neptune's temporary quasi-satellite named?
A4: (309239) 2007 RW10
Q5: How long has Neptune's quasi-satellite been with Neptune?
A5: 12,500 years
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.

Q1: What could have blasted Neptune and Uranus's atmosphere with radiation, aiding in creation?
A1: nearby massive OB star
Q2: What is too low to account for the formation of Neptune?
A2: matter density
Q3: If Neptune was formed from instabilities within the original protoplanetary disc, what was it not formed by?
A3: core accretion
An alternative concept is that they formed closer to the Sun, where the matter density was higher, and then subsequently migrated to their current orbits after the removal of the gaseous protoplanetary disc. This hypothesis of migration after formation is favoured, due to its ability to better explain the occupancy of the populations of small objects observed in the trans-Neptunian region. The current most widely accepted explanation of the details of this hypothesis is known as the Nice model, which explores the effect of a migrating Neptune and the other giant planets on the structure of the Kuiper belt.

Q1: If Neptune formed closer to the sun, what is the matter density?
A1: higher
Q2: If Neptune formed closer to the sun, what caused it to migrate to it's current orbit?
A2: removal of the gaseous protoplanetary disc
Q3: What is the most widely accepted explanation of Neptune's formation called?
A3: the Nice model
Q4: What does The Nice model consider effected the migration of Neptune?
A4: Kuiper belt.
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).

Q1: How many moons does Neptune have?
A1: 14
Q2: What is Neptune's largest moon?
A2: Triton
Q3: Who discovered Triton?
A3: William Lassell
Q4: What orbit does Triton have around Neptune?
A4: retrograde orbit
Q5: What does Triton's orbit suggest about it's relation to Neptune?
A5: that it was captured
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.

Q1: What discovered six moons of Neptune in 1989?
A1: Voyager 2
Q2: What is the second most massive Neptunian moon?
A2: Proteus
Q3: What is notable about the moon Proteus?
A3: irregularly shaped
Q4: Which are Neptune's four innermost moons?
A4: Naiad, Thalassa, Despina and Galatea
Q5: When was Neptune's moon Larissa discovered?
A5: 1981
Because of the distance of Neptune from Earth, its angular diameter only ranges from 2.2 to 2.4 arcseconds, the smallest of the Solar System planets. Its small apparent size makes it challenging to study it visually. Most telescopic data was fairly limited until the advent of Hubble Space Telescope (HST) and large ground-based telescopes with adaptive optics (AO). The first scientifically useful observation of Neptune from ground-based telescopes using adaptive optics, was commenced in 1997 from Hawaii. Neptune is currently entering its spring and summer season and has been shown to be heating up, with increased atmospheric activity and brightness as a consequence. Combined with technological advancements, ground-based telescopes with adaptive optics are recording increasingly more detailed images of this Outer Planet. Both the HST and AO telescopes on Earth has made many new discoveries within the Solar System since the mid-1990s, with a large increase in the number of known satellites and moons around the Outer Planets for example. In 2004 and 2005, five new small satellites of Neptune with diameters between 38 and 61 kilometres were discovered.

Q1: What is Neptune's angular diameter range?
A1: 2.2 to 2.4 arcseconds
Q2: The advent of what telescope made it easier to study Neptune?
A2: Hubble Space Telescope
Q3: When was the first useful observation of Neptune from the ground?
A3: 1997
Q4: What seasons are Neptune currently entering?
A4: spring and summer
Q5: What was discovered around Neptune in 2004 and 2005?
A5: five new small satellites
Voyager 2 is the only spacecraft that has visited Neptune. The spacecraft's closest approach to the planet occurred on 25 August 1989. Because this was the last major planet the spacecraft could visit, it was decided to make a close flyby of the moon Triton, regardless of the consequences to the trajectory, similarly to what was done for Voyager 1's encounter with Saturn and its moon Titan. The images relayed back to Earth from Voyager 2 became the basis of a 1989 PBS all-night program, Neptune All Night.

Q1: What is the only spacecraft to visit Neptune?
A1: Voyager 2
Q2: When did a spacecraft get closest to Neptune?
A2: 25 August 1989
Q3: What near Neptune did a spacecraft visit dangerously close?
A3: Triton
Q4: What program aired on PBS about Neptune?
A4: Neptune All Night