Title: Escape velocity
Content:  In celestial mechanics, escape velocity or escape speed is the minimum speed needed for a free, non-propelled object to escape from the gravitational influence of a primary body, thus reaching an infinite distance from it. It is typically stated as an ideal speed, ignoring atmospheric friction. Although the term "escape velocity" is common, it is more accurately described as a speed than a velocity because it is independent of direction; the escape speed increases with the mass of the primary body and decreases with the distance from the primary body. The escape speed thus depends on how far the object has already traveled, and its calculation 
Title: 2012 FP35
Content:   is an Apollo asteroid about 11 meters in diameter, that made some close approaches to Earth. It orbits the Sun every 583.2 days,  in an ellipse between 0.749 AU  and 1.983. It was discovered on March 24, 2012 by the Catalina Sky Survey. This asteroids was calculated to have passed roughly 0.22 AU from Earth on September 20, 2015. It came within 0.00107 AU of Earth on March 26, 2012. The asteroid is about 7–15 meters in diameter. The size of the asteroid is estimated from the absolute magnitude.
Title: Geocentric orbit
Content:  equator on the Earth to the celestial sphere. ; Escape velocity: as used here, the minimum velocity an object without propulsion needs to have to move away indefinitely from the Earth. An object at this velocity will enter a parabolic trajectory; above this velocity it will enter a hyperbolic trajectory. ; Impulse: the integral of a force over the time during which it acts. Measured in (N·sec or lb * sec). ; Inclination: the angle between a reference plane and another plane or axis. In the sense discussed here the reference plane is the Earth's equatorial plane. ; Orbital characteristics: the six parameters of the Keplerian elements needed to specify 
Title: New Horizons
Content:  New Horizons has been called "the fastest spacecraft ever launched" because it left Earth at 16.26 km/s. It is also the first spacecraft launched directly into a solar escape trajectory, which requires an approximate speed while near Earth of 16.5 km/s, plus additional delta-v to cover air and gravity drag, all to be provided by the launch vehicle. However, it is not the fastest spacecraft to leave the Solar System. , this record is held by Voyager 1, traveling at 16.985 km/s relative to the Sun. Voyager 1 attained greater hyperbolic excess velocity than New Horizons due to gravity assists by Jupiter and Saturn. When New Horizons reaches the distance of 100 AU, it will be travelling at about 13 km/s, around 4 km/s slower than Voyager 1 
Title: 2019 OU1
Content:  On 28 August 2019, safely passed 0.00687 au from Earth, travelling at around 13 km/s.
Title: Orbital speed
Content:  The closer an object is to the Sun the faster it needs to move to maintain the orbit. Objects move fastest at perihelion (closest approach to the Sun) and slowest at aphelion (furthest distance from the Sun). Since planets in the Solar System are in nearly circular orbits their individual orbital velocities do not vary much. Being closest to the Sun and having the most eccentric orbit, Mercury's orbital speed varies from about 59 km/s at perihelion to 39 km/s at aphelion. Halley's Comet on an eccentric orbit that reaches beyond Neptune will be moving 54.6 km/s when 0.586 AU from the Sun, 41.5 km/s when 1 AU from the Sun (passing Earth's orbit), and roughly 1 km/s at aphelion 35 AU from the Sun. Objects passing Earth's orbit going faster than 42.1 km/s have achieved escape velocity and will be ejected from the Solar System if not slowed down by a gravitational interaction with a planet.
Title: JPL Horizons On-Line Ephemeris System
Content:  Objects (such as C/1980 E1) on an outbound ejection trajectory will show an eccentricity greater than 1, an apoapsis distance of AD= 9.99E+99 and an orbit period of PR= 9.99E+99. For objects orbiting the Sun, this is best computed at an epoch (date) when the object is outside of the planetary region of the Solar System and no longer subject to notable planetary perturbation. Due to the galactic tide and passing stars it is impossible to know if an object with a weak hyperbolic trajectory will truly be ejected or gently nudged back inward. The galactic tide and passing stars can also cause objects inbound from the Oort cloud to have a weakly hyperbolic trajectory.
Title: Orbital mechanics
Content:  The formula for an escape velocity is derived as follows. The specific energy (energy per unit mass) of any space vehicle is composed of two components, the specific potential energy and the specific kinetic energy. The specific potential energy associated with a planet of mass M is given by The escape velocity from the Earth's surface is about 11 km/s, but that is insufficient to send the body an infinite distance because of the gravitational pull of the Sun. To escape the Solar System from a location at a distance from the Sun equal to the distance Sun–Earth, but not close to the Earth, requires around 42 km/s velocity, but there will be "partial credit" for the Earth's orbital velocity for spacecraft launched from Earth, if their further acceleration (due to the propulsion system) carries them in the same direction as Earth travels in its orbit.
Title: Phaeton (hypothetical planet)
Content:  velocity. Once the escaped satellite re-entered Phaeton's Hill sphere, it collided with the planet at high speed, shattering it while Ceres, Pallas, Juno, and Vesta assumed heliocentric orbits. Simulations showed that for such a Ceres-sized body to shatter Phaeton, it would need to be travelling at nearly 20 kilometers per second. The disrupted planet hypothesis has also been supported by French-Italian mathematician and astronomer Joseph-Louis Lagrange; Canadian geologist Reginald Daly in 1943; American geochemists Harrison Brown and Clair Patterson; Soviet academics Konstantin Savchenko, Alexander Zavaritskiy, Vasily Fesenkov, Ivan Putilin, and Otto Schmidt; British-Canadian astronomer Michael Ovenden; and American astronomer Donald Menzel. 
Title: Escape velocity
Content:  In this table, the left-hand half gives the escape velocity from the visible surface (which may be gaseous as with Jupiter for example), relative to the centre of the planet or moon (that is, not relative to its moving surface). In the right-hand half, Ve refers to the speed relative to the central body (for example the sun), whereas Vte is the speed (at the visible surface of the smaller body) relative to the smaller body (planet or moon). The last two columns will depend precisely where in orbit escape velocity is reached, as the orbits are not exactly circular (particularly Mercury and Pluto).

Question: Verify the following claims with "True" or "False": A planet has an escape velocity of 0.0112 kilometres per second and its apoapsis is 511592000.0 kms.
Answer: True