Title: Longitude of the periapsis
Content:  In celestial mechanics, the longitude of the periapsis, also called longitude of the pericenter, of an orbiting body is the longitude (measured from the point of the vernal equinox) at which the periapsis (closest approach to the central body) would occur if the body's orbit inclination were zero. It is usually denoted ϖ. For the motion of a planet around the Sun, this position is called longitude of perihelion ϖ, which is the sum of the longitude of the ascending node Ω, and the argument of perihelion ω. The longitude of periapsis is a compound angle, with part of it being measured in the plane of reference and the rest being measured in the plane of the orbit. Likewise, any angle derived from the longitude of periapsis (e.g., mean longitude and true longitude) will also be compound. Sometimes, the term longitude of periapsis is used to refer to ω, the angle between the ascending node and the periapsis. That usage of the term is especially common in discussions of binary stars and exoplanets. However, the angle ω is less ambiguously known as the argument of periapsis.
Title: (459883) 2014 JX55
Content:  When the object was first observed as by the Mount Lemmon Survey in March 2007, it was considered to have the second-smallest positive semi-major axis (0.55 AU) of any known object orbiting the Sun, after Mercury. It was classified as an Apohele asteroid, which always stay inside of Earth's orbit, approaching within 0.116 AU of the Sun approximately every 148 days, before leaving for a distance of 0.98 AU, making it a Mercury- and Venus-crossing asteroid. If these early orbital calculations had not turned out to be wrong, the object would still rank today among the inner heliospheric asteroids with the smallest known perihelia.
Title: (444004) 2004 AS1
Content:  orbits the Sun at a distance of 0.88–1.26 AU once every 13 months (405 days; semi-major axis of 1.07 AU). Its orbit has an eccentricity of 0.17 and an inclination of 17° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Socorro in January 2004.
Title: Expedition 4
Content: Perigee: 384 km ; Apogee: 396 km ; Inclination: 51.6° ; Period: 92 min 
Title: Longitude of the periapsis
Content: i, inclination ; ω, argument of perihelion ; Ω, longitude of ascending node ; ε, obliquity of the ecliptic (for the standard equinox of 2000.0, use 23.43929111°) Define the following: Then: The right ascension α and declination δ of the direction of perihelion are: If A < 0, add 180° to α to obtain the correct quadrant. The ecliptic longitude ϖ and latitude b of perihelion are: If cos(α) < 0, add 180° to ϖ to obtain the correct quadrant. As an example, using the most up-to-date numbers from Brown (2017) for the hypothetical Planet Nine with i = 30°, ω = 136.92°, and Ω = 94°, then α = 237.38°, δ = +0.41° and ϖ = 235.00°, b = +19.97° (Brown actually provides i, Ω, and ϖ, from which ω was computed).
Title: Equation of time
Content:  and D is the number of days past that epoch. At periapsis M = 2π , so solving gives D = Dp = 2.508. This puts the periapsis on 4 January 2000 at 00:11:41 while the actual periapsis is, according to results from the Multiyear Interactive Computer Almanac (abbreviated as MICA), on 3 January 2000 at 05:17:30. This large discrepancy happens because the difference between the orbital radius at the two locations is only 1 part in a million; in other words, radius is a very weak function of time near periapsis. As a practical matter this means that one cannot get a highly accurate result 
Title: (444004) 2004 AS1
Content:  Although rather ordinary, it caused some controversy in astronomical circles due to initial projections posted on the web by the Minor Planet Center (MPC) suggesting an imminent collision with Earth on or about January 15 with a likelihood of 1:4. These projections came from very early observations, and turned out to be inaccurate (which is an ordinary occurrence in astronomy, as new observations refine the projected path of an object). In fact, the poster at the MPC had not realised that the data he had posted was essentially an impact prediction. The asteroid passed Earth on 16 February 2004 at a distance of 0.08539 AU (or 33 times the distance from Earth to the Moon), posing no threat. It is an Apollo asteroid, with perihelion at 0.88 AU, a rather low eccentricity of 0.17, an inclination of 17° and an orbital period of 1.11 years.
Title: 4450 Pan
Content:  Pan orbits the Sun in the inner main-belt at a distance of 0.6–2.3 AU once every 1 years and 9 months (633 days). Its orbit has an eccentricity of 0.59 and an inclination of 6° with respect to the ecliptic. As an Apollo asteroid, it is an Earth-crosser and has a minimum orbit intersection distance with Earth of 0.0287 AU, which corresponds to 11.2 lunar distances. Due to its extremely eccentric orbit, it is also a Venus- and Mars-crosser and approaches Mercury within 20 Gm. It was first observed as  at Heidelberg Observatory in 1937. The body's observation arc begins at Palomar with its official discovery observation.
Title: (450894) 2008 BT18
Content:  orbits the Sun at a distance of 0.9–3.5 AU once every 3 years and 4 months (1,209 days). Its orbit has an eccentricity of 0.59 and an inclination of 8° with respect to the ecliptic. Published by the Digitized Sky Survey, a first precovery was taken at Palomar Observatory in 1955, extending the asteroid's observation arc by 53 years prior to its discovery. The asteroid has a low Earth minimum orbit intersection distance of 0.0108 AU which corresponds to 4.2 lunar distances (LD). On 14 July 2008, it transited Earth within 0.015 AU (5.9 LD).
Title: (84522) 2002 TC302
Content:  orbits the Sun at a distance of 39.2–71.4 AU once every 410 years and 12 months (150,105 days; semi-major axis of 55.28 AU). Its orbit has an eccentricity of 0.29 and an inclination of 35° with respect to the ecliptic. In December 2058, It will come to perihelion (minimum distance from the Sun) at 39.2 AU, which is about the same as Pluto's semi-major axis (average distance from the Sun). Given the long orbit that TNOs have around the Sun, comes to opposition in late October of each year at an apparent magnitude of 20.5. Both the Minor Planet Center (MPC) and the Deep Ecliptic Survey (DES) show to be a resonant trans-Neptunian object in a 2:5 resonance with Neptune, meaning it completes two orbits for every five orbits of Neptune.

Question: Verify the following claims with "True" or "False": The planet has a periapsis of 445895000000.0.
Answer: True