Title: Kepler-1520
Content:  Kepler-1520 (initially published as KIC 12557548) is a K-type main-sequence star located in the constellation Cygnus. The star is particularly important, as measurements taken by the Kepler spacecraft indicate that the variations in the star's light curve cover a range from about 0.2% to 1.3% of the star's light being blocked. This indicates that there may be a rapidly disintegrating planet, a prediction not yet conclusively confirmed, in orbit around the star, losing mass at a rate of 1 Earth mass every billion years. The planet itself is about 0.1 Earth masses, or just twice the mass of Mercury, and is expected to disintegrate in about 100 -200 million years. The planet orbits its star in just 15.7 hours, at a distance only two stellar diameters away from the star's surface, and has an estimated effective temperature of about 2255 K. The orbital period of the planet is one of the shortest ever detected in the history of the extrasolar planet search. In 2016, the planet was confirmed as part of a data release by the Kepler spacecraft.
Title: HD 179070
Content:  The single known planet orbiting this star was identified as a candidate based on photometry from the first four months of data from the Kepler spacecraft. Confirmation was obtained in 2012 after extensive follow-up observations and analysis of the Kepler light curves. The calculated density of the planet is approximately 6.4 g cm−3, similar to earth's 5.5 g cm−3, which suggests a rocky composition. With an equilibrium temperature of 2025 Kelvin, the top few-hundred kilometers of the planet is probably molten.
Title: Kepler-22b
Content:  It is likely to have a volatile-rich composition with a liquid or gaseous outer shell. The only parameters of the planet's orbit that are currently available are its orbital period, which is about 290 days, and its inclination, which is approximately 90°. Evidence suggests that the planet has a moderate surface temperature, assuming that the surface is not subject to extreme greenhouse heating. In the absence of an atmosphere, its equilibrium temperature (assuming an Earth-like albedo) would be approximately 262 K, compared with Earth's 255 K. The planet's first transit was observed on 12 May 2009. Confirmation of the existence of Kepler-22b was announced on 5 December 2011.
Title: HD 205739
Content:  with a projected rotational velocity of 4 km/s. It has 1.3 times the mass of the Sun and 1.6 times the Sun's radius. The abundance of iron is 60% greater than in the Sun, suggesting a higher metallicity. The star is radiating 3.5 times the luminosity of the Sun from its photosphere at an effective temperature of 6,276 K. A Jupiter-like planet has been detected in an eccentric orbit around this star via Doppler spectroscopy. The eccentricity of 0.27 indicates that the orbit carries the body from 0.65 AU out to 1.14 AU between periastron and apastron. The maximum surface temperature of the planet is ~400 K, varying by 100 K over the course of an orbit. There is a data trend in the results which may point to an additional companion further from its star, but this will require a longer observation period to validate.
Title: HD 50554
Content:  2.3 km/s. The star has a slightly higher mass and larger radius than the Sun. It is radiating 137% of the luminosity of the Sun from its photosphere at an effective temperature of 6,036 K. In 2001, a giant planet was announced by the European Southern Observatory, who used the radial velocity method. The discovery was confirmed in 2002 using observations from the lick and keck telescopes. An infrared excess indicates a debris disk is orbiting the star at a distance of 45 AU with a half-width of 4 AU. This may be an analog of the Kuiper belt at an earlier stage of its evolution, which suggests a Neptune-like planet could be orbiting at its inner edge.
Title: HD 171028
Content:  a projected rotational velocity of 2.3 km/s. It has the same mass as the Sun, but the radius is 2.4 times larger. The star is radiating 5.4 times the luminosity of the Sun from its photosphere at an effective temperature of 5,671 K. In the summer of 2007, a Jovian planetary companion was discovered by the HARPS planet search program using the radial velocity method. This object is orbiting at a distance of 1.32 AU from the host star with a period of 550 days and an eccentricity (ovalness) of 0.59. Since the inclination of the orbit is unknown, only a minimum mass can be determined. This planet has at least double the mass of Jupiter.
Title: Kepler-44
Content:  The Kepler spacecraft detected a transiting planet candidate around this star that was confirmed by radial velocity measurements taken by the SOPHIE spectrograph mounted on the 1.93 m telescope at the Haute-Provence Observatory. The planet is likely to be tidally locked to the parent star. In 2015, the planetary nightside temperature was estimated to be equal to 2347 K.
Title: HD 153950 b
Content:  The temperature of the exoplanet is likely to vary during its orbit, temperatures would likely range from 275–375 K as it approaches its periastron/apastron of its orbit. This would also likely apply to a potentially habitable hypothetical moon orbiting the gas giant exoplanet (see below).
Title: Kepler-62e
Content:  The planet orbits a (K-type) star named Kepler-62, orbited by a total of five planets. The star has a mass of 0.69 and a radius of 0.64. It has a temperature of 4,925 K and is 7 billion years old. In comparison, the Sun is 4.6 billion years old and has a temperature of 5,778 K. The star is somewhat metal-poor, with a metallicity ([Fe/H]) of −0.37, or 42% of the solar amount. Its luminosity is 21% that of the Sun. The star's apparent magnitude, or how bright it appears from Earth's perspective, is 13.65. Therefore, it is too dim to be seen with the naked eye.
Title: Kepler-42
Content:  to small size of the star, causing these planets to block a larger proportion of starlight during their transits. Not all of the orbital parameters of the system are known. For example, as with all transiting planets that have not had their properties established by means of other methods such as the radial velocity method, the orbital eccentricity remains unknown. Based on the orbits of the planets and the luminosity and effective temperature of the host star, the equilibrium temperatures of the planets can be calculated. Assuming an extremely high albedo of 0.9 and absence of greenhouse effect, the outer planet Kepler-42 d would have an equilibrium temperature of about 280 K, similar to Earth's 255 K. Estimates for the known planets are in the tables below:

Question: Verify the following claims with "True" or "False": The celestial body known as a planet has an escape velocity of 0.02 k.p.s., a temperature of 155 kelvins and an apoapsis of 520906000.0 kilometres.
Answer: True