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Exoplanets scaled one in 120 million 3D MODEL ONLY tato_713 VIEW IN BROWSER updated 5. 3. 2021 | published 5. 3. 2021 Summary Some of the most notable Earth-sized exoplanets scaled (smaller than 2.5 Earth diameter). Learning > Physics & Astronomy trappist1h trappist1g trappist1f trappist1e trappist1d trappist1c trappist1b trappist1 trappist terrestrialplanet space scalemodel scaledmodel scale proximacentauri planets planetas planeta planet oceanworld kepler62b kepler62 kepler22b kepler22 kepler11b icegigant extraterrestrial corot7 chthonianplanet chthonian astronomy astronomia Originally published here: Exoplanets scaled one in 120 million by tato_713 - Thingiverse The concept of this post is to compare the size in the same scale of various Earth sized exoplanets with the Earth itself or other astronomical bodies like Neptune. Although there are thousands exoplanets confirmed, I made only some of the most notorious ones with known diameter, and nearly Earth sized (up to 2.5 its diameter). The models are just spheres scaled one in 120 million, to compare with terrestrial planets; one in 250 million; and one in 500 million for the biggest ones. The file's names explained: name_1_x_10_y.stl is 1 : x* 10^y. So _1_6_10_7 is 1:600000000 or one in 60 million. Proxima Centauri b Proxima b is the closest exoplanet known to the Solar System, the closest within the habitable zone of its star, the only known planet in the nearest star, Proxima Centauri, and the only one confirmed in the Alpha Centauri system. As is it said, the host star for the planet is part of the Alpha Centauri system, orbiting the two main stars Alpha Centauri A (Rigil Kentaurus) and B (Toliman). Proxima is a flare M type red dwarf while the others are G (Sun like) and K type (orange star) respectively. Flare stars are randomly emit huge flares that could have devastating effects on a close orbit planet atmosphere, unless it has a strong magnetic field. • Type: Planet. • Orbit: Proxima Centauri. • Distance to the Sun: 4.244 ly. • Orbital period: 11.186 d • Composition: Silicate rock. • Density: ~5 g/cm3. • Dimensions: ~14000 km • Model scale: 1:1.2x108 (11cm) 1:2.5x108 (5cm) Luyten b Luyten b is the fourth closest planet in the habitable zone. It's orbiting the Luyten's Star, which is a red dwarf, that unlike Proxima Centauri, it's relatively inactive. This planet is classified as a super-Earth, a planet bigger than Earth, but smaller than Neptune, it isn't related with its composition. • Type: Planet. • Orbit: Luyten's Star. • Distance to the Sun: 12.2 ly. • Orbital period: 18.6498 d • Composition: Silicate rock. • Density: ~6 g/cm3. • Dimensions: ~17000 km • Model scale: 1:1.2x108 (14cm) 1:2.5x108 (7cm) HD 219134 b This planet was at the time of its discovery, the closest known rocky planet. It orbits a K type star. It is in the hot zone of its system, which means that water cannot be liquid on its surface. It is one of the few exoplanets with a detected atmosphere. The star is visible to the naked eye, and is one of the oldest star know with 11 billion of years. • Type: Planet. • Orbit: HD 219134 • Distance to the Sun: 21.25 ly. • Orbital period: 3.092926 d • Composition: Silicate rock. • Density: ~6.4 g/cm3. • Dimensions: ~20400 km • Model scale: 1:1.2x108 (17cm) 1:2.5x108 (8cm) HD 219134 c The HD 219134 system has at least 5, and possibly 7, planets; of which the two most close to the star has known diameter. HD 219134 c is the second one, also with a possible atmosphere. The rest of the planets of this system are also more massive. • Type: Planet. • Orbit: HD 219134 • Distance to the Sun: 21.25 ly. • Orbital period: 6.76458 d • Composition: Silicate rock. • Density: ~7 g/cm3. • Dimensions: ~19250 km • Model scale: 1:1.2x108 (16cm) 1:2.5x108 (8cm) Gliese 1132 b • Type: Planet. • Orbit: Gliese 1132. • Distance to the Sun: 39 ly. • Orbital period: 1.6 d • Composition: Silicate rock. • Density: ~6.3 g/cm3. • Dimensions: ~14500 km • Model scale: 1:1.2x108 (12cm) 1:2.5x108 (6cm) Trappist-1 b Trappist-1 is one of the best studied exoplanets. It has 7 Earth sized planets that transit in front of the host star, viewed from the Solar System. It is an ultra-cool red dwarf slightly larger than Jupiter. All of the planets orbits very close to the star, comparable with the distance between the Earth and the Moon, so a planet of the system is visible from the surface of the others. The planet b (the closest to the star) has a Venus like atmosphere mainly composed of CO2 and it is inferred to have water vapor because of its low density. • Type: Planet. • Orbit: Trappist-1. • Distance to the Sun: 39.6 ly. • Orbital period: 1.51 d • Composition: Silicate rock. Water vapor and CO2 atmosphere • Density: ~4 g/cm3. • Dimensions: ~14200 km • Model scale: 1:1.2x108 (12cm) 1:2.5x108 (6cm) Trappist-1 c Trappist-1 c is, like the b, a Venus like planet with water vapor atmosphere, too hot to be liquid. Like most if not all the planet on the system it is likely tidal locked to the star. • Type: Planet. • Orbit: Trappist-1. • Distance to the Sun: 39.6 ly. • Orbital period: 2.42 d • Composition: Silicate rock. • Density: ~4.8 g/cm3. • Dimensions: ~14000 km • Model scale: 1:1.2x108 (11cm) 1:2.5x108 (5cm) Trappist-1 d Trappist-1 d is the smallest and less densest planet of the Trappist-1 system. It is between the size of Mars and Earth. This planet orbits the inner edge of the habitable zone, but it is likely tidal locked. • Type: Planet. • Orbit: Trappist-1. • Distance to the Sun: 39.6 ly. • Orbital period: 4.049 d • Composition: Silicate rock. • Density: ~3.4 g/cm3. • Dimensions: ~10000 km • Model scale: 1:1.2x108 (8cm) 1:2.5x108 (4cm) Trappist-1 e The e planet is one of the most Earth like one know, well within the habitable zone, slightly smaller, and nearly the same density of our planet. The habitability of the red dwarf planets is cuestionable, mostly because of the tidal lock. The always-day hemisphere may be too hot, while the night one may be too cold. It could be that in the border line between the hemispheres, the air is warm enough to sustain Earth like conditions. Also if the atmosphere is thick enough, it could distribute more efficiently the air temperature. • Type: Planet. • Orbit: Trappist-1. • Distance to the Sun: 39.6 ly. • Orbital period: 6.099 d • Composition: Silicate rock. • Density: ~5.6 g/cm3. • Dimensions: ~11500km • Model scale: 1:1.2x108 (9cm) 1:2.5x108 (4cm) Trappist-1 f Trappist-1 f is about the size of Earth, but two third its mass. This low density is consistent with a water rich world (20% of its mass, contrast to the 0.02% of Earth's mass). This means that it is probably an ocean world, with a combination of water vapor atmosphere, liquid ocean and large ice blocks. • Type: Planet. • Orbit: Trappist-1. • Distance to the Sun: 39.6 ly. • Orbital period: 9.2 d • Composition: Silicate rock. Ocean world?. • Density: ~4.5 g/cm3. • Dimensions: ~13300 km • Model scale: 1:1.2x108 (11cm) 1:2.5x108 (5cm) Trappist-1 g Like other members of this system, Trappist-1 g appear to be composed of high amounts of water, in this case in form of ices. It is the biggest planet of the system, although most of them are similar in size. Because of their proximity, the planet of the Trappist-1 system are locked in an orbital resonance, similar to the moons of Jupiter, Io, Europa and Ganymede. • Type: Planet. • Orbit: Trappist-1. • Distance to the Sun: 39.6 ly. • Orbital period: 12.354 d • Composition: Silicate rock, and ice. • Density: ~4 g/cm3. • Dimensions: ~14500 km • Model scale: 1:1.2x108 (12cm) 1:2.5x108 (6cm) Trappist-1 h The h planet is the outermost one of the Trappist-1 system. It has about the same size and density of that of Mars, but is though to be composed 5% of water ice. It is unlikely that this planetary system has many bigger planets in larger orbits, because their effects on the star light must be detectable, as well as their transits in front of the star. • Type: Planet. • Orbit: Trappist-1. • Distance to the Sun: 39.6 ly. • Orbital period: 18.767 d • Composition: Silicate rock, and ice. • Density: ~4 g/cm3. • Dimensions: ~10000 km • Model scale: 1:1.2x108 (8cm) 1:2.5x108 (4cm) (55 Cancri e) Janssen 55 Cancri was one of the firsts star system to be discovered with more than two exoplanets. It is binary star system of a K type star (55 Cancri A), which has all the 5 known planets of the system, and a smaller M type red dwarf (55 Cancri B). Only the e planet of this system, nicknamed Janssen, has a known radius, because its proximity to the star makes possible the transits. It could be a carbon planet, a planet composed of silicate rock and iron core like Earth, but with a thick crust and mantle of carbonaceous material. This hypothetical type of planet may have layers of graphite and diamond below its surface, and high amount of hydrocarbons like methane in the surface, as well as carbon monoxide, dioxide, and smog in the atmosphere. In the Solar system there aren't large carbon based bodies, only the C-type asteroids (like 253 Mathilde) are mainly composed of carbonaceous material.
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  • A Spitzer Space Telescope Program by Jesica Lynn Trucks

    A Spitzer Space Telescope Program by Jesica Lynn Trucks

    A Dissertation entitled A Variability Study of Y Dwarfs: A Spitzer Space Telescope Program by Jesica Lynn Trucks Submitted to the Graduate Faculty as partial fulfillment of the requirements for the Doctor of Philosophy Degree in Physics with concentration in Astrophysics Dr. Michael Cushing, Committee Chair Dr. S. Thomas Megeath, Committee Member Dr. Rupali Chandar, Committee Member Dr. Richard Irving, Committee Member Dr. Stanimir Metchev, Committee Member Dr. Cyndee Gruden, Interim Dean College of Graduate Studies The University of Toledo August 2019 Copyright 2019, Jesica Lynn Trucks This document is copyrighted material. Under copyright law, no parts of this document may be reproduced without the expressed permission of the author. An Abstract of A Variability Study of Y Dwarfs: A Spitzer Space Telescope Program by Jesica Lynn Trucks Submitted to the Graduate Faculty as partial fulfillment of the requirements for the Doctor of Philosophy Degree in Physics with concentration in Astrophysics The University of Toledo August 2019 I present the results of a search for variability in 14 Y dwarfs consisting 2 epochs of observations, each taken with Spitzer for 12 hours at [3.6] immediately followed by 12 hours at [4.5], separated by 122{464 days and found that Y dwarfs are variable. We used not only periodograms to characterize the variability but we also utilized Bayesian analysis. We found that using different methods to detect variability gives different answers making survey comparisons difficult. We determined the variability fraction of Y dwarfs to be between 37% and 74%. While the mid-infrared light curves of Y dwarfs are generally stable on time scales of months, we have encountered a few that vary dramatically on those time scales.