Planets in different environments
... (Cochran et al. 2002, Guenther 2005). Then a planet of eTau found (Sato et al. 2007), and a hot Jupiter (Quinn et al. 2013). M67 (3.2-5 Gyrs, 1400 Msun): 3 planet found --> Frequency of hot Jupiters: 2+3.01.5 %, consistent with solar neighbourhood (Brucalassi et al. 2014) NGC6791(3.5 Gyrs), NGC ...
... (Cochran et al. 2002, Guenther 2005). Then a planet of eTau found (Sato et al. 2007), and a hot Jupiter (Quinn et al. 2013). M67 (3.2-5 Gyrs, 1400 Msun): 3 planet found --> Frequency of hot Jupiters: 2+3.01.5 %, consistent with solar neighbourhood (Brucalassi et al. 2014) NGC6791(3.5 Gyrs), NGC ...
Document
... a planet between Mars and Jupiter were broken up, thrown into the Sun, or ejected from the solar system. • This was due to the gravitational influence of massive Jupiter which formed first. • It induced high, destructive, collision speeds • This arrested the accumulation process ...
... a planet between Mars and Jupiter were broken up, thrown into the Sun, or ejected from the solar system. • This was due to the gravitational influence of massive Jupiter which formed first. • It induced high, destructive, collision speeds • This arrested the accumulation process ...
Pluto_Ceres_ASP
... (1) A planet is a celestial body that (a) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape1, and (b) is in orbit around a star, and is neither a star nor a satellite of a planet. (2) We distinguish between the ei ...
... (1) A planet is a celestial body that (a) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape1, and (b) is in orbit around a star, and is neither a star nor a satellite of a planet. (2) We distinguish between the ei ...
A report of the SEEDS Direct Imaging Survey
... □ SEEDS has explored the wide-orbit giant planets of the Solar system scale. As a systematic survey, SEEDS has been most successful in direct imaging of planets. □ From SEEDS, 3 direct imaging discovery of planets and boundary-mass-objects (GJ 504 b, κ And b, GJ 758 b) and 3 brown dwarfs detection i ...
... □ SEEDS has explored the wide-orbit giant planets of the Solar system scale. As a systematic survey, SEEDS has been most successful in direct imaging of planets. □ From SEEDS, 3 direct imaging discovery of planets and boundary-mass-objects (GJ 504 b, κ And b, GJ 758 b) and 3 brown dwarfs detection i ...
Observing Planetary Motion 15.3 Directions: Following the
... STARS WOBBLE There are many stars like our Sun. Some of these other stars also may have planets that orbit them. Even though Earth-based astronomers may not have yet seen a planet orbiting another star, they know such orbiting planets exist. How do they know? Because when a planet orbits a star, it ...
... STARS WOBBLE There are many stars like our Sun. Some of these other stars also may have planets that orbit them. Even though Earth-based astronomers may not have yet seen a planet orbiting another star, they know such orbiting planets exist. How do they know? Because when a planet orbits a star, it ...
award
... What conclusion can be drawn from the fact that some planets with solid surfaces and satellites have impact craters? Collisions between Solar System bodies and planetesimals were common at one time. The young planets had softer surfaces. Volcanoes were very active in the early stages of planet forma ...
... What conclusion can be drawn from the fact that some planets with solid surfaces and satellites have impact craters? Collisions between Solar System bodies and planetesimals were common at one time. The young planets had softer surfaces. Volcanoes were very active in the early stages of planet forma ...
GEARS Workshop Monday - Georgia Southern University
... • Complete this exercise in groups of 2 to 3. • This is designed to be completed while you are discussing with other people. • This is not designed to be completed on your own. (despite the fact we keep assigning them as homework) ...
... • Complete this exercise in groups of 2 to 3. • This is designed to be completed while you are discussing with other people. • This is not designed to be completed on your own. (despite the fact we keep assigning them as homework) ...
Planetary System Formation, Extrasolar Planets, Life in the Universe
... snow line, in parts of the disk cool enough for ice to be present • Higher surface density -> more rapid formation of planets • In the outer Solar System, planets grew to ~20 MEarth while gas was still present, captured gas to form gas giants • In inner Solar System, no gas was captured • All circul ...
... snow line, in parts of the disk cool enough for ice to be present • Higher surface density -> more rapid formation of planets • In the outer Solar System, planets grew to ~20 MEarth while gas was still present, captured gas to form gas giants • In inner Solar System, no gas was captured • All circul ...
The Dynamics-Based Approach to Studying Terrestrial Exoplanets
... of which 239 are M dwarfs and only 21 are G dwarfs. Projecting these numbers by volume, we expect 10,000 M-dwarf stars within 35 pc. This estimate is consistent with the number of Mdwarfs in that volume identified by large proper motions and 2MASS photometry (Lepine & Shara 2005; Lepine 2005) but fo ...
... of which 239 are M dwarfs and only 21 are G dwarfs. Projecting these numbers by volume, we expect 10,000 M-dwarf stars within 35 pc. This estimate is consistent with the number of Mdwarfs in that volume identified by large proper motions and 2MASS photometry (Lepine & Shara 2005; Lepine 2005) but fo ...
chapter 8 Notes
... • The apparent motion of the planets, the stars, and the Sun is due to Earth’s rotation. This is the heliocentric model, or Suncentered model of the solar system. ...
... • The apparent motion of the planets, the stars, and the Sun is due to Earth’s rotation. This is the heliocentric model, or Suncentered model of the solar system. ...
Question 1
... • The apparent motion of the planets, the stars, and the Sun is due to Earth’s rotation. This is the heliocentric model, or Suncentered model of the solar system. ...
... • The apparent motion of the planets, the stars, and the Sun is due to Earth’s rotation. This is the heliocentric model, or Suncentered model of the solar system. ...
Kepler 186f - Forum Skylive
... M dwarfs are known to be highly active early in their life, often producing giant and frequent flares that could scorch planets nearby. The M dwarf stars also gravitationally interact with their planets, causing tides that heat the planet and often cause their rotations to be ‘tidally locked’, which ...
... M dwarfs are known to be highly active early in their life, often producing giant and frequent flares that could scorch planets nearby. The M dwarf stars also gravitationally interact with their planets, causing tides that heat the planet and often cause their rotations to be ‘tidally locked’, which ...
15_LectureOutline
... Kuiper-belt objects have been detected from Earth recently; a few are as large as, or larger than, Pluto, and their composition appears similar. ...
... Kuiper-belt objects have been detected from Earth recently; a few are as large as, or larger than, Pluto, and their composition appears similar. ...
Document
... Simulations have shown that the development from planetesimals to planets occurs in time-spans of several 10 million years (Wetherill 1990). In a time-dependent calculation by Wetherill (1986), the motion of 500 planetesimals in their orbit around the Sun was modeled (see Fig. 2.3). These initially ...
... Simulations have shown that the development from planetesimals to planets occurs in time-spans of several 10 million years (Wetherill 1990). In a time-dependent calculation by Wetherill (1986), the motion of 500 planetesimals in their orbit around the Sun was modeled (see Fig. 2.3). These initially ...
Microlensing
... Milestones: A. An optimised planetary microlens follow-up network, including feedback from fully-automated real-time modelling. B. The first census of the cold planet population, involving planets of Neptune to super-Earth (few M⊕ to 20 M⊕) with host star separations around 2 AU. C. Under highly fav ...
... Milestones: A. An optimised planetary microlens follow-up network, including feedback from fully-automated real-time modelling. B. The first census of the cold planet population, involving planets of Neptune to super-Earth (few M⊕ to 20 M⊕) with host star separations around 2 AU. C. Under highly fav ...
Condensation of the Solar Nebula
... Accretion The process by which small ‘seeds’ grew into planets. • Near the Sun, where temperature is high, only metals and rocks can condense. The small pieces of metals and rocks (the planetesimals) collide and stick together to form larger piece of planetesimals. • Small pieces of planetesimals ca ...
... Accretion The process by which small ‘seeds’ grew into planets. • Near the Sun, where temperature is high, only metals and rocks can condense. The small pieces of metals and rocks (the planetesimals) collide and stick together to form larger piece of planetesimals. • Small pieces of planetesimals ca ...
3 The Outer Planets
... beyond Uranus before the planet was observed. Uranus did not move in its orbit exactly as they expected. The force of gravity due to another large object was affecting it. Using predictions of its effect on Uranus, astronomers discovered Neptune in 1846. Neptune is the fourth largest planet in the s ...
... beyond Uranus before the planet was observed. Uranus did not move in its orbit exactly as they expected. The force of gravity due to another large object was affecting it. Using predictions of its effect on Uranus, astronomers discovered Neptune in 1846. Neptune is the fourth largest planet in the s ...
part2
... 1. Planetesimals collide and stick together to form protoplanets because a) of their mutually attractive gravitation. b) they are weakly charged and can attract each other. c) chemical bonds hold them together if they happen to collide. d) Both b and c 2. The terrestrial planets formed close to the ...
... 1. Planetesimals collide and stick together to form protoplanets because a) of their mutually attractive gravitation. b) they are weakly charged and can attract each other. c) chemical bonds hold them together if they happen to collide. d) Both b and c 2. The terrestrial planets formed close to the ...
Document
... more massive (more on this later in the course) • < 1% of the M dwarfs stars (low mass) have giant planets, but may have a large population of neptune-mass planets → low mass stars have low mass planets, high mass stars have more planets of higher mass → planet formation may be a steep function of s ...
... more massive (more on this later in the course) • < 1% of the M dwarfs stars (low mass) have giant planets, but may have a large population of neptune-mass planets → low mass stars have low mass planets, high mass stars have more planets of higher mass → planet formation may be a steep function of s ...
planet
... • The spacecraft missed its intended 140 150 km altitude above Mars during orbit insertion, instead entering the Martian atmosphere at about 57 km. ...
... • The spacecraft missed its intended 140 150 km altitude above Mars during orbit insertion, instead entering the Martian atmosphere at about 57 km. ...
No Slide Title
... A brief history of extra-solar planets • In the 16th century the Italian philosopher Giordano Bruno said that the fixed stars are really suns like our own, with planets going round them • 1991 Radio astronomers Alex Wolszczan & Dale Frail discovered planets around a pulsar PSR1257+12 – Variations i ...
... A brief history of extra-solar planets • In the 16th century the Italian philosopher Giordano Bruno said that the fixed stars are really suns like our own, with planets going round them • 1991 Radio astronomers Alex Wolszczan & Dale Frail discovered planets around a pulsar PSR1257+12 – Variations i ...
How to Become a Planet Hunter-Careers in
... An interferometer combines the light from two or more small telescopes (Mersenne) to yield the angular resolution of a much larger telescope. Interferometer Resolution Interferometer ...
... An interferometer combines the light from two or more small telescopes (Mersenne) to yield the angular resolution of a much larger telescope. Interferometer Resolution Interferometer ...
How Stars and Planets are Born
... • Terrestrial vs. Jovian Planets • Outer solar system is cooler • Large, less dense planets form from H ...
... • Terrestrial vs. Jovian Planets • Outer solar system is cooler • Large, less dense planets form from H ...
Planet
A planet (from Ancient Greek ἀστήρ πλανήτης (astēr planētēs), or πλάνης ἀστήρ (plánēs astēr), meaning ""wandering star"") is an astronomical object orbiting a star, brown dwarf, or stellar remnant that is massive enough to be rounded by its own gravity, is not massive enough to cause thermonuclear fusion, and has cleared its neighbouring region of planetesimals.The term planet is ancient, with ties to history, science, mythology, and religion. Several planets in the Solar System can be seen with the naked eye. These were regarded by many early cultures as divine, or as emissaries of deities. As scientific knowledge advanced, human perception of the planets changed, incorporating a number of disparate objects. In 2006, the International Astronomical Union (IAU) officially adopted a resolution defining planets within the Solar System. This definition is controversial because it excludes many objects of planetary mass based on where or what they orbit. Although eight of the planetary bodies discovered before 1950 remain ""planets"" under the modern definition, some celestial bodies, such as Ceres, Pallas, Juno, Vesta (each an object in the solar asteroid belt), and Pluto (the first trans-Neptunian object discovered), that were once considered planets by the scientific community are no longer viewed as such.The planets were thought by Ptolemy to orbit Earth in deferent and epicycle motions. Although the idea that the planets orbited the Sun had been suggested many times, it was not until the 17th century that this view was supported by evidence from the first telescopic astronomical observations, performed by Galileo Galilei. By careful analysis of the observation data, Johannes Kepler found the planets' orbits were not circular but elliptical. As observational tools improved, astronomers saw that, like Earth, the planets rotated around tilted axes, and some shared such features as ice caps and seasons. Since the dawn of the Space Age, close observation by space probes has found that Earth and the other planets share characteristics such as volcanism, hurricanes, tectonics, and even hydrology.Planets are generally divided into two main types: large low-density giant planets, and smaller rocky terrestrials. Under IAU definitions, there are eight planets in the Solar System. In order of increasing distance from the Sun, they are the four terrestrials, Mercury, Venus, Earth, and Mars, then the four giant planets, Jupiter, Saturn, Uranus, and Neptune. Six of the planets are orbited by one or more natural satellites.More than a thousand planets around other stars (""extrasolar planets"" or ""exoplanets"") have been discovered in the Milky Way: as of 1 October 2015, 1968 known extrasolar planets in 1248 planetary systems (including 490 multiple planetary systems), ranging in size from just above the size of the Moon to gas giants about twice as large as Jupiter. On December 20, 2011, the Kepler Space Telescope team reported the discovery of the first Earth-sized extrasolar planets, Kepler-20e and Kepler-20f, orbiting a Sun-like star, Kepler-20. A 2012 study, analyzing gravitational microlensing data, estimates an average of at least 1.6 bound planets for every star in the Milky Way.Around one in five Sun-like stars is thought to have an Earth-sized planet in its habitable zone.