Planets around Other Stars - Sierra College Astronomy Home Page
... Throughout history the meaning of planets has changed Defining a planet is tricky and was done for our solar system just recently ...
... Throughout history the meaning of planets has changed Defining a planet is tricky and was done for our solar system just recently ...
Sample Schedule 2012
... have solid surfaces and thin or no atmospheres have varied atmospheres ranging from no atmosphere (Mercury) to a thin atmosphere consisting mainly of nitrogen and oxygen (Earth) spin slowly compared to the outer planets have no or few moons (Earth has 1 moon, Mars – 2) have no rings orbiti ...
... have solid surfaces and thin or no atmospheres have varied atmospheres ranging from no atmosphere (Mercury) to a thin atmosphere consisting mainly of nitrogen and oxygen (Earth) spin slowly compared to the outer planets have no or few moons (Earth has 1 moon, Mars – 2) have no rings orbiti ...
Astro 27 Solar System Formation and ExoPlanets Slide Show
... active area of research • Inner planets – formed by rocky material inside “frost line” • Outer planets – formed by hydrogen compound ices as “seeds”, and since H is most of the proto-solar system, these planets are large • Beyond, is Kuiper Belt of 10’s of thousands of giant ice cores • 100x further ...
... active area of research • Inner planets – formed by rocky material inside “frost line” • Outer planets – formed by hydrogen compound ices as “seeds”, and since H is most of the proto-solar system, these planets are large • Beyond, is Kuiper Belt of 10’s of thousands of giant ice cores • 100x further ...
![planetinvasionwebquest[1]. - teachingandlearningwithtech](http://s1.studyres.com/store/data/008592376_1-55293b127f13c43ac60fb598df65ad5f-300x300.png)
planetinvasionwebquest[1]. - teachingandlearningwithtech
... What is the size of the planet? What is the length of days and years? Find 3 interesting facts about Jupiter. Find at least 1 similarity and one 1 difference between Jupiter and Earth. http://starchild.gsfc.nasa.gov/docs/StarChild/solar_system_level1/j upiter.html http://www.enchantedlearning.com/su ...
... What is the size of the planet? What is the length of days and years? Find 3 interesting facts about Jupiter. Find at least 1 similarity and one 1 difference between Jupiter and Earth. http://starchild.gsfc.nasa.gov/docs/StarChild/solar_system_level1/j upiter.html http://www.enchantedlearning.com/su ...
paper
... (iv) the stellar density (assuming the orbital period is known). This last quantity can be used with other measured stellar quantities to deduce, via stellar model ling, the mass of the star, which leads finally to the stellar and planet radii (Gillon et al., 2007; 2009). So far, we have gathered ...
... (iv) the stellar density (assuming the orbital period is known). This last quantity can be used with other measured stellar quantities to deduce, via stellar model ling, the mass of the star, which leads finally to the stellar and planet radii (Gillon et al., 2007; 2009). So far, we have gathered ...
What is it? - Carmenes - Calar Alto Observatory
... exoplanets is getting lower and lower. However, in spite of the efforts of astronomers, we have not been able to detect yet the first exoearth: an exoplanet with roughly the same mass as the Earth (M ~ 0.5-2.0 Mearth). A habitable planet is understood as one that sustains liquid water (and, possibly ...
... exoplanets is getting lower and lower. However, in spite of the efforts of astronomers, we have not been able to detect yet the first exoearth: an exoplanet with roughly the same mass as the Earth (M ~ 0.5-2.0 Mearth). A habitable planet is understood as one that sustains liquid water (and, possibly ...
TRAPPIST: TRAnsiting Planets and PlanetesImals Small Telescope
... (iv) the stellar density (assuming the orbital period is known). This last quantity can be used with other measured stellar quantities to deduce, via stellar model ling, the mass of the star, which leads finally to the stellar and planet radii (Gillon et al., 2007; 2009). So far, we have gathered ...
... (iv) the stellar density (assuming the orbital period is known). This last quantity can be used with other measured stellar quantities to deduce, via stellar model ling, the mass of the star, which leads finally to the stellar and planet radii (Gillon et al., 2007; 2009). So far, we have gathered ...
Chapter 29
... The Planets • The nine planets of our solar system can be grouped into two main categories according to their basic properties. – The terrestrial planets are the inner four planets of Mercury, Venus, Earth, and Mars that are close to the size of Earth and have solid, rocky surfaces. – The Jovian pla ...
... The Planets • The nine planets of our solar system can be grouped into two main categories according to their basic properties. – The terrestrial planets are the inner four planets of Mercury, Venus, Earth, and Mars that are close to the size of Earth and have solid, rocky surfaces. – The Jovian pla ...
Life on hot Jupiters
... • Until now, the only planets for which spectra were available belonged in our own solar system. The planets in the Spitzer studies orbit stars that are so far away, they are too faint to be seen with the naked eye. That means both planets are at least about a million times farther away from us than ...
... • Until now, the only planets for which spectra were available belonged in our own solar system. The planets in the Spitzer studies orbit stars that are so far away, they are too faint to be seen with the naked eye. That means both planets are at least about a million times farther away from us than ...
how to bring two neptune mass planets on the same orbit
... We present the results of three simulations performed using the code FARGO-2D1D (code publicly available at http://fargo.in2p3.fr/). The initial density profile of the disk is : Σ0 = 3430(r/10AU)−2.168 kg.m−2 . Jupiter, Saturn, Neptune and Uranus start on circular orbits at 5.45, 8.18, 11.5 and 14.2 ...
... We present the results of three simulations performed using the code FARGO-2D1D (code publicly available at http://fargo.in2p3.fr/). The initial density profile of the disk is : Σ0 = 3430(r/10AU)−2.168 kg.m−2 . Jupiter, Saturn, Neptune and Uranus start on circular orbits at 5.45, 8.18, 11.5 and 14.2 ...
Chapter 8 Jovian Planet Systems
... So they got started first and were therefore able to capture H and He longer Uranus and Neptune formed farther out, in a thinner part of the nebula So they didn’t get started as soon, and this limited their growth It also made their composition different from Jupiter and Saturn, with less H and He c ...
... So they got started first and were therefore able to capture H and He longer Uranus and Neptune formed farther out, in a thinner part of the nebula So they didn’t get started as soon, and this limited their growth It also made their composition different from Jupiter and Saturn, with less H and He c ...
New Worlds on the Horizon: Earth-Sized Planets Close to Other
... instruments, on the ground and in space, will discover still smaller planets. These worlds will also be on close orbits, many will be much hotter than Earth, and some may have very different compositions. All will help us understand how planets form and the propensity for that process to yield plane ...
... instruments, on the ground and in space, will discover still smaller planets. These worlds will also be on close orbits, many will be much hotter than Earth, and some may have very different compositions. All will help us understand how planets form and the propensity for that process to yield plane ...
3.4, 3.5, 3.6 Notes
... • A dwarf planet is a celestial body that orbits the sun and is round because of its own gravity. • A dwarf planet does not have the mass to have cleared other bodies out of its orbit around the sun. ...
... • A dwarf planet is a celestial body that orbits the sun and is round because of its own gravity. • A dwarf planet does not have the mass to have cleared other bodies out of its orbit around the sun. ...
CH10.AST1001.F16.EDS
... • Close gravitational encounters between two massive planets can eject one planet while flinging the other into a highly elliptical orbit. • Multiple close encounters with smaller planetesimals can also cause inward migration. • Resonances may also contribute. ...
... • Close gravitational encounters between two massive planets can eject one planet while flinging the other into a highly elliptical orbit. • Multiple close encounters with smaller planetesimals can also cause inward migration. • Resonances may also contribute. ...
A low mass for Mars from Jupiter`s early gas
... Scattering by Jupiter initially empties but then repopulates the asteroid belt, with inner-belt bodies originating between 1 and 3 AU and outer-belt bodies originating between and beyond the giant planets. This explains the significant compositional differences across the asteroid belt. The key aspe ...
... Scattering by Jupiter initially empties but then repopulates the asteroid belt, with inner-belt bodies originating between 1 and 3 AU and outer-belt bodies originating between and beyond the giant planets. This explains the significant compositional differences across the asteroid belt. The key aspe ...
A low mass for Mars from Jupiter`s early gas-driven - ICE-CSIC
... Scattering by Jupiter initially empties but then repopulates the asteroid belt, with inner-belt bodies originating between 1 and 3 AU and outer-belt bodies originating between and beyond the giant planets. This explains the significant compositional differences across the asteroid belt. The key aspe ...
... Scattering by Jupiter initially empties but then repopulates the asteroid belt, with inner-belt bodies originating between 1 and 3 AU and outer-belt bodies originating between and beyond the giant planets. This explains the significant compositional differences across the asteroid belt. The key aspe ...
Return Visit Optimization for Planet Finding
... The best chance for repeating a detection will come either one or one-half orbital periods after an initial detection. Since the observed illumination of a planet depends on the orientation of the system, there is no guarantee that the contrast between planet and star will be greater or less at any ...
... The best chance for repeating a detection will come either one or one-half orbital periods after an initial detection. Since the observed illumination of a planet depends on the orientation of the system, there is no guarantee that the contrast between planet and star will be greater or less at any ...
Jovian Planet Systems
... Uranus and Neptune formed farther out, in a thinner part of the nebula So they didn’t get started as soon, and this limited their growth It also made their composition different from Jupiter and Saturn, with less H and He compared to H-compounds, rock, and metal • But there is another aspect of the ...
... Uranus and Neptune formed farther out, in a thinner part of the nebula So they didn’t get started as soon, and this limited their growth It also made their composition different from Jupiter and Saturn, with less H and He compared to H-compounds, rock, and metal • But there is another aspect of the ...
ph507lecnote07
... Debris disks are found around stars generally older than 10 Myr, with no signs of gas accretion (as judged from the absence of emission lines or UV excess) . In the absence of gas drag, a 10 m sized dust grain from the primordial, proto–planetary nebula cannot survive longer than 1 Myr within 10 AU ...
... Debris disks are found around stars generally older than 10 Myr, with no signs of gas accretion (as judged from the absence of emission lines or UV excess) . In the absence of gas drag, a 10 m sized dust grain from the primordial, proto–planetary nebula cannot survive longer than 1 Myr within 10 AU ...
Planets of Our, and Other, Solar Systems
... active area of research • Inner planets – formed by rocky material inside “frost line” • Outer planets – formed by hydrogen compound ices as “seeds”, and since H is most of the proto-solar system, these planets are large • Beyond, is Kuiper Belt of 10’s of thousands of giant ice cores • 100x further ...
... active area of research • Inner planets – formed by rocky material inside “frost line” • Outer planets – formed by hydrogen compound ices as “seeds”, and since H is most of the proto-solar system, these planets are large • Beyond, is Kuiper Belt of 10’s of thousands of giant ice cores • 100x further ...
Lecture #33: Solar System Origin I The Main Point What is a
... ordinary chondrite meteorites ALL have ages of approximately 4.6 billion years. • Tiny fractions of some very primitive meteorites and cosmic dust particles have ages even slightly older than this. • The oldest rocks from the lunar highlands are about 4.4 billion years old. Astro 102/104 ...
... ordinary chondrite meteorites ALL have ages of approximately 4.6 billion years. • Tiny fractions of some very primitive meteorites and cosmic dust particles have ages even slightly older than this. • The oldest rocks from the lunar highlands are about 4.4 billion years old. Astro 102/104 ...
fourth grade - Math/Science Nucleus
... by planetary scientists. It is difficult to tell which books give you the best up-to-date information on the planets. The aim of this activity is to help students learn that scientific information is by definition provisional. It is always subject to change as new data is gathered, or as new interpr ...
... by planetary scientists. It is difficult to tell which books give you the best up-to-date information on the planets. The aim of this activity is to help students learn that scientific information is by definition provisional. It is always subject to change as new data is gathered, or as new interpr ...
Dwarf planet
A dwarf planet is a planetary-mass object that is neither a planet nor a natural satellite. That is, it is in direct orbit of the Sun, and is massive enough for its shape to be in hydrostatic equilibrium under its own gravity, but has not cleared the neighborhood around its orbit.The term dwarf planet was adopted in 2006 as part of a three-way categorization of bodies orbiting the Sun, brought about by an increase in discoveries of objects farther away from the Sun than Neptune that rivaled Pluto in size, and finally precipitated by the discovery of an even more massive object, Eris. The exclusion of dwarf planets from the roster of planets by the IAU has been both praised and criticized; it was said to be the ""right decision"" by astronomer Mike Brown, who discovered Eris and other new dwarf planets, but has been rejected by Alan Stern, who had coined the term dwarf planet in 1990.The International Astronomical Union (IAU) currently recognizes five dwarf planets: Ceres, Pluto, Haumea, Makemake, and Eris. Brown criticizes this official recognition: ""A reasonable person might think that this means that there are five known objects in the solar system which fit the IAU definition of dwarf planet, but this reasonable person would be nowhere close to correct.""It is suspected that another hundred or so known objects in the Solar System are dwarf planets. Estimates are that up to 200 dwarf planets may be found when the entire region known as the Kuiper belt is explored, and that the number may exceed 10,000 when objects scattered outside the Kuiper belt are considered. Individual astronomers recognize several of these, and in August 2011 Mike Brown published a list of 390 candidate objects, ranging from ""nearly certain"" to ""possible"" dwarf planets. Brown currently identifies eleven known objects – the five accepted by the IAU plus 2007 OR10, Quaoar, Sedna, Orcus, 2002 MS4 and Salacia – as ""virtually certain"", with another dozen highly likely. Stern states that there are more than a dozen known dwarf planets.However, only two of these bodies, Ceres and Pluto, have been observed in enough detail to demonstrate that they actually fit the IAU's definition. The IAU accepted Eris as a dwarf planet because it is more massive than Pluto. They subsequently decided that unnamed trans-Neptunian objects with an absolute magnitude brighter than +1 (and hence a diameter of ≥838 km assuming a geometric albedo of ≤1) are to be named under the assumption that they are dwarf planets. The only two such objects known at the time, Makemake and Haumea, went through this naming procedure and were declared to be dwarf planets. The question of whether other likely objects are dwarf planets has never been addressed by the IAU. The classification of bodies in other planetary systems with the characteristics of dwarf planets has not been addressed.