PLANETS
... The planet with the lowest eccentricity is Venus with 0.007. Unless there is some gravitational tugging (such as with the Galilean Satellites) that keeps an orbit eccentric, orbits will usually circularize with time. About 10% of the planets found so far have an eccentricity of nearly 0. About 15% h ...
... The planet with the lowest eccentricity is Venus with 0.007. Unless there is some gravitational tugging (such as with the Galilean Satellites) that keeps an orbit eccentric, orbits will usually circularize with time. About 10% of the planets found so far have an eccentricity of nearly 0. About 15% h ...
Solar System
... Jupiter- largest planet, has Great Red Spot, has twice as much mass as all other planets put together. Mars- the red planet, most like the Earth, has two moons called Deimos and Phobos. Mercury- closest to the Sun, has craters, has no atmosphere Neptune- has an icy moon called Triton, bluish in colo ...
... Jupiter- largest planet, has Great Red Spot, has twice as much mass as all other planets put together. Mars- the red planet, most like the Earth, has two moons called Deimos and Phobos. Mercury- closest to the Sun, has craters, has no atmosphere Neptune- has an icy moon called Triton, bluish in colo ...
uc6ss. - Math/Science Nucleus
... The Sun is a star. A self-luminous sphere of gas and plasma that is held together by its own gravity, and energized by nuclear reactions in its interior. The Sun has a four part structure. The outermost layer is the corona, the Sun’s outer atmosphere. This is a zone of super hot (temperatures vary, ...
... The Sun is a star. A self-luminous sphere of gas and plasma that is held together by its own gravity, and energized by nuclear reactions in its interior. The Sun has a four part structure. The outermost layer is the corona, the Sun’s outer atmosphere. This is a zone of super hot (temperatures vary, ...
Universe and Solar System
... Role: You are a member of your 6th grade class, which is helping your school compete for a hosting the President for a nationally televised address on space. Audience: The selection team for the President’s visit to a middle school, including educators and NASA scientists. Situation: The first space ...
... Role: You are a member of your 6th grade class, which is helping your school compete for a hosting the President for a nationally televised address on space. Audience: The selection team for the President’s visit to a middle school, including educators and NASA scientists. Situation: The first space ...
Astronomy lab: Planets
... • On the FIND tab, click on the boxes to the right of each planet. • On the VIEWING OPTIONs tab shut off all objects but the planets. • Select and center the sun, zoom in until Saturn's orbit fills the screen, rotate the image until Earth is below the sun. Print it out to the printer in rm. 231, 232 ...
... • On the FIND tab, click on the boxes to the right of each planet. • On the VIEWING OPTIONs tab shut off all objects but the planets. • Select and center the sun, zoom in until Saturn's orbit fills the screen, rotate the image until Earth is below the sun. Print it out to the printer in rm. 231, 232 ...
Why is it so difficult to detect planets around other stars? Planet
... the Sun with spectral lines that are slightly redshifted then slightly blueshifted with a repeating period of 16 months—what could you ...
... the Sun with spectral lines that are slightly redshifted then slightly blueshifted with a repeating period of 16 months—what could you ...
File
... • Earth is the third planet from the Sun. • Earth is the only body in our solar system known to have life on it. • Earth’s atmosphere affects the climate, shields the surface from harmful radiation, and burns up most meteoroids before they strike the surface. ...
... • Earth is the third planet from the Sun. • Earth is the only body in our solar system known to have life on it. • Earth’s atmosphere affects the climate, shields the surface from harmful radiation, and burns up most meteoroids before they strike the surface. ...
Document
... ratio of Type I & II migration may be less than previously thought (Winn et al. 2010) one cannot distinguish between p-p scattering and Kozai migration by spin-orbit misalignments or eccentricities alone Need to search for counterparts of migration processes very long term radial velocity me ...
... ratio of Type I & II migration may be less than previously thought (Winn et al. 2010) one cannot distinguish between p-p scattering and Kozai migration by spin-orbit misalignments or eccentricities alone Need to search for counterparts of migration processes very long term radial velocity me ...
Planets
... This idea is named the Nebular Hypothesis. It was first presented by the German philosopher Immanuel Kant in the late 1700’s. Such clouds have been observed around stars other than our sun (e.g., Beta Pictoris) ...
... This idea is named the Nebular Hypothesis. It was first presented by the German philosopher Immanuel Kant in the late 1700’s. Such clouds have been observed around stars other than our sun (e.g., Beta Pictoris) ...
tremaine_stanford
... it is unlikely (2-¾) that any planets will be ejected or collide before the Sun dies most of the solar system is “full”, and it is likely that planets have been lost from the solar system in the past ...
... it is unlikely (2-¾) that any planets will be ejected or collide before the Sun dies most of the solar system is “full”, and it is likely that planets have been lost from the solar system in the past ...
1 1. The Solar System
... The relative sizes of the planets One way to help visualize the relative sizes in the solar system is to imagine a model in which it is reduced in size by a factor of a billion (109). Then the Earth is about 1.3 cm in diameter (the size of a grape). The Moon orbits about a foot (~30.5 cm) away. The ...
... The relative sizes of the planets One way to help visualize the relative sizes in the solar system is to imagine a model in which it is reduced in size by a factor of a billion (109). Then the Earth is about 1.3 cm in diameter (the size of a grape). The Moon orbits about a foot (~30.5 cm) away. The ...
Dynamical simulations of the HR8799 planetary
... et al. 2005; Morbidelli & Levison 2006), but the basic scenario is that the four outer planets formed in a significantly more compact configuration than they are currently found. Indeed, some of the model solutions proposed invoke a system in which the initial planetary order was Jupiter, Neptune, Ura ...
... et al. 2005; Morbidelli & Levison 2006), but the basic scenario is that the four outer planets formed in a significantly more compact configuration than they are currently found. Indeed, some of the model solutions proposed invoke a system in which the initial planetary order was Jupiter, Neptune, Ura ...
Planet Exploration http://www.kidsastronomy.com/solar_system.htm
... hydrogen, helium, methane 142,983 km 317 x Earth ● Largest planet ● Spins so fast that it is fat in middle, its shape is ...
... hydrogen, helium, methane 142,983 km 317 x Earth ● Largest planet ● Spins so fast that it is fat in middle, its shape is ...
lec01_26sep2011
... heat, the solar atmosphere originally extended beyond the orbits of all the planets and that it progressively shrank to its present limits. This might have occurred through causes similar to those which made the famous star of 1572 suddenly shine so brightly for several months in the constellation o ...
... heat, the solar atmosphere originally extended beyond the orbits of all the planets and that it progressively shrank to its present limits. This might have occurred through causes similar to those which made the famous star of 1572 suddenly shine so brightly for several months in the constellation o ...
PowerPoint
... Exploring (Earth-like) Exoplanets • RV search for new low-mass planets • Transit follow-up studies • Gravitational microlensing follow-up studies • Direct imaging studies ...
... Exploring (Earth-like) Exoplanets • RV search for new low-mass planets • Transit follow-up studies • Gravitational microlensing follow-up studies • Direct imaging studies ...
Small Bodies of the Solar System Transcript
... We can determine the size of an asteroid by the time taken for it to eclipse the light of a background star if it moves in front, in what is known as an occultation. If its orbital parameters are known – how far away it is, how fast it’s moving – then the duration of the eclipse can allow you to est ...
... We can determine the size of an asteroid by the time taken for it to eclipse the light of a background star if it moves in front, in what is known as an occultation. If its orbital parameters are known – how far away it is, how fast it’s moving – then the duration of the eclipse can allow you to est ...
Solar system - Institute of Astronomy
... equatorial orbits is a mystery. Singer (2003) suggests a capture of a more massive asteroid which disintegrated, the largest fragments of which already fell onto Mars. ...
... equatorial orbits is a mystery. Singer (2003) suggests a capture of a more massive asteroid which disintegrated, the largest fragments of which already fell onto Mars. ...
6 Scale Model of the Solar System
... • the scaled locations of each of the planets in the Solar System; that is, you will determine the city along the highway (I-25) each planet will be located nearest to, and how far north or south of this city the planet will be located. If more than one planet is located within a given city, identif ...
... • the scaled locations of each of the planets in the Solar System; that is, you will determine the city along the highway (I-25) each planet will be located nearest to, and how far north or south of this city the planet will be located. If more than one planet is located within a given city, identif ...
- Europhysics News
... The huge diversity in the physical and orbital properties of exoplanets forces us to reconsider the model of planetary formation currently accepted for the solar system. This model is based upon the properties of planetary orbits, mostly coplanar, circular and concentric around the Sun. Following th ...
... The huge diversity in the physical and orbital properties of exoplanets forces us to reconsider the model of planetary formation currently accepted for the solar system. This model is based upon the properties of planetary orbits, mostly coplanar, circular and concentric around the Sun. Following th ...
FCAT 2.0 Content Limits - Wonders of Science and Math
... a better sense of its size. This may enable us to come up with valuable questions about the solar system or the planets in it. These questions can also be used for "Exploration and Discovery" — to make observations, get inspiration, and determine what questions to ask. 8. Have students use a graphic ...
... a better sense of its size. This may enable us to come up with valuable questions about the solar system or the planets in it. These questions can also be used for "Exploration and Discovery" — to make observations, get inspiration, and determine what questions to ask. 8. Have students use a graphic ...
6 Scale Model of the Solar System
... • the scaled locations of each of the planets in the Solar System; that is, you will determine the city along the highway (I-25) each planet will be located nearest to, and how far north or south of this city the planet will be located. If more than one planet is located within a given city, identif ...
... • the scaled locations of each of the planets in the Solar System; that is, you will determine the city along the highway (I-25) each planet will be located nearest to, and how far north or south of this city the planet will be located. If more than one planet is located within a given city, identif ...
Lecture 1: Properties of the Solar System Properties of the Solar
... Large size, low density and in outer solar system: Jupiter, Saturn, Uranus, Neptune. ...
... Large size, low density and in outer solar system: Jupiter, Saturn, Uranus, Neptune. ...
Migrating Planets - Lunar and Planetary Laboratory
... the 2:1. Such orbits are ellipses with semimajor axes of 39.5 AU and 47.8 AU, respectively. (The length of the semimajor axis is equal to the object’s average distance from the sun.) More modest concentrations of transNeptunian bodies would be found at other resonances, such as the 5:3. The populati ...
... the 2:1. Such orbits are ellipses with semimajor axes of 39.5 AU and 47.8 AU, respectively. (The length of the semimajor axis is equal to the object’s average distance from the sun.) More modest concentrations of transNeptunian bodies would be found at other resonances, such as the 5:3. The populati ...
Interpretations of Solar System Phenomena according to the
... It is interesting to point out, and of no great surprise, that brown dwarf stars are also similar to the Sun and the gas giant planets in terms of the relative abundances of hydrogen and helium that are found in their atmospheres. According to standard stellar formation theory brown dwarfs coalesce ...
... It is interesting to point out, and of no great surprise, that brown dwarf stars are also similar to the Sun and the gas giant planets in terms of the relative abundances of hydrogen and helium that are found in their atmospheres. According to standard stellar formation theory brown dwarfs coalesce ...
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.