Periodic mass extinctions and the Planet X model reconsidered
... now been observed around some young stars. In this case the mass of Planet X could be lower, ∼ 1 M⊕ , since it need not have cleared the gap itself. This lower limit is based solely on the comet scattering dynamics. Other hybrid scenarios (Lykawka and Mukai, 2008) are also possible whereby Planet X ...
... now been observed around some young stars. In this case the mass of Planet X could be lower, ∼ 1 M⊕ , since it need not have cleared the gap itself. This lower limit is based solely on the comet scattering dynamics. Other hybrid scenarios (Lykawka and Mukai, 2008) are also possible whereby Planet X ...
Inner Planets Lab
... The inner four planets are called terrestrial planets. That means that they are like the earth in some ways. The terrestrial planets Mercury, Venus, Earth, Mars, and the earth's moon have similar compositions and densities. The term terrestrial can be misleading because each of the four has vastly d ...
... The inner four planets are called terrestrial planets. That means that they are like the earth in some ways. The terrestrial planets Mercury, Venus, Earth, Mars, and the earth's moon have similar compositions and densities. The term terrestrial can be misleading because each of the four has vastly d ...
pdf - Starchitect
... Creating Planets and Moons Opportunities to build planets come in specific windows during the life of the star. Giant worlds come first: these can’t support life, but they can help shield planets from asteroids and comets that could lead to extinction events. Moons come next, since they are often fo ...
... Creating Planets and Moons Opportunities to build planets come in specific windows during the life of the star. Giant worlds come first: these can’t support life, but they can help shield planets from asteroids and comets that could lead to extinction events. Moons come next, since they are often fo ...
Properties of the Planets - Onondaga Community College
... Neptune: Much like Uranus in appearance, size and compostion, although cluds can be seen throuogh the atmosphere. These most distant Jovian planets are the runts of the Jovian litter, yet they still occupy a volume more than that of 64 Earth’s. ...
... Neptune: Much like Uranus in appearance, size and compostion, although cluds can be seen throuogh the atmosphere. These most distant Jovian planets are the runts of the Jovian litter, yet they still occupy a volume more than that of 64 Earth’s. ...
Making the Cards - Teaching Made Practical
... able to survive on Earth because of its unique characteristics – an atmosphere that is breathable, liquid water, and temperatures that are not too hot or too cold. ...
... able to survive on Earth because of its unique characteristics – an atmosphere that is breathable, liquid water, and temperatures that are not too hot or too cold. ...
Scaling the Solar System
... 3. Take another one of the seven balls and divide it into seven. One of those is the MOON. 4. You can also do a distance scale with this model...but MARS is far! If you used 3lbs of dough for this model, the distance between EARTH and MARS would be 7 city blocks! ...
... 3. Take another one of the seven balls and divide it into seven. One of those is the MOON. 4. You can also do a distance scale with this model...but MARS is far! If you used 3lbs of dough for this model, the distance between EARTH and MARS would be 7 city blocks! ...
Objectives –
... a. Gas Giants are denser than rocky planets. b. Gas Giants have poisonous atmospheres. c. Gas Giants weigh less than rocky planets. 19. The sunlight that reaches Neptune is about ____________ times dimmer than Earth. (Enter a number) 20. This world was called a planet in the video, but since 2006 ha ...
... a. Gas Giants are denser than rocky planets. b. Gas Giants have poisonous atmospheres. c. Gas Giants weigh less than rocky planets. 19. The sunlight that reaches Neptune is about ____________ times dimmer than Earth. (Enter a number) 20. This world was called a planet in the video, but since 2006 ha ...
Astro 10-Lecture 13: Formation and Structure of the Solar
... 3. The giant planets had disks of their own so their moons orbit in their equatorial plane 4a. Because the inner solar system was hot, only rock and metal could condense which resulted in terrestrial planets 4b. The outer solar system was cold enough for ices to condense and for hydrogen gas to be c ...
... 3. The giant planets had disks of their own so their moons orbit in their equatorial plane 4a. Because the inner solar system was hot, only rock and metal could condense which resulted in terrestrial planets 4b. The outer solar system was cold enough for ices to condense and for hydrogen gas to be c ...
Class 1 and 2 lecture slides (Solar System Formation)
... – Since outer planets can accrete gas if large enough, the relative timescales of planetary growth and gas loss are important ...
... – Since outer planets can accrete gas if large enough, the relative timescales of planetary growth and gas loss are important ...
THE SOLAR SYSTEM
... the Sun at a rate of 108,000 kilometers (67,000 miles) per hour! Q: Do all the planets rotate and revolve at the same speed? A: No. Each planet rotates on its axis at a different speed and revolves around the Sun at a different rate as well. The time it takes a planet to circle the Sun is known as i ...
... the Sun at a rate of 108,000 kilometers (67,000 miles) per hour! Q: Do all the planets rotate and revolve at the same speed? A: No. Each planet rotates on its axis at a different speed and revolves around the Sun at a different rate as well. The time it takes a planet to circle the Sun is known as i ...
Page pour l`impression
... There is a resonance of order n/m, where n and m are two integers, if a planet makes n revolutions when the other one makes m revolutions. In Neptune's rings, the edge of the Adams ring is in a resonance 42:43 with the satellite Galatea. Resonances between the rotation motion of a body and its revol ...
... There is a resonance of order n/m, where n and m are two integers, if a planet makes n revolutions when the other one makes m revolutions. In Neptune's rings, the edge of the Adams ring is in a resonance 42:43 with the satellite Galatea. Resonances between the rotation motion of a body and its revol ...
Chapter_7
... • The moons of the outer planets probably formed from planetesimals orbiting the growing planets. • Once a body became massive enough that it’s gravitational force could draw in additional material, it became ringed with debris. • Moon formation in the outer planets is probably a scaled-down version ...
... • The moons of the outer planets probably formed from planetesimals orbiting the growing planets. • Once a body became massive enough that it’s gravitational force could draw in additional material, it became ringed with debris. • Moon formation in the outer planets is probably a scaled-down version ...
Understanding the Solar System
... “Introduction to the Solar System” sheet for students to follow along with; then explain to the students about the solar system (found on handout). Send out a letter to parents explaining what their children will learn in class this week (solar system) along with explaining the fifth day’s project. ...
... “Introduction to the Solar System” sheet for students to follow along with; then explain to the students about the solar system (found on handout). Send out a letter to parents explaining what their children will learn in class this week (solar system) along with explaining the fifth day’s project. ...
ph709-15-testrevision
... of planetary radii. SELECTION: Of course, while planets close to their parent stars will preferentially be found, due to their shorter orbital periods and greater likelihood to transit, planetary transits will be detected at all orbital separations. CONFIRMATION: In general, the detection of three s ...
... of planetary radii. SELECTION: Of course, while planets close to their parent stars will preferentially be found, due to their shorter orbital periods and greater likelihood to transit, planetary transits will be detected at all orbital separations. CONFIRMATION: In general, the detection of three s ...
Asteroids,Comets, Meteor ppt.
... • 150,000 in catalogs, and probably over a million with diameter >1 km. • Small asteroids are more common than large asteroids. • All the asteroids in the solar system wouldn’t add up to even a small terrestrial planet. ...
... • 150,000 in catalogs, and probably over a million with diameter >1 km. • Small asteroids are more common than large asteroids. • All the asteroids in the solar system wouldn’t add up to even a small terrestrial planet. ...
The Kuiper Belt
... Sedna has been estimated to have more than half the diameter of Pluto and may be larger than any other planetary body found since Pluto -- at 730 to 1,470 miles or 1,180 to 2,360 kilometers (km) across, compared to Pluto's diameter of around 1,440 miles or 2,320 km. ...
... Sedna has been estimated to have more than half the diameter of Pluto and may be larger than any other planetary body found since Pluto -- at 730 to 1,470 miles or 1,180 to 2,360 kilometers (km) across, compared to Pluto's diameter of around 1,440 miles or 2,320 km. ...
Asteroids,Comets, Meteor ppt.
... • 150,000 in catalogs, and probably over a million with diameter >1 km. • Small asteroids are more common than large asteroids. • All the asteroids in the solar system wouldn’t add up to even a small terrestrial planet. ...
... • 150,000 in catalogs, and probably over a million with diameter >1 km. • Small asteroids are more common than large asteroids. • All the asteroids in the solar system wouldn’t add up to even a small terrestrial planet. ...
An Earth-sized Planet in the Habitable Zone of a
... The high coplanarity of the planets’ orbits (given by the fact that they all transit the star) suggest that they formed from a protoplanetary disk. The leading theories for the growth of planets include in-situ accretion of local material in a disk (26, 27), collisional growth of inwardmigrating pla ...
... The high coplanarity of the planets’ orbits (given by the fact that they all transit the star) suggest that they formed from a protoplanetary disk. The leading theories for the growth of planets include in-situ accretion of local material in a disk (26, 27), collisional growth of inwardmigrating pla ...
Instructional Design 1
... same methods, we can expand their knowledge of not only science concepts but technology knowledge as well The progressive philosophy suggests that the curriculum be interdisciplinary and the teacher needs to guide students through problem-solving and scientific projects. Dewey sees the teacher as th ...
... same methods, we can expand their knowledge of not only science concepts but technology knowledge as well The progressive philosophy suggests that the curriculum be interdisciplinary and the teacher needs to guide students through problem-solving and scientific projects. Dewey sees the teacher as th ...
Lectures 1-2: Properties of the Solar System
... o Convenient because the density of water is 1 g cm-3. o To determine volume, need: 1. Distance from Earth. 2. Angular extent of the planet. o To determine the mass (from Kepler’s 3rd Law) we need: ...
... o Convenient because the density of water is 1 g cm-3. o To determine volume, need: 1. Distance from Earth. 2. Angular extent of the planet. o To determine the mass (from Kepler’s 3rd Law) we need: ...
ppt
... resembles each other in mass and size more than any other planet-satellite pair in the solar system. • The distance is also the smallest, 19,640 km • Charon’s orbit period is the same as its rotational period, and also the same as the Pluto’s rotation period (6.3 days) – Both keep the same face towa ...
... resembles each other in mass and size more than any other planet-satellite pair in the solar system. • The distance is also the smallest, 19,640 km • Charon’s orbit period is the same as its rotational period, and also the same as the Pluto’s rotation period (6.3 days) – Both keep the same face towa ...
Chapter 19 - BEEarthScience8
... Giant storms on the surface of the sun Cause the auroras on Earth ...
... Giant storms on the surface of the sun Cause the auroras on Earth ...
The Milky Way
... with a large comet from the outer Solar System. b. Jupiter swept up so much material that not enough was left to form a planet. c. Mars was once larger and collided with a large planetesimal from the inner Solar System that sent debris outward. *d. Jupiter formed early, and its gravitational influen ...
... with a large comet from the outer Solar System. b. Jupiter swept up so much material that not enough was left to form a planet. c. Mars was once larger and collided with a large planetesimal from the inner Solar System that sent debris outward. *d. Jupiter formed early, and its gravitational influen ...
Where in the Solar System Are Smaller Objects Found?
... plane, then there is only one asteroid per two trillion square kilometers (2,000,000,000,000 km2) of the orbital plane. This means that in an area that is four times the area of Earth’s surface, you would only find one rock about a kilometer in diameter. Astronomers have investigated whether the ast ...
... plane, then there is only one asteroid per two trillion square kilometers (2,000,000,000,000 km2) of the orbital plane. This means that in an area that is four times the area of Earth’s surface, you would only find one rock about a kilometer in diameter. Astronomers have investigated whether the ast ...
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.