PPT 5 - Uranus, Neptune and Pluto
... methane; 105 times less dense than Earth’s atmosphere. Surface composed of ices: nitrogen, methane, carbon ...
... methane; 105 times less dense than Earth’s atmosphere. Surface composed of ices: nitrogen, methane, carbon ...
JWST Study of Planetary Systems and Solar System Objects
... Planetary atmospheres will be characterized with near-IR spectra from NIRSpec. The 1-5 µm region contains many atomic and molecular transitions that are seen in absorption in planetary atmospheres, including species like H2O, CO2, O2 that are very difficult to detect in ground-based spectra due to h ...
... Planetary atmospheres will be characterized with near-IR spectra from NIRSpec. The 1-5 µm region contains many atomic and molecular transitions that are seen in absorption in planetary atmospheres, including species like H2O, CO2, O2 that are very difficult to detect in ground-based spectra due to h ...
Debris Belts around Vega - Astronomical Society of the Pacific
... giant planets orbiting in the gap between belts. • Our own solar system also has four giant planets orbiting between the rocky asteroid belt and the icy Kuiper belt. • No planets have yet been detected around Vega, but if the star were eventually found to have several giant planets in orbit, this ...
... giant planets orbiting in the gap between belts. • Our own solar system also has four giant planets orbiting between the rocky asteroid belt and the icy Kuiper belt. • No planets have yet been detected around Vega, but if the star were eventually found to have several giant planets in orbit, this ...
ES 104 Midterm Exam Study Guide 1
... Know how the craters and the maria on Earth’s moon were formed. Jovian planets versus the Terrestrial planets – be familiar with the physical and compositional differences between these 2 categories of planets – look over the table that you completed for the first homework activity. Also know why th ...
... Know how the craters and the maria on Earth’s moon were formed. Jovian planets versus the Terrestrial planets – be familiar with the physical and compositional differences between these 2 categories of planets – look over the table that you completed for the first homework activity. Also know why th ...
Temperate Earth-sized planets transiting a nearby ultracool
... gases19. Statistical analyses of sub-Neptune-sized planets detected by the Kepler spacecraft indicate that most Earth-sized planets in close orbit around solar-type stars are rocky20,21. Nonetheless, the paucity of material in the inner region of the protoplanetary disk of an ultracool dwarf would s ...
... gases19. Statistical analyses of sub-Neptune-sized planets detected by the Kepler spacecraft indicate that most Earth-sized planets in close orbit around solar-type stars are rocky20,21. Nonetheless, the paucity of material in the inner region of the protoplanetary disk of an ultracool dwarf would s ...
BLENDED UNIT PLANNING DOCUMENT
... Section 2: The Sun 1. Why is it usually impossible to see the sun’s corona from Earth? 2. Describe the three features found on or above the Sun’s surface? Section 3: The Inner Planets 1. Compare the atmosphere of all four planets? 2. How are the four planets similar? 3. Give one important characteri ...
... Section 2: The Sun 1. Why is it usually impossible to see the sun’s corona from Earth? 2. Describe the three features found on or above the Sun’s surface? Section 3: The Inner Planets 1. Compare the atmosphere of all four planets? 2. How are the four planets similar? 3. Give one important characteri ...
The Solar System - Gordon College English Center
... The Solar System is the name that was given to the collection of celestial bodies that contains the Sun (which is a star by definition) and eight planets (which Earth is one of them) that orbit the sun regularly. In ancient times, people gazed at the night sky. They observed thousands of spots of li ...
... The Solar System is the name that was given to the collection of celestial bodies that contains the Sun (which is a star by definition) and eight planets (which Earth is one of them) that orbit the sun regularly. In ancient times, people gazed at the night sky. They observed thousands of spots of li ...
Planetary Systems Around White Dwarfs Given the ubiquity of
... he vast majority of all known planet-hosting stars, including the Sun, will eventually evolve into red giants, lose a significant fraction of their mass as a planetary nebula, and finally end their lives as white dwarfs: extremely dense Earth-sized stellar embers that slowly consume their thermal he ...
... he vast majority of all known planet-hosting stars, including the Sun, will eventually evolve into red giants, lose a significant fraction of their mass as a planetary nebula, and finally end their lives as white dwarfs: extremely dense Earth-sized stellar embers that slowly consume their thermal he ...
No Slide Title
... billion years) in the Universe are slim – With less heavy elements available terrestrial planets may be smaller and lower in mass than in our solar system – Is there a threshold metallicity for life to start (e.g. ½ solar)? ...
... billion years) in the Universe are slim – With less heavy elements available terrestrial planets may be smaller and lower in mass than in our solar system – Is there a threshold metallicity for life to start (e.g. ½ solar)? ...
Earth-like worlds on eccentric orbits - Physics
... but Mischna et al. also found significantly less warming under a less-optimized cloud cover. An important uncertainty here is the CO2 cloud lifetime, which might be short if the cloud particles snow out on to the surface soon after forming, as occurs on Mars today. The seasonal sequestering of CO2 a ...
... but Mischna et al. also found significantly less warming under a less-optimized cloud cover. An important uncertainty here is the CO2 cloud lifetime, which might be short if the cloud particles snow out on to the surface soon after forming, as occurs on Mars today. The seasonal sequestering of CO2 a ...
SOLAR SYSTEM BRACELET/ANKLET
... Astronomical Unit measurements. If the seed beads could be cut into fractions, the distance between the inner planets would be much more accurate, thus the less then 1 AU are represented by a white seed bead. Using representative AU’s however, you can make an interesting necklace. Vocabulary: Planet ...
... Astronomical Unit measurements. If the seed beads could be cut into fractions, the distance between the inner planets would be much more accurate, thus the less then 1 AU are represented by a white seed bead. Using representative AU’s however, you can make an interesting necklace. Vocabulary: Planet ...
Project Icarus: Astronomical Considerations Relating to the Choice
... (i.e. just beyond the orbit of Jupiter in our Solar System), with a period of 6.8 years. Although this would span the habitable zone (i.e. the range of distances from a star on which liquid water would be stable on a planetary surface given certain assumptions about atmospheric composition), this or ...
... (i.e. just beyond the orbit of Jupiter in our Solar System), with a period of 6.8 years. Although this would span the habitable zone (i.e. the range of distances from a star on which liquid water would be stable on a planetary surface given certain assumptions about atmospheric composition), this or ...
takes its time doing so. The coolest white dwarfs
... mostly hydrogen atmosphere white dwarfs, though the statistics have taken into account the contribution from white dwarfs without hydrogen. The cooler white dwarfs were identified from the Lutyen Half Second proper motion catalogusing a method developed by Schmidt 1975. There were over 80 stars know ...
... mostly hydrogen atmosphere white dwarfs, though the statistics have taken into account the contribution from white dwarfs without hydrogen. The cooler white dwarfs were identified from the Lutyen Half Second proper motion catalogusing a method developed by Schmidt 1975. There were over 80 stars know ...
pptx - University of Rochester
... 5:4, 6:5 resonances and capture into the 7:6 resonance. Stochastic forcing would pull the system out of resonance unless the gas disk is depleted soon after capture • Encounters with planetary embryos can remove two planets from outer resonances allowing them to end up in adjacent orbits like Kepler ...
... 5:4, 6:5 resonances and capture into the 7:6 resonance. Stochastic forcing would pull the system out of resonance unless the gas disk is depleted soon after capture • Encounters with planetary embryos can remove two planets from outer resonances allowing them to end up in adjacent orbits like Kepler ...
PDF only - at www.arxiv.org.
... 3.5. Disk Signatures: High resolution imaging and spectroscopy of protoplanetary and debris disks can provide constraints on the early stages of planet formation that are very complimentary to exoplanet observations. These observations can also reveal disk asymmetries most likely due to perturbatio ...
... 3.5. Disk Signatures: High resolution imaging and spectroscopy of protoplanetary and debris disks can provide constraints on the early stages of planet formation that are very complimentary to exoplanet observations. These observations can also reveal disk asymmetries most likely due to perturbatio ...
Educator`s Guide for Oasis in Space
... Where might these aliens live? What would they need to survive? Things to Do: 1. Pass around pictures and stories of controversial formations on other planets, such as the “Mars Face”, the pyramids and the canals some claim to be on Mars (see below). 2. Have students discuss or write about what they ...
... Where might these aliens live? What would they need to survive? Things to Do: 1. Pass around pictures and stories of controversial formations on other planets, such as the “Mars Face”, the pyramids and the canals some claim to be on Mars (see below). 2. Have students discuss or write about what they ...
Volume 2 - Euresis Journal
... Astronomers are very adept at measuring velocities of celestial bodies using the Doppler effect that velocity induces on the light waves emitted by those bodies. Just as the pitch of the sound from an approaching train whistle is higher than that from a receding one, light from an approaching star g ...
... Astronomers are very adept at measuring velocities of celestial bodies using the Doppler effect that velocity induces on the light waves emitted by those bodies. Just as the pitch of the sound from an approaching train whistle is higher than that from a receding one, light from an approaching star g ...
Light and shadow from distant worlds
... astronomical techniques to observe a planet spatially resolved from the star is high-contrast imaging, as being developed for a Terrestrial Planet Finder mission3,4. Recent advances in ground-based imaging5,6 have led to the discovery of giant planets orbiting dozens to hundreds of astronomical unit ...
... astronomical techniques to observe a planet spatially resolved from the star is high-contrast imaging, as being developed for a Terrestrial Planet Finder mission3,4. Recent advances in ground-based imaging5,6 have led to the discovery of giant planets orbiting dozens to hundreds of astronomical unit ...
10 - The Catholic University of America
... for Mars, Venus, and Mercury, than that for the Earth. This larger mass fraction would result in relatively large ancient oceans on Mars and Venus. For dust particles produced by comets and asteroids, PE was found to have a maximum (~0.001-0.02) at diameters of particles d~100 micron. These maximum ...
... for Mars, Venus, and Mercury, than that for the Earth. This larger mass fraction would result in relatively large ancient oceans on Mars and Venus. For dust particles produced by comets and asteroids, PE was found to have a maximum (~0.001-0.02) at diameters of particles d~100 micron. These maximum ...
ORBITAL MOTION
... Debris disks are remnant accretion disks with little or no gas left (just dust & rocks), outflow has stopped, the star is visible. Theory: Gas disperses, “planetesimals” form (100 km diameter rocks), collide & stick together due to gravity forming protoplanets). Protoplanets interact with dust disks ...
... Debris disks are remnant accretion disks with little or no gas left (just dust & rocks), outflow has stopped, the star is visible. Theory: Gas disperses, “planetesimals” form (100 km diameter rocks), collide & stick together due to gravity forming protoplanets). Protoplanets interact with dust disks ...
What is a planet? - X-ray and Observational Astronomy Group
... • There are two main models which have been proposed to • describe the formation of the extra-solar planets: – (I) Planets form from dust which agglomerates into cores which then accrete gas from a disc. – (II) A gravitational instability in a protostellar disc creates a number of giant planets. ...
... • There are two main models which have been proposed to • describe the formation of the extra-solar planets: – (I) Planets form from dust which agglomerates into cores which then accrete gas from a disc. – (II) A gravitational instability in a protostellar disc creates a number of giant planets. ...
Powerpoint to Solar System Scale Activity by Doreen Jarvis
... Place the piece of paper on your desk in front of you vertically. In very small letters, write “Sun” on the very top edge of the strip and then write “Pluto” on the very bottom of the strip. ...
... Place the piece of paper on your desk in front of you vertically. In very small letters, write “Sun” on the very top edge of the strip and then write “Pluto” on the very bottom of the strip. ...
PowerPoint Presentation - A Tour of the Solar System
... Asteroids are either rocky or metallic objects that orbit the Sun. They are too small to considered planets but are sometimes called planetoids. ...
... Asteroids are either rocky or metallic objects that orbit the Sun. They are too small to considered planets but are sometimes called planetoids. ...
October, 2006 - The Astronomical Society of Las Cruces
... exactly 1.5 times that of Neptune is corrected. Like a pendulum slightly disturbed from hanging straight down, Pluto's orbital period oscillates around 1.5 times Neptune's rather than remains at exactly that value. For other Trans-Neptunian objects in the 2:3 resonance lock the same conditions hold. ...
... exactly 1.5 times that of Neptune is corrected. Like a pendulum slightly disturbed from hanging straight down, Pluto's orbital period oscillates around 1.5 times Neptune's rather than remains at exactly that value. For other Trans-Neptunian objects in the 2:3 resonance lock the same conditions hold. ...
Our Planetary System
... Neptune • Similar to Uranus (except for axis tilt) • Many moons (including Triton) ...
... Neptune • Similar to Uranus (except for axis tilt) • Many moons (including Triton) ...
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.