Fulltext
... Even today, some textbooks describe the Solar System as a quiet, highly ordered structure. The Sun is in the center and planets revolve around it on neat elliptical orbits that are assumed to be the same since the time of creation of the Solar System. The space in between (the interplanetary space) ...
... Even today, some textbooks describe the Solar System as a quiet, highly ordered structure. The Sun is in the center and planets revolve around it on neat elliptical orbits that are assumed to be the same since the time of creation of the Solar System. The space in between (the interplanetary space) ...
Introduction to the Solar System
... (Figure 1.6) shows the Sun and the major objects that orbit the Sun. There are eight planets (Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune) and the five known dwarf planets and the five known dwarf planets (Ceres, Pluto, Makemake, Haumea, and Eris). ...
... (Figure 1.6) shows the Sun and the major objects that orbit the Sun. There are eight planets (Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune) and the five known dwarf planets and the five known dwarf planets (Ceres, Pluto, Makemake, Haumea, and Eris). ...
Chapter 15 The Formation of Planetary Systems
... However many multi-planet systems are now known, and one system has two planets that resemble Jupiter and Saturn. (See earlier slide with a Jupiter-like orbit for reminder of why it takes so long to find these planets.) ! Selection effect biases sample toward massive planets ...
... However many multi-planet systems are now known, and one system has two planets that resemble Jupiter and Saturn. (See earlier slide with a Jupiter-like orbit for reminder of why it takes so long to find these planets.) ! Selection effect biases sample toward massive planets ...
minimum mass solar nebulæ and planetary migration
... The Minimum Mass Solar Nebula (hereafter MMSN) is the protoplanetary disk of solar composition that has the amount of metals necessary to build the eight planets of the Solar System (and the asteroid belts). From the masses and compositions of the planets, a density of solids is derived at several l ...
... The Minimum Mass Solar Nebula (hereafter MMSN) is the protoplanetary disk of solar composition that has the amount of metals necessary to build the eight planets of the Solar System (and the asteroid belts). From the masses and compositions of the planets, a density of solids is derived at several l ...
Chapter 15 The Formation of Planetary Systems
... However many multi-planet systems are now known, and one system has two planets that resemble Jupiter and Saturn. (See earlier slide with a Jupiter-like orbit for reminder of why it takes so long to find these planets.) Selection effect biases sample toward massive planets ...
... However many multi-planet systems are now known, and one system has two planets that resemble Jupiter and Saturn. (See earlier slide with a Jupiter-like orbit for reminder of why it takes so long to find these planets.) Selection effect biases sample toward massive planets ...
Slide 1
... Multiple Epoch HST imaging reveals an object bound to the system Planet discovered at 115AU Interpretation rests on chaotic zone boundary ...
... Multiple Epoch HST imaging reveals an object bound to the system Planet discovered at 115AU Interpretation rests on chaotic zone boundary ...
Chapter 10
... • Orbits of Near-Earth Objects (NEOs) carry them into the inner Solar System and across the Earth’s orbit – More than 5000 have been found, which represents an Earth collision probability of once every 10,000 years – They may be “dead” comets, shifted into their orbits by Jupiter and devoid of surfa ...
... • Orbits of Near-Earth Objects (NEOs) carry them into the inner Solar System and across the Earth’s orbit – More than 5000 have been found, which represents an Earth collision probability of once every 10,000 years – They may be “dead” comets, shifted into their orbits by Jupiter and devoid of surfa ...
Analysis of Two Pulsating X-ray Sources
... itself is the stellar core of a Sun-sized star at the end of its evolutionary history – a rotating carbon core. The light curve above is produced by the dynamics of the system and not the white dwarf itself, which emits most of its radiation in X-rays. More massive stars, which catastrophically coll ...
... itself is the stellar core of a Sun-sized star at the end of its evolutionary history – a rotating carbon core. The light curve above is produced by the dynamics of the system and not the white dwarf itself, which emits most of its radiation in X-rays. More massive stars, which catastrophically coll ...
The first cool rocky/icy exoplanet
... other than the Sun (Beaulieu et al. 2006). This discovery from gravitational microlensing, the technique of monitoring stars in the galactic bulge magnified by the bending of light due to the gravitational field of an intervening foreground star, provides the first observational hint that planets l ...
... other than the Sun (Beaulieu et al. 2006). This discovery from gravitational microlensing, the technique of monitoring stars in the galactic bulge magnified by the bending of light due to the gravitational field of an intervening foreground star, provides the first observational hint that planets l ...
planet formation scenarios Core accretion model
... • One obtains a 2-D problem (instead of 3-D) and higher capture chances. • Can increase formation speed by a factor of 10 or more. Is even effective if only 1% of planetesimals is small enough for shear-dominated regime ...
... • One obtains a 2-D problem (instead of 3-D) and higher capture chances. • Can increase formation speed by a factor of 10 or more. Is even effective if only 1% of planetesimals is small enough for shear-dominated regime ...
THE THOUSAND-YARD MODEL or, The Earth as a Peppercorn
... paces (more than twice as as the total distance walked up till then). This gap marks the boundary between the inner and outer solar systems. The inner solar system contains the four small, hard, "terrestrial" (Earth-like) planet; the outer solar system contains the four large, fluid, "Jovian" (Jupit ...
... paces (more than twice as as the total distance walked up till then). This gap marks the boundary between the inner and outer solar systems. The inner solar system contains the four small, hard, "terrestrial" (Earth-like) planet; the outer solar system contains the four large, fluid, "Jovian" (Jupit ...
Overview of Our Solar System
... The Terrestrial 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. – Th ...
... The Terrestrial 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. – Th ...
Sun and Planets.notebook
... Terrestrial Planets (the four “inner planets”) • Larger / Smaller planets of relatively high / low ...
... Terrestrial Planets (the four “inner planets”) • Larger / Smaller planets of relatively high / low ...
userfiles/602xxh/files/2013%e5%b1%8a%e9%ab%98%e4%b8%89
... most certain about are large—up to 25 times the size of Earth. According to Christophe Lovis, one of the scientists behind the finding, these five planets are similar to Neptune(海王星). “They’re made mainly of rocks and ice，” he said. “They’re probably not suitable for people to live in.” ...
... most certain about are large—up to 25 times the size of Earth. According to Christophe Lovis, one of the scientists behind the finding, these five planets are similar to Neptune(海王星). “They’re made mainly of rocks and ice，” he said. “They’re probably not suitable for people to live in.” ...
class14
... Formed in orbit around jovian planets. Circular orbits in same direction as planet rotation. ...
... Formed in orbit around jovian planets. Circular orbits in same direction as planet rotation. ...
The Search for Extrasolar Planets
... 1995, when Mayor & Queloz5 announced the first discovery of an extrasolar planet orbiting the star 51 Pegasi, by using precise radial velocities (Fig. 1) obtained with the ELODIE spectrograph in the Haute-Provence Observatory. The planet has a mass of 0.44 MJ and an orbital period of 4.23 days, whic ...
... 1995, when Mayor & Queloz5 announced the first discovery of an extrasolar planet orbiting the star 51 Pegasi, by using precise radial velocities (Fig. 1) obtained with the ELODIE spectrograph in the Haute-Provence Observatory. The planet has a mass of 0.44 MJ and an orbital period of 4.23 days, whic ...
Intro to Solar System
... photographic plates 39 AU from the Sun, now is orbiting closer than Neptune methane coated ice surface temperature 60 K nitrogen and CO ices rotation period 6.4 days atmosphere - N, CO, methane Intro to Solar System ...
... photographic plates 39 AU from the Sun, now is orbiting closer than Neptune methane coated ice surface temperature 60 K nitrogen and CO ices rotation period 6.4 days atmosphere - N, CO, methane Intro to Solar System ...
Lecture 3
... The Romans named the planet after the Roman god Jupiter (the god of sky and thunder). When viewed from Earth, Jupiter is the third brightest object in the night sky after the Moon and Venus. (At certain points in its orbit, Mars can briefly exceed Jupiter's brightness.) ...
... The Romans named the planet after the Roman god Jupiter (the god of sky and thunder). When viewed from Earth, Jupiter is the third brightest object in the night sky after the Moon and Venus. (At certain points in its orbit, Mars can briefly exceed Jupiter's brightness.) ...
Sumerian Picture of Tiamat
... according to my research, that conclusion is wrong. Below, I proof that this additional heavenly body, that is currently no longer present in our solar system, was the planet known as Tiamat. The figure on the left-hand side shows these twelve spheres numbered according to the ordering of the sizes ...
... according to my research, that conclusion is wrong. Below, I proof that this additional heavenly body, that is currently no longer present in our solar system, was the planet known as Tiamat. The figure on the left-hand side shows these twelve spheres numbered according to the ordering of the sizes ...
Models
... Use a ruler to measure the diameter of each object then draw a circle around the diameter to show the scale size of the planet. Color the planet to look like the planet Add at least one fact about the planet. ...
... Use a ruler to measure the diameter of each object then draw a circle around the diameter to show the scale size of the planet. Color the planet to look like the planet Add at least one fact about the planet. ...
DeltaScience - Delta Education
... baseball and a tennis ball are about the same size. However, a baseball is heavier because it has more mass. Thus it is more dense than a tennis ball. ...
... baseball and a tennis ball are about the same size. However, a baseball is heavier because it has more mass. Thus it is more dense than a tennis ball. ...
Lecture8_2014_v2 - UCO/Lick Observatory
... • Three planets of 15, 5 and 7 Earth masses • Small, red star Page ...
... • Three planets of 15, 5 and 7 Earth masses • Small, red star Page ...
Directed Reading
... a. oxygen and nitrogen. b. hydrogen and helium. c. nitrogen and helium. d. hydrogen and oxygen. ______ 29. Today, hydrogen and helium occur mainly in the a. oceans. b. middle atmosphere. c. lower atmosphere. d. upper atmosphere. ______ 30. Earth’s early atmosphere formed when volcanic eruptions rele ...
... a. oxygen and nitrogen. b. hydrogen and helium. c. nitrogen and helium. d. hydrogen and oxygen. ______ 29. Today, hydrogen and helium occur mainly in the a. oceans. b. middle atmosphere. c. lower atmosphere. d. upper atmosphere. ______ 30. Earth’s early atmosphere formed when volcanic eruptions rele ...
Other Bodies in the Solar System
... Titius vonWittenburg • In 1801 Giuseppe Piazzi discovered the planet “Ceres” • William Herschel categorized Ceres and the other dwarf planets as asteroids , “star like” http://upload.wikimedia. org/wikipedia/commons/ 9/92/Giuseppe_Piazzi.jpg ...
... Titius vonWittenburg • In 1801 Giuseppe Piazzi discovered the planet “Ceres” • William Herschel categorized Ceres and the other dwarf planets as asteroids , “star like” http://upload.wikimedia. org/wikipedia/commons/ 9/92/Giuseppe_Piazzi.jpg ...
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.