The Origin of Mercury - Institute of Planetary Science
... From this Urey (1951, 1952) noted that Mercury must have an iron-to-silicate ratio much larger than that of any other terrestrial planet. The silicate-to-iron mass ratio is usually estimated to lie in the range from 30 : 70 to 34 : 66 or roughly 0.5. Harder and Schubert (2001) argued that the presen ...
... From this Urey (1951, 1952) noted that Mercury must have an iron-to-silicate ratio much larger than that of any other terrestrial planet. The silicate-to-iron mass ratio is usually estimated to lie in the range from 30 : 70 to 34 : 66 or roughly 0.5. Harder and Schubert (2001) argued that the presen ...
Edward RD Scott and Horton E. Newsom Institute of
... grains [9], planetary vaporization or planetary colli sions [7]. Despite these problems, the equilibrium condensa tion model is the only available quantitative guide to primordial radial variations in solid compositions, and it is still widely used. Even though there is little supporting evidence, ...
... grains [9], planetary vaporization or planetary colli sions [7]. Despite these problems, the equilibrium condensa tion model is the only available quantitative guide to primordial radial variations in solid compositions, and it is still widely used. Even though there is little supporting evidence, ...
Origin of Water Ice in the Solar System
... an important modification to the simple vapor-pressuredriven picture. Because the gaseous phase of the solar nebula is supported to a small extent by the pressure force, the gas molecules orbit slightly more slowly than the Keplerian speed associated with their radial distance from the disk center. ...
... an important modification to the simple vapor-pressuredriven picture. Because the gaseous phase of the solar nebula is supported to a small extent by the pressure force, the gas molecules orbit slightly more slowly than the Keplerian speed associated with their radial distance from the disk center. ...
Formation of Giant Planets
... The planet then contracts and cools to the present state at constant mass. Aside from core nucleated accretion, the only giant planet formation scenario receiving significant attention is the gas instability model, in which a giant planet forms directly from the contraction of a clump that was produ ...
... The planet then contracts and cools to the present state at constant mass. Aside from core nucleated accretion, the only giant planet formation scenario receiving significant attention is the gas instability model, in which a giant planet forms directly from the contraction of a clump that was produ ...
gas giant planets as dynamical barriers to inward
... of the protoplanetary disk where the radial drift speed of dust, pebbles, and small planetesimals is slowed, creating a localized enhancement in the density of solid material (Johansen et al. 2009). One favorable location for this to happen is at the snowline (Kokubo & Ida 1998; Morbidelli et al. 20 ...
... of the protoplanetary disk where the radial drift speed of dust, pebbles, and small planetesimals is slowed, creating a localized enhancement in the density of solid material (Johansen et al. 2009). One favorable location for this to happen is at the snowline (Kokubo & Ida 1998; Morbidelli et al. 20 ...
Theory of planet formation
... • shortest inspiral time is 100 yr from 1 AU for 30 cm particles • the “meter-size barrier”: planetesimals must grow from << 1 m to >> 1 m in less than a century ...
... • shortest inspiral time is 100 yr from 1 AU for 30 cm particles • the “meter-size barrier”: planetesimals must grow from << 1 m to >> 1 m in less than a century ...
The Potato Radius: a Lower Minimum Size for Dwarf Planets
... shape of objects in the universe. For example, at an average radius of ~ 200 km – 300 km, the icy moons and rocky asteroids of our Solar System transition from a rounded potato shape to a sphere. We derive this potato-to-sphere transition radius -- or “potato radius” -- from first principles. Using ...
... shape of objects in the universe. For example, at an average radius of ~ 200 km – 300 km, the icy moons and rocky asteroids of our Solar System transition from a rounded potato shape to a sphere. We derive this potato-to-sphere transition radius -- or “potato radius” -- from first principles. Using ...
Whipple: Exploring the Solar System Beyond Neptune Using a
... The Whipple mission will reach deep into the outer Solar System, conducting a blind survey for occultations of bright stars by small, distant objects. This technique can detect objects even in the Oort Cloud. Observations of stellar occultations will reveal information about the numbers and sizes of ...
... The Whipple mission will reach deep into the outer Solar System, conducting a blind survey for occultations of bright stars by small, distant objects. This technique can detect objects even in the Oort Cloud. Observations of stellar occultations will reveal information about the numbers and sizes of ...
Embedding Comets in the Asteroid Belt - SwRI Boulder
... equals to 1/2). This event triggered a global instability in the orbits of the planets that led to a violent reorganization of the outer Solar System. Uranus and Neptune penetrated the trans-planetary disk, scattering its inhabitants throughout the Solar System. The interaction between the ice giant ...
... equals to 1/2). This event triggered a global instability in the orbits of the planets that led to a violent reorganization of the outer Solar System. Uranus and Neptune penetrated the trans-planetary disk, scattering its inhabitants throughout the Solar System. The interaction between the ice giant ...
Chapter 10
... trillions of icy bodies believed to lie far beyond Pluto’s orbit to a distance of about 150,000 AU ...
... trillions of icy bodies believed to lie far beyond Pluto’s orbit to a distance of about 150,000 AU ...
Ch11_Lecture
... trillions of icy bodies believed to lie far beyond Pluto’s orbit to a distance of about 150,000 AU ...
... trillions of icy bodies believed to lie far beyond Pluto’s orbit to a distance of about 150,000 AU ...
Planetary migration and the Late Heavy
... and Neptune, which likely were the last planets to accrete and which could have altered the dynamical state of the planetary system more than a half billion years after the formation of the terrestrial planets. Still other models associate the LHB with collisional process in the early asteroid belt. ...
... and Neptune, which likely were the last planets to accrete and which could have altered the dynamical state of the planetary system more than a half billion years after the formation of the terrestrial planets. Still other models associate the LHB with collisional process in the early asteroid belt. ...
The Solar Nebula
... Slowly they grew in size until they formed large rocky and icy bodies called planetesimals, which were the size of boulders and small asteroids. The sticking mechanism that turned micron sized grains into metre sized rocks is not well understood… ...
... Slowly they grew in size until they formed large rocky and icy bodies called planetesimals, which were the size of boulders and small asteroids. The sticking mechanism that turned micron sized grains into metre sized rocks is not well understood… ...
Formation of the Solar System
... are hotter than outer parts. The disk has lots of stuff there, but very little of it can be solid at high temperatures: small, rocky/metal planetesimals. Outer parts are cooler, easy for hydrogen compounds (“ices”) to form: bigger, icy planetesimals ...
... are hotter than outer parts. The disk has lots of stuff there, but very little of it can be solid at high temperatures: small, rocky/metal planetesimals. Outer parts are cooler, easy for hydrogen compounds (“ices”) to form: bigger, icy planetesimals ...
Timing of the formation and migration of giant planets as constrained
... known chondrite groups (1) and are thought to have formed in an impact-generated gas-melt plume ~4.8 ± 0.3 My after the formation of Ca,Al-rich inclusions, the earliest solar system solids dated (4, 5). Detailed equilibrium condensation calculations (6) and bulk chemical and isotopic studies of CB c ...
... known chondrite groups (1) and are thought to have formed in an impact-generated gas-melt plume ~4.8 ± 0.3 My after the formation of Ca,Al-rich inclusions, the earliest solar system solids dated (4, 5). Detailed equilibrium condensation calculations (6) and bulk chemical and isotopic studies of CB c ...
Probabilities of Collisions of Migrating Bodies and Dust Particles
... For one object (from 10P runs with BULSTO) its probability of collisions with Earth and Venus was 0.3 and 0.7, respectively. For another object (from 2P runs) during its lifetime (352 Myr) its probability of collisions with Earth, Venus and Mars was 0.172, 0.224, and 0.065, respectively. For all 120 ...
... For one object (from 10P runs with BULSTO) its probability of collisions with Earth and Venus was 0.3 and 0.7, respectively. For another object (from 2P runs) during its lifetime (352 Myr) its probability of collisions with Earth, Venus and Mars was 0.172, 0.224, and 0.065, respectively. For all 120 ...
Planets in orbit around planetesimal belts? ββββββββ
... the β Pic debris disk have revealed an effect of strong forward scattering that decreases the degree of linear polarization with decreasing radial distance from the star (Krivova et al., 2000; Tamura et al., 2006). The strong forward scattering is also manifested in the pronounced dip around 5.3 arc ...
... the β Pic debris disk have revealed an effect of strong forward scattering that decreases the degree of linear polarization with decreasing radial distance from the star (Krivova et al., 2000; Tamura et al., 2006). The strong forward scattering is also manifested in the pronounced dip around 5.3 arc ...
PPT
... The Main Points • We didn’t observe the origin of the Solar System, so we have to develop theories that match “circumstantial evidence” - what the Solar System is like today • Observed data (today) are most consistent with theory that all the planets formed out of the same cloud of gas at the same ...
... The Main Points • We didn’t observe the origin of the Solar System, so we have to develop theories that match “circumstantial evidence” - what the Solar System is like today • Observed data (today) are most consistent with theory that all the planets formed out of the same cloud of gas at the same ...
Interpretations of Solar System Phenomena according to the
... are found in their atmospheres. According to standard stellar formation theory brown dwarfs coalesce from clouds of gas and dust, just as fusing stars do, but they do not accrue enough mass that is required to initiate and sustain nucleosynthesis. Irrespective of this shortfall of mass, their format ...
... are found in their atmospheres. According to standard stellar formation theory brown dwarfs coalesce from clouds of gas and dust, just as fusing stars do, but they do not accrue enough mass that is required to initiate and sustain nucleosynthesis. Irrespective of this shortfall of mass, their format ...
e - DTM
... Ipatov, S.I., Computer modelling of the process of solar system formation, Proc. Intern. IMACS Conference on Mathematical modelling and applied mathematics (June 18-23, 1990, Moscow). Ed. by A.A. Samarskii and M.P. Sapagovas. Elsevier. Amsterdam, pp. 245-252 (1992). Ipatov, S.I., Methods of choosing ...
... Ipatov, S.I., Computer modelling of the process of solar system formation, Proc. Intern. IMACS Conference on Mathematical modelling and applied mathematics (June 18-23, 1990, Moscow). Ed. by A.A. Samarskii and M.P. Sapagovas. Elsevier. Amsterdam, pp. 245-252 (1992). Ipatov, S.I., Methods of choosing ...
Asteroids and Comets
... Comets originally orbited among the giant planets as planetesimals, then were tossed into the Oort cloud by those planets The shape of the Oort cloud is determined from observations of comet orbits Some comet orbits seem to come from a flatter, less remote region – the Kuiper belt, which exten ...
... Comets originally orbited among the giant planets as planetesimals, then were tossed into the Oort cloud by those planets The shape of the Oort cloud is determined from observations of comet orbits Some comet orbits seem to come from a flatter, less remote region – the Kuiper belt, which exten ...
Lecture7
... Gravitational instability model: pros and cons • Pros: – Under some circumstances it may be natural to form gravitationally unstable disks – Happens very fast ...
... Gravitational instability model: pros and cons • Pros: – Under some circumstances it may be natural to form gravitationally unstable disks – Happens very fast ...
Lecture7_2014
... Gravitational instability model: pros and cons • Pros: – Under some circumstances it may be natural to form gravitationally unstable disks – Happens very fast ...
... Gravitational instability model: pros and cons • Pros: – Under some circumstances it may be natural to form gravitationally unstable disks – Happens very fast ...
Source of zodiac glow identified ground vehicles
... SwRI researchers design and build gas bearing test rig Researchers at Southwest Research Institute (SwRI) have designed and built a 60,000 rpm gas bearing test rig to test the rotordynamic stability of gas bearings. The use of gas bearings has increased over the past several decades to include micro ...
... SwRI researchers design and build gas bearing test rig Researchers at Southwest Research Institute (SwRI) have designed and built a 60,000 rpm gas bearing test rig to test the rotordynamic stability of gas bearings. The use of gas bearings has increased over the past several decades to include micro ...