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AST_s309_ss11_6 - Astronomy Program
... Difficult case. This results in no radial velocity variations as the fainter binary probably has too little flux to be measured by high resolution spectrographs. Large amounts of telescope time can be wasted with no conclusion. High resolution imaging may help to see faint background star. ...
... Difficult case. This results in no radial velocity variations as the fainter binary probably has too little flux to be measured by high resolution spectrographs. Large amounts of telescope time can be wasted with no conclusion. High resolution imaging may help to see faint background star. ...
Dynamics of disks with planets
... The standard model of planet formation agrees with numerous observations of circumstellar disks. Many dusty disks known as Vega-excess systems (because of infrared radiation detected by satellite IRAS around Vega, much exceeding the flux from the star itself) are good, if not exact, analogues of an ...
... The standard model of planet formation agrees with numerous observations of circumstellar disks. Many dusty disks known as Vega-excess systems (because of infrared radiation detected by satellite IRAS around Vega, much exceeding the flux from the star itself) are good, if not exact, analogues of an ...
a High-Mass Protostar with a Rotating Disk.
... The molecular cloud southwest of the H II region NGC 7538 is a well known site of high-mass star formation [6]. However, the OH and H2 O maser source 8000 south of IRS 1, NGC 7538 S, is even younger and more extreme than any of the other known high–mass (proto)stars in this region. It is very deeply ...
... The molecular cloud southwest of the H II region NGC 7538 is a well known site of high-mass star formation [6]. However, the OH and H2 O maser source 8000 south of IRS 1, NGC 7538 S, is even younger and more extreme than any of the other known high–mass (proto)stars in this region. It is very deeply ...
Our Solar System - hrsbstaff.ednet.ns.ca
... Learning Outcomes (Students will…) -Explain the theories for the origin of the solar system -Distinguish between questions that can be answered by science and those that cannot, and between problems that can be solved by technology and those that cannot with regards to solar system formation. -Esti ...
... Learning Outcomes (Students will…) -Explain the theories for the origin of the solar system -Distinguish between questions that can be answered by science and those that cannot, and between problems that can be solved by technology and those that cannot with regards to solar system formation. -Esti ...
Catching Planets in Formation with GMT
... • Substantial mismatch between predicted and observed distribution of exoplanets. • Major uncertainties: • How do gas-giant planets form. • How much do planets migrate. • Are there many habitable (water, etc) planets. ...
... • Substantial mismatch between predicted and observed distribution of exoplanets. • Major uncertainties: • How do gas-giant planets form. • How much do planets migrate. • Are there many habitable (water, etc) planets. ...
HollandLZ 07Nature Canestro Oikopleura Retinoic DB in
... magnitude of this diminution (generally about one part in 100) translates into an estimate of the planet’s radius. Using low-tech, groundbased telescopes, working at optical-light wavelengths, it is easy to make photometric observations that can discern an effect of this magnitude. The radii of all ...
... magnitude of this diminution (generally about one part in 100) translates into an estimate of the planet’s radius. Using low-tech, groundbased telescopes, working at optical-light wavelengths, it is easy to make photometric observations that can discern an effect of this magnitude. The radii of all ...
Lecture PowerPoint
... Q:2 Does life in any form however simple or complex, carbon-based or other, exist elsewhere than on Earth? Are there Earth-like planets beyond our solar system? ...
... Q:2 Does life in any form however simple or complex, carbon-based or other, exist elsewhere than on Earth? Are there Earth-like planets beyond our solar system? ...
Field Star Distributions of the Hercules Thick Disk Cloud
... about the l=0 line of symmetry. In Figure 9 presents the calculation for two fields where the excess was not seen and Figure 10 presents the excess for two fields with the excess. While no difference is seen in the distribution of Figure 9, Figure 10 shows the Q1 line of sight has more stars between ...
... about the l=0 line of symmetry. In Figure 9 presents the calculation for two fields where the excess was not seen and Figure 10 presents the excess for two fields with the excess. While no difference is seen in the distribution of Figure 9, Figure 10 shows the Q1 line of sight has more stars between ...
ppt
... There are only two astronomical bodies that have a radius ~ 1.5 REarth: 1. White Dwarf 2. A terrestrial planet White Dwarfs have a mass of ~ 1 Solar Mass, so the radial velocity amplitude should be ~ 100s km/s. This is excluded by low precision radial velocity measurements. ...
... There are only two astronomical bodies that have a radius ~ 1.5 REarth: 1. White Dwarf 2. A terrestrial planet White Dwarfs have a mass of ~ 1 Solar Mass, so the radial velocity amplitude should be ~ 100s km/s. This is excluded by low precision radial velocity measurements. ...
Structure and Evolution of Gas and Dust in Inner
... Grain growth – settling of large grains to midplane, reduced opactiy in irradiation surface – decrease MIR flux ...
... Grain growth – settling of large grains to midplane, reduced opactiy in irradiation surface – decrease MIR flux ...
c12exoplanets1_backup
... “ There are innumerable worlds of different sizes. These worlds are at irregular distances, more in one direction and less in another, and some are flourishing, others declining. Here they come into being, there they die, and they are destroyed by collision with one another. Some of the worlds have ...
... “ There are innumerable worlds of different sizes. These worlds are at irregular distances, more in one direction and less in another, and some are flourishing, others declining. Here they come into being, there they die, and they are destroyed by collision with one another. Some of the worlds have ...
Parade of Planets
... Parade of Planets This article originally appeared in the March 2000 issue of Astronomy. 21 February, 2000 The parade of extrasolar planets around normal stars began in 1995 when Michel Mayor and Didier Queloz of the Geneva Observatory in Switzerland discovered a planet at a distance of only 4.6 mil ...
... Parade of Planets This article originally appeared in the March 2000 issue of Astronomy. 21 February, 2000 The parade of extrasolar planets around normal stars began in 1995 when Michel Mayor and Didier Queloz of the Geneva Observatory in Switzerland discovered a planet at a distance of only 4.6 mil ...
Determining the mass of an extrasolar planet
... the top of page 98. It says there that the “other information” needed to find the mass of an extrasolar planet comes from two sources: the H-R diagram and Kepler’s Third Law as modified by Newton. How do these additional resources come into play in this process? The role of the HR diagram is to prov ...
... the top of page 98. It says there that the “other information” needed to find the mass of an extrasolar planet comes from two sources: the H-R diagram and Kepler’s Third Law as modified by Newton. How do these additional resources come into play in this process? The role of the HR diagram is to prov ...
The Formation of Massive Star Systems by Accretion
... radiation pressure produced no noticeable effects. After ~20,000 years, the disk became gravitationally unstable and developed a pronounced twoarmed spiral that transported angular momentum efficiently (Fig. 1B) (24). Accretion onto the protostar continued smoothly. Accretion, unimpeded by radiation ...
... radiation pressure produced no noticeable effects. After ~20,000 years, the disk became gravitationally unstable and developed a pronounced twoarmed spiral that transported angular momentum efficiently (Fig. 1B) (24). Accretion onto the protostar continued smoothly. Accretion, unimpeded by radiation ...
alien planets - astronomy
... rogue planets—planet-sized objects that have been ejected from their star systems and are no longer bound to their stars by gravity. ...
... rogue planets—planet-sized objects that have been ejected from their star systems and are no longer bound to their stars by gravity. ...
Accretion Disk
... still be two stars: a low mass star still burning hydrogen, and a helium proto-white dwarf. The separation will be very small, and the hot core will ionize the ejected envelope, producing a planetary nebula. ...
... still be two stars: a low mass star still burning hydrogen, and a helium proto-white dwarf. The separation will be very small, and the hot core will ionize the ejected envelope, producing a planetary nebula. ...
The Origin of the Solar System
... Computer simulations show that Jovian planets can grow by direct gas accretion without forming rocky ...
... Computer simulations show that Jovian planets can grow by direct gas accretion without forming rocky ...
Discovery of a probable 4 − 5 Jupiter
... planet may become a benchmark for physical studies of young giant planets but also for formation and evolution theories of planetary systems. ...
... planet may become a benchmark for physical studies of young giant planets but also for formation and evolution theories of planetary systems. ...
PowerPoint プレゼンテーション
... Around TTSs, f(CO) has been estimated to be upto ~200. Since Td would be higher around Herbig Ae stars, f(CO) would be less than 200. ...
... Around TTSs, f(CO) has been estimated to be upto ~200. Since Td would be higher around Herbig Ae stars, f(CO) would be less than 200. ...
Nebular Theory: Summary
... • Most inhabit the asteroid belt between Mars & Jupiter. – Jupiter’s gravity prevented a planet from forming there. ...
... • Most inhabit the asteroid belt between Mars & Jupiter. – Jupiter’s gravity prevented a planet from forming there. ...
Time From the Perspective of a Particle Physicist
... • condensation starts, protoplanets grow in size -objects collide; stick together • over millions of years sweep out most smaller objects as collide with larger objects existing planets • only ~circular orbits won’t collide any further (asteroid belt between Mars and Jupiter) • Possible motion of ...
... • condensation starts, protoplanets grow in size -objects collide; stick together • over millions of years sweep out most smaller objects as collide with larger objects existing planets • only ~circular orbits won’t collide any further (asteroid belt between Mars and Jupiter) • Possible motion of ...
WASP2007_national_pressV5
... Dr Don Pollacco, of Queen's University Belfast, said “We are the only team to have found transiting planets in both the Northern and Southern hemispheres; for the first time we have both SuperWASP cameras running, giving complete coverage of the whole sky”. Exoplanet expert Professor Andrew Cameron, ...
... Dr Don Pollacco, of Queen's University Belfast, said “We are the only team to have found transiting planets in both the Northern and Southern hemispheres; for the first time we have both SuperWASP cameras running, giving complete coverage of the whole sky”. Exoplanet expert Professor Andrew Cameron, ...
Milky Way Bulge
... • Discovered in 1994 from star counts + radial velocity study of K,M giants towards Galactic Center. • ~5 x 109 M • ~17 kpc beyond GC, and currently falling into disk ...
... • Discovered in 1994 from star counts + radial velocity study of K,M giants towards Galactic Center. • ~5 x 109 M • ~17 kpc beyond GC, and currently falling into disk ...
Birth - Wayne State University Physics and Astronomy
... undergo fusion into helium, with about 4 million tons turning to energy in the process This rate of hydrogen use means that eventually the Sun (and all other stars) will run out of central fuel ...
... undergo fusion into helium, with about 4 million tons turning to energy in the process This rate of hydrogen use means that eventually the Sun (and all other stars) will run out of central fuel ...
What Exoplanets tell us about Planet Formation
... within our Solar System, little is known about them • Exoplanets have provided first-order information about planetary growth – Inner giant planets imply that migration is important – Planet-metallicity correlation implies (most if not all) giant planets formed via core-nucleated accretion ...
... within our Solar System, little is known about them • Exoplanets have provided first-order information about planetary growth – Inner giant planets imply that migration is important – Planet-metallicity correlation implies (most if not all) giant planets formed via core-nucleated accretion ...
Beta Pictoris
Beta Pictoris (β Pic, β Pictoris) is the second brightest star in the constellation Pictor. It is located 63.4 light years from our solar system, and is 1.75 times as massive and 8.7 times as luminous as the Sun. The Beta Pictoris system is very young, only 8–20 million years old, although it is already in the main sequence stage of its evolution. Beta Pictoris is the title member of the Beta Pictoris moving group, an association of young stars which share the same motion through space and have the same age.Beta Pictoris shows an excess of infrared emission compared to normal stars of its type, which is caused by large quantities of dust and gas (including carbon monoxide) near the star. Detailed observations reveal a large disk of dust and gas orbiting the star, which was the first debris disk to be imaged around another star. In addition to the presence of several planetesimal belts and cometary activity, there are indications that planets have formed within this disk and that the processes of planet formation may still be ongoing. Material from the Beta Pictoris debris disk is thought to be the dominant source of interstellar meteoroids in our solar system.The European Southern Observatory (ESO) has confirmed the presence of a planet, Beta Pictoris b, matching previous predictions, through the use of direct imagery, orbiting in the plane of the debris disk surrounding the star. This planet is currently the closest extrasolar planet to its star ever photographed: the observed separation is roughly the same as the distance between Saturn and the Sun.