Direct Imaging Searches Around White Dwarfs - X
... than their progenitors – Improve resolution problem through widening of orbits • M(MS) / M(WD) (Jeans 1924) ...
... than their progenitors – Improve resolution problem through widening of orbits • M(MS) / M(WD) (Jeans 1924) ...
White Dwarf Stars - Stellar Physics Department
... H for magnetic white dwarfs that do show any detectable polarization. P for polarized magnetic white dwarfs. V for variable white dwarfs. And finally to complete the classification, a temperature index can follow their spectral classification. This index is defined as θ = 50400/Teff . Therefore, a w ...
... H for magnetic white dwarfs that do show any detectable polarization. P for polarized magnetic white dwarfs. V for variable white dwarfs. And finally to complete the classification, a temperature index can follow their spectral classification. This index is defined as θ = 50400/Teff . Therefore, a w ...
High-resolution simulations of the final assembly of Earth
... may not even track the innermost water-rich material (Cyr et al. 1998; Kornet et al. 2004). It is therefore unclear whether the Solar System’s initial water distribution is typical of protoplanetary disks in the Galaxy. The starting iron contents of protoplanets are interpolated between the values f ...
... may not even track the innermost water-rich material (Cyr et al. 1998; Kornet et al. 2004). It is therefore unclear whether the Solar System’s initial water distribution is typical of protoplanetary disks in the Galaxy. The starting iron contents of protoplanets are interpolated between the values f ...
Regular Keplerian motions in classical many-body
... an arbitrary mass, being placed halfway between the bodies of equal masses, influences their motion because of an additional gravitational pull: the net force on either one of the pair is the sum of two gravitational forces (pointing in the same direction), one from the central body and the other fr ...
... an arbitrary mass, being placed halfway between the bodies of equal masses, influences their motion because of an additional gravitational pull: the net force on either one of the pair is the sum of two gravitational forces (pointing in the same direction), one from the central body and the other fr ...
Science Across Disciplines
... birth of a new field of astronomy: the study of extrasolar planetary systems around main sequence stars. Since then, more than 200 planets outside our own Solar System have been discovered. These planets most closely resemble the gas giant planets, with masses in the range 20 – 3 000 M ⊕, but many o ...
... birth of a new field of astronomy: the study of extrasolar planetary systems around main sequence stars. Since then, more than 200 planets outside our own Solar System have been discovered. These planets most closely resemble the gas giant planets, with masses in the range 20 – 3 000 M ⊕, but many o ...
Voyage of Discovery - MESSENGER Education
... There are two basic types of planets. Earth-like (“terrestrial”) planets—Mercury, Venus, Earth, and Mars—are small, dense, rocky worlds. They all have solid surfaces and are located in the inner part of the Solar System. Jupiter-like (“Jovian”) planets—Jupiter, Saturn, Uranus and Neptune—are large p ...
... There are two basic types of planets. Earth-like (“terrestrial”) planets—Mercury, Venus, Earth, and Mars—are small, dense, rocky worlds. They all have solid surfaces and are located in the inner part of the Solar System. Jupiter-like (“Jovian”) planets—Jupiter, Saturn, Uranus and Neptune—are large p ...
Solar System
... jects that orbit the Sun directly, the largest eight are the wind; it extends out to the edge of the scattered disc. The planets,[lower-alpha 3] with the remainder being significantly Oort cloud, which is thought to be the source for longsmaller objects, such as dwarf planets and small Solar period c ...
... jects that orbit the Sun directly, the largest eight are the wind; it extends out to the edge of the scattered disc. The planets,[lower-alpha 3] with the remainder being significantly Oort cloud, which is thought to be the source for longsmaller objects, such as dwarf planets and small Solar period c ...
ISA_lecture01 - School of Physics
... A “planet” is a celestial body that (a) is in orbit around the Sun, (b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and (c) has cleared the neighbourhood around its orbit. A “dwarf planet” is a celestial bo ...
... A “planet” is a celestial body that (a) is in orbit around the Sun, (b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and (c) has cleared the neighbourhood around its orbit. A “dwarf planet” is a celestial bo ...
- ANU Repository
... There have been several recent works estimating the occurrence of planets around M dwarfs, the distribution with radii, and the number of planets within a ‘habitable zone’ (HZ) bounded by minimum and maximum irradiance levels. Both Dressing & Charbonneau (2013, hereafter, DC13) and Gaidos (2013, her ...
... There have been several recent works estimating the occurrence of planets around M dwarfs, the distribution with radii, and the number of planets within a ‘habitable zone’ (HZ) bounded by minimum and maximum irradiance levels. Both Dressing & Charbonneau (2013, hereafter, DC13) and Gaidos (2013, her ...
Slides - Geophysical Sciences
... The Kuiper Belt started with higher mass that was scattered by the planets’ changing orbits The resonance moves the planets into higher e, i orbits Compton Lectures – Autumn 2012 ...
... The Kuiper Belt started with higher mass that was scattered by the planets’ changing orbits The resonance moves the planets into higher e, i orbits Compton Lectures – Autumn 2012 ...
observations of white dwarfs in the solar neighborhood
... and June 22. We used the SITE 2048 2048 CCD and the 600 line mm1 grating to obtain a spectral range of 4210– 7560 Å with substantial vignetting toward the ends of this range. The 100 slit gave 3.2 Å spectral resolution (FWHM). The main observing program was focused on accurate radial velocitie ...
... and June 22. We used the SITE 2048 2048 CCD and the 600 line mm1 grating to obtain a spectral range of 4210– 7560 Å with substantial vignetting toward the ends of this range. The 100 slit gave 3.2 Å spectral resolution (FWHM). The main observing program was focused on accurate radial velocitie ...
CHEOPS Science Requirements Document
... confirmed. We have learned that planets are quite common, and that their properties are much more diverse than originally predicted (Udry et al. 2007). We have even witnessed the first few direct detections and analysis of their atmospheres in recent years. These pioneering measurements, previously ...
... confirmed. We have learned that planets are quite common, and that their properties are much more diverse than originally predicted (Udry et al. 2007). We have even witnessed the first few direct detections and analysis of their atmospheres in recent years. These pioneering measurements, previously ...
White dwarfs from GAIA: The 7th dimension
... •A maximum likelihood analysis can differentiate between the different luminosity functions, and hence reconstruct the star formation history. •Massive white dwarfs have a negligible MS+RGC+AGB lifetime ...
... •A maximum likelihood analysis can differentiate between the different luminosity functions, and hence reconstruct the star formation history. •Massive white dwarfs have a negligible MS+RGC+AGB lifetime ...
Powerpoint Presentation (large file)
... 1. How did Uranus and Neptune come to be discovered? 2. What gives Uranus its distinctive greenish-blue color? 3. Why are the clouds on Neptune so much more visible than those on Uranus? 4. Are Uranus and Neptune merely smaller versions of Jupiter and Saturn? 5. What is so unusual about the magnetic ...
... 1. How did Uranus and Neptune come to be discovered? 2. What gives Uranus its distinctive greenish-blue color? 3. Why are the clouds on Neptune so much more visible than those on Uranus? 4. Are Uranus and Neptune merely smaller versions of Jupiter and Saturn? 5. What is so unusual about the magnetic ...
MEarth
... collapse or to steep temperature gradients and climatic conditions not suitable for life. Works reviewed in Scalo et al. and Tarter et al. argue that atmospheric heat circulation should prevent each of these barriers to habitability. Regardless, the absence of such heat redistribution would be readi ...
... collapse or to steep temperature gradients and climatic conditions not suitable for life. Works reviewed in Scalo et al. and Tarter et al. argue that atmospheric heat circulation should prevent each of these barriers to habitability. Regardless, the absence of such heat redistribution would be readi ...
Making More Terrestrial Planets
... as a result of strong secular perturbations from the giant planets, which peak at the ν6 resonance at 2.1 AU. Objects in the ν6 resonance experience large, chaotic oscillations in e. These oscillations are driven by the coincidence of the rate of precession of the orbit’s longitude of perihelion wit ...
... as a result of strong secular perturbations from the giant planets, which peak at the ν6 resonance at 2.1 AU. Objects in the ν6 resonance experience large, chaotic oscillations in e. These oscillations are driven by the coincidence of the rate of precession of the orbit’s longitude of perihelion wit ...
Final Unit Plan
... moons or satellites (Cessna, 2009). Jupiter is often referred to as the prototype for Jovian planets, and is also the largest planet in the solar system. Its brightness can be viewed from earth with the naked eye. Although Jupiter is not known for beautiful rings, it, like all other Jovian planets, ...
... moons or satellites (Cessna, 2009). Jupiter is often referred to as the prototype for Jovian planets, and is also the largest planet in the solar system. Its brightness can be viewed from earth with the naked eye. Although Jupiter is not known for beautiful rings, it, like all other Jovian planets, ...
The Occurrence and Architecture of Exoplanetary Systems
... of the Solar System with a list of observations similar to the one provided above. Many authors of such articles have expressed a wish to have the same type of information for other planetary systems. In a representative example, Williams & Cremin (1968) wrote, “It is difficult to decide whether all ...
... of the Solar System with a list of observations similar to the one provided above. Many authors of such articles have expressed a wish to have the same type of information for other planetary systems. In a representative example, Williams & Cremin (1968) wrote, “It is difficult to decide whether all ...
McDonald I....Tisserand, P. et al ExELS an
... (Marshall et al. 2005). The populations included in the model are such that stars are limited to between 0.08 and 4 M (B–M type stars). No transiting planets have yet been found around stars outside this range and the proposed target area does not include large or young open clusters or star-formin ...
... (Marshall et al. 2005). The populations included in the model are such that stars are limited to between 0.08 and 4 M (B–M type stars). No transiting planets have yet been found around stars outside this range and the proposed target area does not include large or young open clusters or star-formin ...
The scattering of small bodies in planetary systems
... The scattering of small bodies by planets is an important dynamical process in planetary systems. In this paper we present an analytical model to describe this process using the simplifying assumption that each particle’s dynamics is dominated by a single planet at a time. As such the scattering pro ...
... The scattering of small bodies by planets is an important dynamical process in planetary systems. In this paper we present an analytical model to describe this process using the simplifying assumption that each particle’s dynamics is dominated by a single planet at a time. As such the scattering pro ...
planet migration in planetesimal disks
... to that of Neptune (aUra /aNep). It can be evaluated using a Monte Carlo method, if the assumption used to derive Equation 5 is again made. The colored curves in Figure 1 show the results for five different values of aUra /aNep . Currently aUra /aNep = 0.64 (orange curve). Figure 1 shows that if aUr ...
... to that of Neptune (aUra /aNep). It can be evaluated using a Monte Carlo method, if the assumption used to derive Equation 5 is again made. The colored curves in Figure 1 show the results for five different values of aUra /aNep . Currently aUra /aNep = 0.64 (orange curve). Figure 1 shows that if aUr ...
Voyage of Discovery - Journey through the Universe
... Solar System in a Nutshell The major components of the Solar System are the Sun and the eight planets revolving around it. The Solar System also includes the moons of the planets, asteroids, comets, dwarf planets, and small icy bodies beyond Neptune. The Solar System is truly the family of the Sun. ...
... Solar System in a Nutshell The major components of the Solar System are the Sun and the eight planets revolving around it. The Solar System also includes the moons of the planets, asteroids, comets, dwarf planets, and small icy bodies beyond Neptune. The Solar System is truly the family of the Sun. ...
final stages of planet formation
... suffer collisions at velocities v H that we assume are sufficient to fragment them. 3. We note that tiso as used by us measures the duration of the final doubling of an oligarch’s mass. It may be much smaller than the duration of orderly or runaway growth, or even the initial phase of oligarchy. Th ...
... suffer collisions at velocities v H that we assume are sufficient to fragment them. 3. We note that tiso as used by us measures the duration of the final doubling of an oligarch’s mass. It may be much smaller than the duration of orderly or runaway growth, or even the initial phase of oligarchy. Th ...
Evidence from the asteroid belt for a violent past evolution of
... migrate through the disk by scattering planetesimals and leaving them “behind” relative to its migration direction. In this case, the migration speed does not slow down with time: it actually accelerates (until some saturation or migration reversal point is hit). So, obviously, a formula like (3) do ...
... migrate through the disk by scattering planetesimals and leaving them “behind” relative to its migration direction. In this case, the migration speed does not slow down with time: it actually accelerates (until some saturation or migration reversal point is hit). So, obviously, a formula like (3) do ...
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.