
THE 2MASS WIDE-FIELD T DWARF SEARCH. II. DISCOVERY OF
... Adam J. Burgasser,1,2 Michael W. McElwain,1 and J. Davy Kirkpatrick3 Received 2003 June 10; accepted 2003 July 22 ...
... Adam J. Burgasser,1,2 Michael W. McElwain,1 and J. Davy Kirkpatrick3 Received 2003 June 10; accepted 2003 July 22 ...
CHEOPS Definition Study Report
... Immediately after the selection, ESA carried out an internal study, which set the basis for the definition of the mission science requirements, the system requirements for satellite and payload, and the preparation of the Invitation to Tender (ITT) for the ESA industrial activities. The ITT was issu ...
... Immediately after the selection, ESA carried out an internal study, which set the basis for the definition of the mission science requirements, the system requirements for satellite and payload, and the preparation of the Invitation to Tender (ITT) for the ESA industrial activities. The ITT was issu ...
The properties of a spectroscopically selected sample of cataclysmic variables Amornrat Aungwerojwit
... of cataclysmic variable (CV) evolution with relatively few modifications. The predictions made by this theory, however, are in strong disagreement with the observations. These discrepancies may, at least in part, be related to observational selection effects. In order to circumvent observational bia ...
... of cataclysmic variable (CV) evolution with relatively few modifications. The predictions made by this theory, however, are in strong disagreement with the observations. These discrepancies may, at least in part, be related to observational selection effects. In order to circumvent observational bia ...
On the Migratory Behavior of Planetary Systems The Harvard
... underwent a period of upheaval, during which giant planets “migrated” from where they formed. This thesis addresses a question key to understanding how planetary systems evolve: is planetary migration typically a smooth, disk-driven process or a violent process involving strong multi-body gravitatio ...
... underwent a period of upheaval, during which giant planets “migrated” from where they formed. This thesis addresses a question key to understanding how planetary systems evolve: is planetary migration typically a smooth, disk-driven process or a violent process involving strong multi-body gravitatio ...
Trans-Neptunian Objects as Natural Probes to the Unknown Solar System
... dynamically and chemically evolved protoplanetary disk composed of billions of planetesimals, the building blocks from which the planets formed during the early solar system. Consequently, the study of the physical and dynamical properties of TNOs can reveal important clues about the properties of t ...
... dynamically and chemically evolved protoplanetary disk composed of billions of planetesimals, the building blocks from which the planets formed during the early solar system. Consequently, the study of the physical and dynamical properties of TNOs can reveal important clues about the properties of t ...
4373 - Zuber, M. T., H. Y. McSween Jr., R. P. Binzel, L. T. Elkins
... contribute to grain growth (Lunine 1997). The basic idea is that infall and rotation of the turbulent, protosolar molecular cloud caused flattening to a disk (cf. Weidenschilling and Cuzzi 1993). Dust grains from the protoplanetary disk collide, stick together and form clumps that progressively grow ...
... contribute to grain growth (Lunine 1997). The basic idea is that infall and rotation of the turbulent, protosolar molecular cloud caused flattening to a disk (cf. Weidenschilling and Cuzzi 1993). Dust grains from the protoplanetary disk collide, stick together and form clumps that progressively grow ...
New Extreme Trans-Neptunian Objects: Towards a Super
... Extreme trans-Neptunian objects (ETNOs) have orbits that are not easily explained through the currently observed solar system configuration. Objects like Sedna and 2012 VP113 are the two most prominent members of the ETNOs (Trujillo and Sheppard 2014). Their large perihelia of 76 and 80 AU respectiv ...
... Extreme trans-Neptunian objects (ETNOs) have orbits that are not easily explained through the currently observed solar system configuration. Objects like Sedna and 2012 VP113 are the two most prominent members of the ETNOs (Trujillo and Sheppard 2014). Their large perihelia of 76 and 80 AU respectiv ...
The Dynamical History of Chariklo and its Rings
... et al. (2016) the minimum distance obtained between Chariklo and a planet during a close encounter must be ≤ 10Rtd in order for the encounter to have a significant effect on the rings. We will refer to this distance as the ’ring limit’, R. They considered the effect ‘noticeable’ if the maximum chang ...
... et al. (2016) the minimum distance obtained between Chariklo and a planet during a close encounter must be ≤ 10Rtd in order for the encounter to have a significant effect on the rings. We will refer to this distance as the ’ring limit’, R. They considered the effect ‘noticeable’ if the maximum chang ...
Pebble Accretion and the Diversity of Planetary Systems
... where P and a are the orbital period and semi-major axis, M is the mass of the perturbing embryo, ∆a is the orbital separation, rH = ha is the mutual Hill radius, and PVS is given by Ohtsuki et al. (2002). In addition to altering the eccentricities and inclinations of nearby planetesimals, embryos c ...
... where P and a are the orbital period and semi-major axis, M is the mass of the perturbing embryo, ∆a is the orbital separation, rH = ha is the mutual Hill radius, and PVS is given by Ohtsuki et al. (2002). In addition to altering the eccentricities and inclinations of nearby planetesimals, embryos c ...
White dwarf binary
... Low-mass stars with < 2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as carbon white dwarfs Very low-mass stars with < 0.5MSun never become hot enough to fuse helium nuclei, and end as helium white ...
... Low-mass stars with < 2MSun have long lives, never become hot enough to fuse carbon nuclei, and end as carbon white dwarfs Very low-mass stars with < 0.5MSun never become hot enough to fuse helium nuclei, and end as helium white ...
Chap2-RadialVelocity
... Spectrum of a star obtained using the HARPS instrument on the ESO 3.6-metre telescope at the La Silla Observatory in Chile. The lines are the light from the star spread out through various orders. The dark gaps in the lines are absorption features from different elements in the star. The regularly s ...
... Spectrum of a star obtained using the HARPS instrument on the ESO 3.6-metre telescope at the La Silla Observatory in Chile. The lines are the light from the star spread out through various orders. The dark gaps in the lines are absorption features from different elements in the star. The regularly s ...
Chapter 21 A Family of Planets
... much larger than the distance between Mars and Earth. The figure below shows the orbits of the outer planets. ...
... much larger than the distance between Mars and Earth. The figure below shows the orbits of the outer planets. ...
Worlds Beyond: A Strategy for the Detection and Characterization of
... 10H would require unusually high atomic or molecular absorption. Also, the calculations used µ = 18 amu, the value for water vapor, but the pressure is likely to be dominated by heavier species. Both of these choices cause the signal to be larger than expected for an Earthlike planet. In addition, d ...
... 10H would require unusually high atomic or molecular absorption. Also, the calculations used µ = 18 amu, the value for water vapor, but the pressure is likely to be dominated by heavier species. Both of these choices cause the signal to be larger than expected for an Earthlike planet. In addition, d ...
Super-Earth and Sub-Neptune Exoplanets: a First Look from the
... place where photosynthesis happens, and it carries that message with it as it departs the Solar System, broadcasting into the cosmos that our planet teems with life. If global photosynthetic life thrives on an extrasolar planet, we might be able to detect it. A large telescope, equipped with a sensi ...
... place where photosynthesis happens, and it carries that message with it as it departs the Solar System, broadcasting into the cosmos that our planet teems with life. If global photosynthetic life thrives on an extrasolar planet, we might be able to detect it. A large telescope, equipped with a sensi ...
The Exploration of Neptune and Triton
... cryovolcanic in origin (see Croft et al., 1995), and are likely formed by the same complex interaction between tidal dissipation, heat transfer, and tectonics that drives resurfacing on Europa, Ganymede, and Enceladus. However, Voyager’s limited coverage and spatial resolution prevents us from unrav ...
... cryovolcanic in origin (see Croft et al., 1995), and are likely formed by the same complex interaction between tidal dissipation, heat transfer, and tectonics that drives resurfacing on Europa, Ganymede, and Enceladus. However, Voyager’s limited coverage and spatial resolution prevents us from unrav ...
Dawes Review. The tidal downsizing hypothesis of planet formation
... not accrete more gas in this picture. They may actually loose most of their primordial gas if tidal forces from the host stars are stronger than self-gravity of the clumps. However, before the clumps are destroyed, solid planetary cores are formed inside them when grains grow and sediment to the cen ...
... not accrete more gas in this picture. They may actually loose most of their primordial gas if tidal forces from the host stars are stronger than self-gravity of the clumps. However, before the clumps are destroyed, solid planetary cores are formed inside them when grains grow and sediment to the cen ...
Icarus Origin of the structure of the Kuiper belt during a... orbits of Uranus and Neptune
... was needed in order for the KBOs to accrete where we see them. In particular, the growth of these objects within a reasonable time (107 –108 My) requires the existence of about 10 to 30 M ⊕ of solid material in a dynamically cold disk (Stern, 1996; Stern and Colwell, 1997a, 1997b; Kenyon and Luu, 19 ...
... was needed in order for the KBOs to accrete where we see them. In particular, the growth of these objects within a reasonable time (107 –108 My) requires the existence of about 10 to 30 M ⊕ of solid material in a dynamically cold disk (Stern, 1996; Stern and Colwell, 1997a, 1997b; Kenyon and Luu, 19 ...
Full Program with Abstracts - CIERA
... 100.04 – Kepler & K2: One spacecraft, Two Missions This year, we mark twenty years of exploring the diversity of planets and planetary systems orbiting main sequence stars. Exoplanet discoveries spill into the thousands, and the sensitivity boundaries continue to expand. NASA's Kepler Mission unveil ...
... 100.04 – Kepler & K2: One spacecraft, Two Missions This year, we mark twenty years of exploring the diversity of planets and planetary systems orbiting main sequence stars. Exoplanet discoveries spill into the thousands, and the sensitivity boundaries continue to expand. NASA's Kepler Mission unveil ...
Measuring distances to the edge of the local group
... Scientific Justification Be sure to include overall significance to astronomy. For standard proposals limit text to one page with figures, captions and references on no more than two additional pages. We propose to measure the distance to the nearby dwarf irregular galaxies Sextans A, B, and NGC 310 ...
... Scientific Justification Be sure to include overall significance to astronomy. For standard proposals limit text to one page with figures, captions and references on no more than two additional pages. We propose to measure the distance to the nearby dwarf irregular galaxies Sextans A, B, and NGC 310 ...
Origin of the Structure of the Kuiper Belt during a Dynamical
... properties of the Kuiper belt seem to be explained, at least qualitatively. Therefore, is there any need to re-investigate the problem? We think that the answer is yes, for at least three reasons. First, the idea that both the cold and the hot populations formed closer to the Sun and were transporte ...
... properties of the Kuiper belt seem to be explained, at least qualitatively. Therefore, is there any need to re-investigate the problem? We think that the answer is yes, for at least three reasons. First, the idea that both the cold and the hot populations formed closer to the Sun and were transporte ...
Chaos in the Solar System
... two-body problems is an excellent starting approximation. Using their “Keplerian” orbits, one can calculate a first approximation to their forces on each other. Successive iterations of that procedure, carried out with great sophistication, are the techniques called celestial mechanics. The classic ...
... two-body problems is an excellent starting approximation. Using their “Keplerian” orbits, one can calculate a first approximation to their forces on each other. Successive iterations of that procedure, carried out with great sophistication, are the techniques called celestial mechanics. The classic ...
CAPTURE OF IRREGULAR SATELLITES DURING PLANETARY
... the dynamically excited orbits of the outer planets caused a severe depletion of the planetesimal disks at 20Y35 AU and that a fraction of these planetesimals evolved into the inner solar system, producing the LHB. To study (2), we use the LHB variant of the Nice model taken from Gomes et al. (2005) ...
... the dynamically excited orbits of the outer planets caused a severe depletion of the planetesimal disks at 20Y35 AU and that a fraction of these planetesimals evolved into the inner solar system, producing the LHB. To study (2), we use the LHB variant of the Nice model taken from Gomes et al. (2005) ...
Kepler Mission
... detecting other planets. Tests carried out with these photodiodes informed scientists that they had very high precision. However, they still needed to be cooled to near liquid nitrogen temperatures in order to minimize thermal noise. They linked one cooled photometer with the cooled diodes and left ...
... detecting other planets. Tests carried out with these photodiodes informed scientists that they had very high precision. However, they still needed to be cooled to near liquid nitrogen temperatures in order to minimize thermal noise. They linked one cooled photometer with the cooled diodes and left ...
Long-term monitoring of the short period SU UMa
... system. This is well explained by a phase-dependent dissipation of a tidally deformed precessing accretion disk. The most acceptable model for SU UMa stars is the thermaltidal instability model developed by Osaki (1989), well reproducing the majority of observations. V844 Her was discovered by Antip ...
... system. This is well explained by a phase-dependent dissipation of a tidally deformed precessing accretion disk. The most acceptable model for SU UMa stars is the thermaltidal instability model developed by Osaki (1989), well reproducing the majority of observations. V844 Her was discovered by Antip ...
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.