The Early Evolution of Solids in Protoplanetary Disks
... of planets. According to the core accretion scenario, the formation of planets involves a variety of physical mechanisms starting from the coagulation of sub-µm sized particles and going up to the gas-accretion phase leading to the build up of rocky planets and gas giants. The first stages of this p ...
... of planets. According to the core accretion scenario, the formation of planets involves a variety of physical mechanisms starting from the coagulation of sub-µm sized particles and going up to the gas-accretion phase leading to the build up of rocky planets and gas giants. The first stages of this p ...
Planetary Systems and Planets in Systems (pdf file 10.5
... trend that remains after the discovery of now more than about 100 planets. Current results also point out that the planetary frequency is rising as a function of the [Fe/H]. Furthermore, the source of this high metallicity is shown to have most probably an “original” source, although there are also ...
... trend that remains after the discovery of now more than about 100 planets. Current results also point out that the planetary frequency is rising as a function of the [Fe/H]. Furthermore, the source of this high metallicity is shown to have most probably an “original” source, although there are also ...
Strongly suggested reading: The Milky Way`s stellar disk
... presumably has to await Gaia. In addition there is a second aspect of non-axisymmetric substructure, which is known to be present in the Disk, but which is far from being sensibly characterized: there are groups of chemically similar stars on similar but very unusual orbits (streams, e.g., Helmi et ...
... presumably has to await Gaia. In addition there is a second aspect of non-axisymmetric substructure, which is known to be present in the Disk, but which is far from being sensibly characterized: there are groups of chemically similar stars on similar but very unusual orbits (streams, e.g., Helmi et ...
Protoplanetary Disks and their Evolution
... Levy & Lunine 1993; Mannings et al. 2000; Reipurth et al. 2005). There are also several related reviews that have also been recently written for this series including the inner disk (Dullemond & Monnier 2010), debris disks (Wyatt 2008), and dynamical processes (Armitage 2011). This review focuses on ...
... Levy & Lunine 1993; Mannings et al. 2000; Reipurth et al. 2005). There are also several related reviews that have also been recently written for this series including the inner disk (Dullemond & Monnier 2010), debris disks (Wyatt 2008), and dynamical processes (Armitage 2011). This review focuses on ...
The HARPS search for southern extra-solar planets
... – After 4 years of the HARPS survey (Mayor et al. 2003), the number of low-mass planets detected was large enough to allow for a preliminary analysis of the statistical properties of this specific population (Udry & Santos 2007; Mayor & Udry 2008). The mass distribution of small-mass planets was fou ...
... – After 4 years of the HARPS survey (Mayor et al. 2003), the number of low-mass planets detected was large enough to allow for a preliminary analysis of the statistical properties of this specific population (Udry & Santos 2007; Mayor & Udry 2008). The mass distribution of small-mass planets was fou ...
Circumstellar dust emission from nearby Solar
... Today β Pictoris is considered to be a young star on the main sequence (spectral class A6 V) with indications that planet formation is still ongoing (Zuckerman et al. 2001; Wahhaj et al. 2003). Furthermore, Lagrange et al. (2009) were able to directly image a giant planet using the Very Large Telesc ...
... Today β Pictoris is considered to be a young star on the main sequence (spectral class A6 V) with indications that planet formation is still ongoing (Zuckerman et al. 2001; Wahhaj et al. 2003). Furthermore, Lagrange et al. (2009) were able to directly image a giant planet using the Very Large Telesc ...
Spitzer Spectroscopy of Circumstellar Disks in the 5 Myr Old Upper
... short wavelengths indicating that the inner ∼10 AU are cleared of primordial dust. Such excesses are more analogous to second generation, optically-thin debris disks produced by the collision of planetesimals. Of particular interest, none of the ∼30 F or G-type stars (1.2– 1.8 M⊙ ) included in the S ...
... short wavelengths indicating that the inner ∼10 AU are cleared of primordial dust. Such excesses are more analogous to second generation, optically-thin debris disks produced by the collision of planetesimals. Of particular interest, none of the ∼30 F or G-type stars (1.2– 1.8 M⊙ ) included in the S ...
Dissertation in Astronomy submitted to the Combined
... – observed by the Kepler telescope – was initiated to unveil a population of close-in planets (a < 0.5 au) that have been undetected by previous RV surveys. This e↵ort led to the confirmation of the planetary nature of two close-in planets, Kepler-432 b and Kepler-91 b, providing evidence that short ...
... – observed by the Kepler telescope – was initiated to unveil a population of close-in planets (a < 0.5 au) that have been undetected by previous RV surveys. This e↵ort led to the confirmation of the planetary nature of two close-in planets, Kepler-432 b and Kepler-91 b, providing evidence that short ...
A Decade of Radial-Velocity Discoveries in the Exoplanet Domain
... mlim and orbital periods shorter than Plim. The minimum rate is obtained just by counting the fraction of stars hosting planets in this particular slice of parameter space. For planets more massive than 0.5 MJup, Marcy et al. (2005) find in the Lick+Keck+AAT sample that 16/1330 = 1.2% of the stars h ...
... mlim and orbital periods shorter than Plim. The minimum rate is obtained just by counting the fraction of stars hosting planets in this particular slice of parameter space. For planets more massive than 0.5 MJup, Marcy et al. (2005) find in the Lick+Keck+AAT sample that 16/1330 = 1.2% of the stars h ...
Evolution of the Milky Way with radial motions of stars and gas
... such coefficients from the simulation of an early-type barred disk and, applying them in a semi-analytical model of that same disk, they showed that all the main features of the N-body+SPH simulation can be reproduced to a good accuracy. They also showed that radial migration moves around not only “pa ...
... such coefficients from the simulation of an early-type barred disk and, applying them in a semi-analytical model of that same disk, they showed that all the main features of the N-body+SPH simulation can be reproduced to a good accuracy. They also showed that radial migration moves around not only “pa ...
Extra-solar planets
... orbits the Sun (0.39 AU). While the Doppler technique preferentially selects systems in tight orbits, giant planets so close to the parent star were generally unexpected. Theoretical progress in understanding their formation and their properties has been rapid, but it remains far from complete. ‡ Ba ...
... orbits the Sun (0.39 AU). While the Doppler technique preferentially selects systems in tight orbits, giant planets so close to the parent star were generally unexpected. Theoretical progress in understanding their formation and their properties has been rapid, but it remains far from complete. ‡ Ba ...
The distributions and ages of refractory objects in the solar nebula
... 0.1–1 cm sized objects, such as the large CAIs, would have drift inwards at rates of 1–10 cm/s. Thus CAIs would drift inward from 2 AU (the inner edge of the asteroid belt) to the inner edge of the disk in as little as 105 years. Two primary models have been invoked to explain how CAIs were not on ...
... 0.1–1 cm sized objects, such as the large CAIs, would have drift inwards at rates of 1–10 cm/s. Thus CAIs would drift inward from 2 AU (the inner edge of the asteroid belt) to the inner edge of the disk in as little as 105 years. Two primary models have been invoked to explain how CAIs were not on ...
Extra-solar planets
... expected. More than one-third have significantly elliptical orbits, with e > 0.3, compared with the largest eccentricities in our solar system, of about 0.2 for Mercury and Pluto and 0.05 for Jupiter. Even more significantly, about two-thirds are orbiting their host star much closer than Mercury orb ...
... expected. More than one-third have significantly elliptical orbits, with e > 0.3, compared with the largest eccentricities in our solar system, of about 0.2 for Mercury and Pluto and 0.05 for Jupiter. Even more significantly, about two-thirds are orbiting their host star much closer than Mercury orb ...
Understanding Resolution
... star has an affect on the appearance of the Airy disk. A very bright star puts so much light into the central disk that the disk itself may take up 85% of the Airy disk diameter. The central disk of a faint star may take up less than 50% of the Airy disk diameter, leaving more dark space in the firs ...
... star has an affect on the appearance of the Airy disk. A very bright star puts so much light into the central disk that the disk itself may take up 85% of the Airy disk diameter. The central disk of a faint star may take up less than 50% of the Airy disk diameter, leaving more dark space in the firs ...
Galactic planetary science
... in reality, the presence of a host star is not even a mandatory circumstance. The current statistical estimates indicate that, on average, every star in our Galaxy hosts at least one planetary companion [1], i.e. our Milky Way is crowded with one hundred billion planets. The most revolutionary aspec ...
... in reality, the presence of a host star is not even a mandatory circumstance. The current statistical estimates indicate that, on average, every star in our Galaxy hosts at least one planetary companion [1], i.e. our Milky Way is crowded with one hundred billion planets. The most revolutionary aspec ...
Document
... upon disk conditions - but s ~ 1 m is typical… To grow from small scales to planetesimals via pairwise collisions cannot avoid passing through this stage ...
... upon disk conditions - but s ~ 1 m is typical… To grow from small scales to planetesimals via pairwise collisions cannot avoid passing through this stage ...
Detecting Exoplanets Talk
... • This method is most sensitive for very massive and close-in planets. • Thus, it selects for hot Jupiters. • Here is a nice video showing the shifting spectral lines on which the measurements are based: http://vimeo.com/14390954 • It also, as noted before, gives lower limits on mass (M sin i). • Th ...
... • This method is most sensitive for very massive and close-in planets. • Thus, it selects for hot Jupiters. • Here is a nice video showing the shifting spectral lines on which the measurements are based: http://vimeo.com/14390954 • It also, as noted before, gives lower limits on mass (M sin i). • Th ...
Exoplanet Detection Techniques - Lunar and Planetary Laboratory
... Figure 2, reproduced from Pepe et al. (2011), shows an example of one of the lowest amplitude exoplanets, detected with HARPS. The velocity semi-amplitude for this planet is K = 0.769 m s−1 and the orbital period is 58.43 days. The data was comprised of 185 observations spanning 7.5 years. The resid ...
... Figure 2, reproduced from Pepe et al. (2011), shows an example of one of the lowest amplitude exoplanets, detected with HARPS. The velocity semi-amplitude for this planet is K = 0.769 m s−1 and the orbital period is 58.43 days. The data was comprised of 185 observations spanning 7.5 years. The resid ...
Detecting Extrasolar Moons akin to Solar System Satellites with an
... that do not contribute to the OSE because of planetmoon eclipses. This masking can only occur during the planetary transit when |xp (t)| ≤ R⋆ . Note that partial planet-moon eclipses as well as moon-moon eclipses are ignored (but treated by Kipping 2011a). In this model, the ingress and egress of th ...
... that do not contribute to the OSE because of planetmoon eclipses. This masking can only occur during the planetary transit when |xp (t)| ≤ R⋆ . Note that partial planet-moon eclipses as well as moon-moon eclipses are ignored (but treated by Kipping 2011a). In this model, the ingress and egress of th ...
Characterization of exoplanetary systems with the direct
... In the year of the 20th anniversary of the discovery of the first extrasolar planet we can count more than 1800 companions found with different techniques. The majority of them are indirect methods that infer the presence of an orbiting body by observing the parent star (radial velocity, transits, a ...
... In the year of the 20th anniversary of the discovery of the first extrasolar planet we can count more than 1800 companions found with different techniques. The majority of them are indirect methods that infer the presence of an orbiting body by observing the parent star (radial velocity, transits, a ...
Scenarios of giant planet formation and evolution and their impact
... isolation from each other. This was possible because Jupiter avoided migrating into the inner Solar System, most probably due to the presence of Saturn, and never acquired a large-eccentricity orbit, even during the phase of orbital instability that the giant planets most likely experienced. Thus, t ...
... isolation from each other. This was possible because Jupiter avoided migrating into the inner Solar System, most probably due to the presence of Saturn, and never acquired a large-eccentricity orbit, even during the phase of orbital instability that the giant planets most likely experienced. Thus, t ...
Exoplanetary Geophysics-
... transit photometry now generates a clear majority of new planetary candidates, and groundbased surveys such as the HAT Net (Bakos et al. 2012) and SuperWASP (Smith et al. 2013), are generating dozens of confirmed planets per year. The preliminary version of the Kepler Q12 planet candidate catalog, c ...
... transit photometry now generates a clear majority of new planetary candidates, and groundbased surveys such as the HAT Net (Bakos et al. 2012) and SuperWASP (Smith et al. 2013), are generating dozens of confirmed planets per year. The preliminary version of the Kepler Q12 planet candidate catalog, c ...
Insights into planet formation from debris disks: II. Giant impacts in
... and Ward 1976; Canup 2004a). Continued work on the giant impact hypothesis eventually resulted in what has become known as the Canonical model (e.g. Canup and Asphaug 2001; Canup 2004b,a), in which a roughly Mars mass body (known as Theia) collides with a nearly fully formed proto-Earth at an obliqu ...
... and Ward 1976; Canup 2004a). Continued work on the giant impact hypothesis eventually resulted in what has become known as the Canonical model (e.g. Canup and Asphaug 2001; Canup 2004b,a), in which a roughly Mars mass body (known as Theia) collides with a nearly fully formed proto-Earth at an obliqu ...
Constraints on Long-Period Planets from an L′ and M band Survey
... We take our normalization instead from the Carnegie Planet Sample, as described in Fischer & Valenti (2005). Their Table 1 (online only) lists 850 stars that have been thoroughly investigated with RV. They state that all planets with mass at least 1 MJup and orbital period less than 4 years have bee ...
... We take our normalization instead from the Carnegie Planet Sample, as described in Fischer & Valenti (2005). Their Table 1 (online only) lists 850 stars that have been thoroughly investigated with RV. They state that all planets with mass at least 1 MJup and orbital period less than 4 years have bee ...
Volatiles in protoplanetary disks
... The solar system was formed from a protoplanetary disk during a time frame of 2-3 million years, spanning ages of at least 4567-4564 Myr – a number known to a high degree of precision, thanks to accurate radiometric dating of primitive meteoritic material formed by gas-condensation processes (Scott ...
... The solar system was formed from a protoplanetary disk during a time frame of 2-3 million years, spanning ages of at least 4567-4564 Myr – a number known to a high degree of precision, thanks to accurate radiometric dating of primitive meteoritic material formed by gas-condensation processes (Scott ...
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.