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 ...
1 Exoplanet Observations - Wiley-VCH
... a much larger number of radial velocity observations than are usually obtained during initial discovery and characterization of planets [30]. Therefore, while the short-period planets certainly have low eccentricities, it is not known precisely to what level their orbits might be noncircular. The se ...
... a much larger number of radial velocity observations than are usually obtained during initial discovery and characterization of planets [30]. Therefore, while the short-period planets certainly have low eccentricities, it is not known precisely to what level their orbits might be noncircular. The se ...
The chemical history of molecules in circumstellar disks I: Ices
... chemical evolution from the pre-stellar core to the protostar and circumstellar disk. The model computes infall trajectories from any point in the cloud core and tracks the radial and vertical motion of material in the viscously evolving disk. It includes a full time-dependent radiative transfer tre ...
... chemical evolution from the pre-stellar core to the protostar and circumstellar disk. The model computes infall trajectories from any point in the cloud core and tracks the radial and vertical motion of material in the viscously evolving disk. It includes a full time-dependent radiative transfer tre ...
Investigation of Extrasolar Planets Using Radial Velocity Technique
... labeled Super-Earths, have also been detected. They are about 5 to 10 Earth’s mass [16]. In 2008, NASA announced the discovery of an Extrasolar planet orbiting just around a star Fomalhaut [17]. This was the first Extrasolar planet to be directly imaged by Hubble Space Telescope. In 2009, Fischer et ...
... labeled Super-Earths, have also been detected. They are about 5 to 10 Earth’s mass [16]. In 2008, NASA announced the discovery of an Extrasolar planet orbiting just around a star Fomalhaut [17]. This was the first Extrasolar planet to be directly imaged by Hubble Space Telescope. In 2009, Fischer et ...
Program and abstracts in one word document
... Dust cloud formation occurs in the atmospheres of very low mass stars and brown dwarfs at gas temperatures of less then 1800K for pressures between 1 and 10 bars, i.e. in the line forming region of these atmospheres. Recently, we have been modeling cloud formation via 2D multi-group Radiation Hydro- ...
... Dust cloud formation occurs in the atmospheres of very low mass stars and brown dwarfs at gas temperatures of less then 1800K for pressures between 1 and 10 bars, i.e. in the line forming region of these atmospheres. Recently, we have been modeling cloud formation via 2D multi-group Radiation Hydro- ...
Abstracts for “Extreme Solar Systems” Talk Abstracts “Pulsar Planets
... to monitor 180,000 stars in the Galactic bulge continuously for 7 days to look for transiting extrasolar planets. The SWEEPS sample represents the farthest such sample, and includes stars down to 0.45 solar mass. We discovered 16 candidates with orbital periods between 0.4 and 4.2 days. In two cases ...
... to monitor 180,000 stars in the Galactic bulge continuously for 7 days to look for transiting extrasolar planets. The SWEEPS sample represents the farthest such sample, and includes stars down to 0.45 solar mass. We discovered 16 candidates with orbital periods between 0.4 and 4.2 days. In two cases ...
Direct Imaging of Radial Velocity Exoplanets
... To observe the eclipse caused by the planet, we, as observers on Earth, need to have an edge-on view of the transit. This method also requires long term observation of the system to determine the orbital period of the exoplanet being observed. Moreover, this method is known for producing many false ...
... To observe the eclipse caused by the planet, we, as observers on Earth, need to have an edge-on view of the transit. This method also requires long term observation of the system to determine the orbital period of the exoplanet being observed. Moreover, this method is known for producing many false ...
9 The Clearing of Protoplanetary Disks and of the Protosolar Nebula
... 9.1.2 Constraints on the dispersal of the gas component The initial mass and lifetime of gas in circumstellar disks affect both the formation of giant planets as well as the formation of terrestrial planets. According to the widely accepted scenario of giant planet formation, rocky cores need to rea ...
... 9.1.2 Constraints on the dispersal of the gas component The initial mass and lifetime of gas in circumstellar disks affect both the formation of giant planets as well as the formation of terrestrial planets. According to the widely accepted scenario of giant planet formation, rocky cores need to rea ...
Evolution in circumstellar envelopes of Be stars: From disks to rings?
... disks of several Be stars. Subtle variations in the wings of optically thin and thick emission lines suggest that the conventional, static picture of the disk being in quasi-contact with the central star is justified primarily (or perhaps only) after an outburst event. Some weeks to months later, a ...
... disks of several Be stars. Subtle variations in the wings of optically thin and thick emission lines suggest that the conventional, static picture of the disk being in quasi-contact with the central star is justified primarily (or perhaps only) after an outburst event. Some weeks to months later, a ...
Astronomy Assignment #8 Exoplanets II
... The regions most populated by exoplanets appear to be 1. Very close to the star with a between .02 and 1.5 AU and with planet masses greater than 63 Earth masses. This is the location of terrestrial planets, but clearly the masses of these planets indicate that they are Jovian planets. 2. Not so clo ...
... The regions most populated by exoplanets appear to be 1. Very close to the star with a between .02 and 1.5 AU and with planet masses greater than 63 Earth masses. This is the location of terrestrial planets, but clearly the masses of these planets indicate that they are Jovian planets. 2. Not so clo ...
Discovery and spectroscopy of the young Jovian planet
... that are bright at young ages – referred to as “hot-start”. Alternatively, two-stage formation, first of a dense solid core followed by gas accretion through a shock, as likely in the case of Jupiter, can produce a range of states including lower-entropy planets that are cooler, and slightly smaller ...
... that are bright at young ages – referred to as “hot-start”. Alternatively, two-stage formation, first of a dense solid core followed by gas accretion through a shock, as likely in the case of Jupiter, can produce a range of states including lower-entropy planets that are cooler, and slightly smaller ...
PDF only - at www.arxiv.org.
... orbiting a G2 V star at 4 AU for ages 0.1–5 Gyr (Burrows et al. 2004). Planets shine by reflected light in the visible. Young exoplanets (< 1 Gyr for 1 MJ) are detectable by their intrinsic luminosity. Note strong J (1.25 µm) and H (1.65 µm) emission where groundbased facilities have sensitive opera ...
... orbiting a G2 V star at 4 AU for ages 0.1–5 Gyr (Burrows et al. 2004). Planets shine by reflected light in the visible. Young exoplanets (< 1 Gyr for 1 MJ) are detectable by their intrinsic luminosity. Note strong J (1.25 µm) and H (1.65 µm) emission where groundbased facilities have sensitive opera ...
Astron 104 Laboratory #9 Cepheid Variable Stars
... actually radiating into space (i.e, how bright it actually is). • The star’s distance from us. In principle, if we know the first two of these quantities, we can calculate the distance. The apparent magnitude is usually easy to measure because all we need to do is use a telescope that has a calibrat ...
... actually radiating into space (i.e, how bright it actually is). • The star’s distance from us. In principle, if we know the first two of these quantities, we can calculate the distance. The apparent magnitude is usually easy to measure because all we need to do is use a telescope that has a calibrat ...
Neutral material around the B[e] supergiant star LHA 115
... We obtained high-resolution optical spectra using the Fiber-fed Extended Range Optical Spectrograph (FEROS), and also lowresolution optical spectra using the Boller & Chivens spectrograph (B&C). The FEROS spectra were obtained in three different years. The oldest one is from 1999 October 27, when the ...
... We obtained high-resolution optical spectra using the Fiber-fed Extended Range Optical Spectrograph (FEROS), and also lowresolution optical spectra using the Boller & Chivens spectrograph (B&C). The FEROS spectra were obtained in three different years. The oldest one is from 1999 October 27, when the ...
minimum mass extrasolar nebula derived from the
... the mean host temperature is approximately between 4500K and 6300K. For comparison the Sun has an effective temperature of about 5777K. Yet, the surface density profiles show 3.3- 3.5 that the Solar system’s mass distribution is quite different from the majority of extrasolar systems explored which ...
... the mean host temperature is approximately between 4500K and 6300K. For comparison the Sun has an effective temperature of about 5777K. Yet, the surface density profiles show 3.3- 3.5 that the Solar system’s mass distribution is quite different from the majority of extrasolar systems explored which ...
Migrating Dust Particles
... size they drifted towards the Sun. This material was later accreted to planetesimals which are held together by self-gravity. As the planetesimals extend their gravitational range they have a run-away growth towards becoming planets. In this step the planetesimals grow more the larger they get. This ...
... size they drifted towards the Sun. This material was later accreted to planetesimals which are held together by self-gravity. As the planetesimals extend their gravitational range they have a run-away growth towards becoming planets. In this step the planetesimals grow more the larger they get. This ...
Lokal fulltext - Chalmers Publication Library
... only in the spectral energy distribution (SED) they could not infer any shape. The excess is beyond 12 µm and peaks close to 60 µm. They interpreted this as emission from solid particles at 85 AU from the star, distributed in either a shell or a ring (see Figure 1.1). Since such excess first was obs ...
... only in the spectral energy distribution (SED) they could not infer any shape. The excess is beyond 12 µm and peaks close to 60 µm. They interpreted this as emission from solid particles at 85 AU from the star, distributed in either a shell or a ring (see Figure 1.1). Since such excess first was obs ...
Dynamical habitability of planetary systems
... with each other. Earth, for example, is in particular disturbed by the massive planet Jupiter and suffers even from being in a 13:7 resonance of the mean motions with the planet Venus. The perturbations are, however, too small to change orbits drastically within timescales of billions of years (see, ...
... with each other. Earth, for example, is in particular disturbed by the massive planet Jupiter and suffers even from being in a 13:7 resonance of the mean motions with the planet Venus. The perturbations are, however, too small to change orbits drastically within timescales of billions of years (see, ...
Debris Disks: Seeing Dust, Thinking of Planetesimals and Planets
... Received 2010 March 5; accepted 2010 March 24 ...
... Received 2010 March 5; accepted 2010 March 24 ...
The spectral characteristics of transiting extrasolar planet Jae
... modelling process and a prediction of spectral transition of an Earth-like extrasolar planet orbiting around Sun-like star is reported. The model allows for atmospheric rotation effects: both stellar and planetary atmosphere rotation. The spectral line broadening caused by the stellar rotation is de ...
... modelling process and a prediction of spectral transition of an Earth-like extrasolar planet orbiting around Sun-like star is reported. The model allows for atmospheric rotation effects: both stellar and planetary atmosphere rotation. The spectral line broadening caused by the stellar rotation is de ...
Observations, Modeling and Theory of Debris Disks
... Universidad Autónoma de Madrid Main sequence stars, like the Sun, are often found to be orbited by circumstellar material that can be categorized into two groups, planets and debris. The latter is made up of asteroids and comets, as well as the dust and gas derived from them, which makes debris dis ...
... Universidad Autónoma de Madrid Main sequence stars, like the Sun, are often found to be orbited by circumstellar material that can be categorized into two groups, planets and debris. The latter is made up of asteroids and comets, as well as the dust and gas derived from them, which makes debris dis ...
Observations, Modeling and Theory of Debris Disks
... Universidad Autónoma de Madrid Main sequence stars, like the Sun, are often found to be orbited by circumstellar material that can be categorized into two groups, planets and debris. The latter is made up of asteroids and comets, as well as the dust and gas derived from them, which makes debris dis ...
... Universidad Autónoma de Madrid Main sequence stars, like the Sun, are often found to be orbited by circumstellar material that can be categorized into two groups, planets and debris. The latter is made up of asteroids and comets, as well as the dust and gas derived from them, which makes debris dis ...
thick disk - asteroSTEP
... The old thick disk is a very significant component for studying Galaxy formation, because it presents a kinematically and chemically recognizable relic of the early Galaxy. Secular heating is unlikely to affect its dynamics significantly, because its stars spend most of their time away from the Gal ...
... The old thick disk is a very significant component for studying Galaxy formation, because it presents a kinematically and chemically recognizable relic of the early Galaxy. Secular heating is unlikely to affect its dynamics significantly, because its stars spend most of their time away from the Gal ...
OGLE-TR-211 - Repositorio Académico
... Spectroscopic follow-up observations of the OGLE Campaign #5 transit candidates were carried out during three observing slots allocated to the LP666 program in April/May 2006, February 2007 and April 2007 on VLT with the FLAMES spectrograph. Also, part of the Geneva group observing time under progra ...
... Spectroscopic follow-up observations of the OGLE Campaign #5 transit candidates were carried out during three observing slots allocated to the LP666 program in April/May 2006, February 2007 and April 2007 on VLT with the FLAMES spectrograph. Also, part of the Geneva group observing time under progra ...
The Circumstellar Environments of Young Stars at AU Scales
... part to explain the NIR interferometer measurements. The outline of this review is as follows. Sections 2 and 3 summarize the observational state of the art and emerging interpretations, drawing a physically motivated distinction between inner and outer disk regions that also naturally addresses dis ...
... part to explain the NIR interferometer measurements. The outline of this review is as follows. Sections 2 and 3 summarize the observational state of the art and emerging interpretations, drawing a physically motivated distinction between inner and outer disk regions that also naturally addresses dis ...
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.