Searching for Planets Around Other Stars
... If you are viewing the star when this happens, you will see the brightness of the star decrease because the planet is blocking it. ...
... If you are viewing the star when this happens, you will see the brightness of the star decrease because the planet is blocking it. ...
Disk Instability Models
... Heretical Explanation for Microlensing Planets • Most stars form in regions of high-mass star formation (e.g., Orion, Carina) where their protoplanetary disks can be photoevaporated away by nearby O stars. • Photoevaporation converts gas giant protoplanets into ice giants if the protoplanet orbit ...
... Heretical Explanation for Microlensing Planets • Most stars form in regions of high-mass star formation (e.g., Orion, Carina) where their protoplanetary disks can be photoevaporated away by nearby O stars. • Photoevaporation converts gas giant protoplanets into ice giants if the protoplanet orbit ...
Great Migrations & other natural history tales
... (the work on MRI is ongoing… also on whether the disks have sufficient ionization for MRI). ...
... (the work on MRI is ongoing… also on whether the disks have sufficient ionization for MRI). ...
Extra-Solar Planets
... Detecting Other Planetary Systems For 50 years, astronomers have been looking for planets around other stars. Since planets are at least 100,000,000 times fainter than stars (because all they do is reflect a bit of the star’s light), direct detection is not (yet) possible. But planets can be found ...
... Detecting Other Planetary Systems For 50 years, astronomers have been looking for planets around other stars. Since planets are at least 100,000,000 times fainter than stars (because all they do is reflect a bit of the star’s light), direct detection is not (yet) possible. But planets can be found ...
Circumstellar Disks: the Formation and Evolution of
... • Spitzer MIPS 24 and 70 m imaging has revealed a large extended disk at distances > 85 away from the central star • The dust geometry and the low apparent vsini of the star suggests that the star-disk system is face-on • Mid-infrared imaging is sensitive to smallest grains that are either ...
... • Spitzer MIPS 24 and 70 m imaging has revealed a large extended disk at distances > 85 away from the central star • The dust geometry and the low apparent vsini of the star suggests that the star-disk system is face-on • Mid-infrared imaging is sensitive to smallest grains that are either ...
LEO - nina`s Senior project
... orbital period of 500 years. A planet was discovered in the orbit of the primary star in November 2009.The Gamma Leonis system has a combined apparent visual magnitude of 1.98 and is approximately 130 light years distant from the Sun. It is easy to observe in a small telescope under good conditions ...
... orbital period of 500 years. A planet was discovered in the orbit of the primary star in November 2009.The Gamma Leonis system has a combined apparent visual magnitude of 1.98 and is approximately 130 light years distant from the Sun. It is easy to observe in a small telescope under good conditions ...
Moro_Martin`s Talk - CIERA
... planetesimals are needed to generate the dust). Massive planets create structure in debris disks and high resolution observations show that structure is indeed present. Structure is sensitive to long period planets, complementing radial velocity and transit surveys. Debris disk help us learn about d ...
... planetesimals are needed to generate the dust). Massive planets create structure in debris disks and high resolution observations show that structure is indeed present. Structure is sensitive to long period planets, complementing radial velocity and transit surveys. Debris disk help us learn about d ...
PLANETS
... • Requires angular separation ≥ 0.5 arcsec (close to Sun, long orbital periods years – remember: at 1 parsec, 1 arcsec corresponds to 1 AU) Example: Sirius: Also known as Alpha Canis Majoris, Sirius is the fifth closest system to the Sun at 8.6 light-years. Sirius is composed of a main-sequence star ...
... • Requires angular separation ≥ 0.5 arcsec (close to Sun, long orbital periods years – remember: at 1 parsec, 1 arcsec corresponds to 1 AU) Example: Sirius: Also known as Alpha Canis Majoris, Sirius is the fifth closest system to the Sun at 8.6 light-years. Sirius is composed of a main-sequence star ...
ppt
... Fig. 3.— Relative radial velocity measurements made during transits of WASP-14. The symbols are as follows: Subaru (circles), Keck (squares), Joshi et al. 2009 (triangles). Top panel: The Keplerian radial velocity has been subtracted, to isolate the Rossiter-McLaughlin effect. The predicted times of ...
... Fig. 3.— Relative radial velocity measurements made during transits of WASP-14. The symbols are as follows: Subaru (circles), Keck (squares), Joshi et al. 2009 (triangles). Top panel: The Keplerian radial velocity has been subtracted, to isolate the Rossiter-McLaughlin effect. The predicted times of ...
Searching for Baby Planets in a Star`s Dusty Rings
... occur at different distances from the star because of large radial temperature gradients in the disk. Alternatively, they could arise from the concentration of millimeter-sized particles in regions of gas where the turbulence is low or the pressure is high. The work by Isella et al. [1] makes a cons ...
... occur at different distances from the star because of large radial temperature gradients in the disk. Alternatively, they could arise from the concentration of millimeter-sized particles in regions of gas where the turbulence is low or the pressure is high. The work by Isella et al. [1] makes a cons ...
Harpell/Astro 10
... a) Closely examining very high-resolution photographs of other star systems. b) Observing mini-eclipses of a star as an unseen planet passes in front of it. c) Identifying spectral lines that look like what we expect to see from a planet rather than a star. d) Observing a star carefully enough to no ...
... a) Closely examining very high-resolution photographs of other star systems. b) Observing mini-eclipses of a star as an unseen planet passes in front of it. c) Identifying spectral lines that look like what we expect to see from a planet rather than a star. d) Observing a star carefully enough to no ...
Birth of Stars
... to about 10 million K when nuclear fusion of hydrogen into helium begins inside its core At this stage, the (proto)star is said to have reached the main sequence It is now more or less in (hydrostatic) equilibrium and generates energy mainly through nuclear fusion inside its core ...
... to about 10 million K when nuclear fusion of hydrogen into helium begins inside its core At this stage, the (proto)star is said to have reached the main sequence It is now more or less in (hydrostatic) equilibrium and generates energy mainly through nuclear fusion inside its core ...
Where planets are formed: Protoplanetary disk evolution and planet
... • During the dynamical evolution of clusters, stars orbit around the cluster center, and sometime they can get very close each other. • A close encounter between a disk-bearing star and another star can have crucial consequences on the disk evolution, resulting in: • Significant mass loss from the d ...
... • During the dynamical evolution of clusters, stars orbit around the cluster center, and sometime they can get very close each other. • A close encounter between a disk-bearing star and another star can have crucial consequences on the disk evolution, resulting in: • Significant mass loss from the d ...
the search for planets - Cosmos
... change in position of a star due to the pull of an orbiting planet. This technique is most sensitive to high mass planets with large periods orbiting nearby low-mass stars. The great advantage of this method is that it allows the determination of the mass and orbital inclination of the planet. Astro ...
... change in position of a star due to the pull of an orbiting planet. This technique is most sensitive to high mass planets with large periods orbiting nearby low-mass stars. The great advantage of this method is that it allows the determination of the mass and orbital inclination of the planet. Astro ...
Article 1
... In fact, there’s evidence in our own solar system that the giant planets Jupiter, Saturn, Uranus, and Neptune formed at (or near) the snow line then migrated to the their current orbital positions. During the final stages of planetary accretion, Jupiter migrated inward toward the Sun while Saturn, U ...
... In fact, there’s evidence in our own solar system that the giant planets Jupiter, Saturn, Uranus, and Neptune formed at (or near) the snow line then migrated to the their current orbital positions. During the final stages of planetary accretion, Jupiter migrated inward toward the Sun while Saturn, U ...
Studies of young stellar objects (25+5)
... Sequence of images of radio jet at 3.6 cm Curiel et al. (2006) ...
... Sequence of images of radio jet at 3.6 cm Curiel et al. (2006) ...
Exoplanets 2
... in our Solar System seem bright because they reflect light from the Sun in the visible. ...
... in our Solar System seem bright because they reflect light from the Sun in the visible. ...
Stephen E. Strom
... • Results – Significant differences between (uv; ground) and ISO – Concensus: [gas/dust] << ISM value • Not enough to build giant planets • Could mitigate dust migration; quantitative study needed ...
... • Results – Significant differences between (uv; ground) and ISO – Concensus: [gas/dust] << ISM value • Not enough to build giant planets • Could mitigate dust migration; quantitative study needed ...
First light from far-away planet shines the way to new earths
... The technique allowed them to view the reflected light spectrum of 51 Pegasi b, and extract a few parameters from it. These included estimates of the planet’s mass and its reflectivity, or ‘albedo’. Dr Nicolas Cowan, a leading astronomer at Amherst College in Massachusetts, US, who was not involved ...
... The technique allowed them to view the reflected light spectrum of 51 Pegasi b, and extract a few parameters from it. These included estimates of the planet’s mass and its reflectivity, or ‘albedo’. Dr Nicolas Cowan, a leading astronomer at Amherst College in Massachusetts, US, who was not involved ...
Document
... time-dependent calculation by Wetherill (1986), the motion of 500 planetesimals in their orbit around the Sun was modeled (see Fig. 2.3). These initially had masses between that of Ceres and half that of the Moon (Table 2.1), and were distributed across a distance range between 0.4 and 2 AU. In the ...
... time-dependent calculation by Wetherill (1986), the motion of 500 planetesimals in their orbit around the Sun was modeled (see Fig. 2.3). These initially had masses between that of Ceres and half that of the Moon (Table 2.1), and were distributed across a distance range between 0.4 and 2 AU. In the ...
87 Sr
... How did these Hot Jupiters get orbits so close to their stars? • Formed there – but most scientists feel that Jovian planets formed far from farther out • Migrated there - planet interacts with a disk of gas or planetesimals, gravitational forces cause the planet to spiral inward • Flung there – gr ...
... How did these Hot Jupiters get orbits so close to their stars? • Formed there – but most scientists feel that Jovian planets formed far from farther out • Migrated there - planet interacts with a disk of gas or planetesimals, gravitational forces cause the planet to spiral inward • Flung there – gr ...
Planets beyond the solar system
... Needs several years to find then confirm Earth-like planets – “the soonest we anticipate announcing an Earth-size planet orbiting a Sun-like star would be sometime in 2012-2013”. ...
... Needs several years to find then confirm Earth-like planets – “the soonest we anticipate announcing an Earth-size planet orbiting a Sun-like star would be sometime in 2012-2013”. ...
The Sun and Planets Homework 9.
... does this technique work best for detecting massive planets, and those in short period orbits around their host star? What planetary parameters can you determine using this technique? 2. Briefly explain the transit method for detecting extrasolar planets. What type of planets is this technique most ...
... does this technique work best for detecting massive planets, and those in short period orbits around their host star? What planetary parameters can you determine using this technique? 2. Briefly explain the transit method for detecting extrasolar planets. What type of planets is this technique most ...
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.