The Origin of the Solar System and Other Planetary Systems
... “hot Jupiters”; they are not included in the previous figure but are numerous. Stars with composition like our Sun are much more likely to have planets, showing that the “dusty disk” theory of solar system formation is plausible. Some of these “planets” may actually be brown dwarfs (i.e. a large bod ...
... “hot Jupiters”; they are not included in the previous figure but are numerous. Stars with composition like our Sun are much more likely to have planets, showing that the “dusty disk” theory of solar system formation is plausible. Some of these “planets” may actually be brown dwarfs (i.e. a large bod ...
A report of the SEEDS Direct Imaging Survey
... 120 nights from 2009; finished in 2015 Jan, only <1 night loss due to HiCIAO NIR direct imaging and census of giant planets in the outer regions (10-100AU) around ~500 solar-type and massive stars Exploring protoplanetary disks and debris disks for the origin of their diversity and evolution at the ...
... 120 nights from 2009; finished in 2015 Jan, only <1 night loss due to HiCIAO NIR direct imaging and census of giant planets in the outer regions (10-100AU) around ~500 solar-type and massive stars Exploring protoplanetary disks and debris disks for the origin of their diversity and evolution at the ...
The Solar System 2003
... Apart from the eight planets in the Solar System, there is also known a few hundreds of extrasolar planets, which orbit foreign stars. Contemporary astronomical instruments do not allow to observe these distant planets directly, but their properties are calculated from photometric and astrometric m ...
... Apart from the eight planets in the Solar System, there is also known a few hundreds of extrasolar planets, which orbit foreign stars. Contemporary astronomical instruments do not allow to observe these distant planets directly, but their properties are calculated from photometric and astrometric m ...
The First Thousand Exoplanets
... variation is inversely proportional to the square root of the orbital distance and proportional to the planet mass times the sin of the inclination angle of the orbit. Because of the uncertainty in inclination, a minimum mass is measured and for any sample of planet systems at random orientations t ...
... variation is inversely proportional to the square root of the orbital distance and proportional to the planet mass times the sin of the inclination angle of the orbit. Because of the uncertainty in inclination, a minimum mass is measured and for any sample of planet systems at random orientations t ...
Large and small planets Journey through the Solar System
... Using the table below, write the information from the second column (the diameter) next to the planets on the board. Explain clearly to the children that the Sun is very large, and that it is not a planet at all, but a star. It is interesting to see how large the sun is compared to the planets. Use ...
... Using the table below, write the information from the second column (the diameter) next to the planets on the board. Explain clearly to the children that the Sun is very large, and that it is not a planet at all, but a star. It is interesting to see how large the sun is compared to the planets. Use ...
summary - guideposts
... differentiated as they formed. In that case, Earth’s first atmosphere was not captured from the nebula but was outgassed from Earth’s interior. Gas in planet forming disks can be blown away quickly by nearby stars, so Jovian planets, which grow primarily from gas, must form quickly. Models suggest t ...
... differentiated as they formed. In that case, Earth’s first atmosphere was not captured from the nebula but was outgassed from Earth’s interior. Gas in planet forming disks can be blown away quickly by nearby stars, so Jovian planets, which grow primarily from gas, must form quickly. Models suggest t ...
Habitable zone - Penn State University
... 1. Big planets are not rocky • One of the most important results from Kepler is that we have learned when a planet is likely to be rocky – Transit depth gives us the planet’s radius – Some Kepler target stars are bright enough so that we can make radial velocity (Doppler) measurements of the planet ...
... 1. Big planets are not rocky • One of the most important results from Kepler is that we have learned when a planet is likely to be rocky – Transit depth gives us the planet’s radius – Some Kepler target stars are bright enough so that we can make radial velocity (Doppler) measurements of the planet ...
The mystery of cosmic oceans and dunes Earth
... the star, the surrounding circulating matter begins to flatten into a protoplanetary disk, a little like a spun clump of dough flattening to form a pizza base. Matter in this disk coalesces to form planets. Several complex and competing processes are in play during planetary formation. The initial m ...
... the star, the surrounding circulating matter begins to flatten into a protoplanetary disk, a little like a spun clump of dough flattening to form a pizza base. Matter in this disk coalesces to form planets. Several complex and competing processes are in play during planetary formation. The initial m ...
Lecture 1: Observations of planetary systems
... Rp ≪ R∗ for all but the very youngest planets, so for planets at ∼AU radii the transit probability is p ∼ 10−3 –10−2 . Transit searches must therefore observe large numbers of stars in order to detect planets, and are very strongly biased towards short-period planets3 . Note also that transits provi ...
... Rp ≪ R∗ for all but the very youngest planets, so for planets at ∼AU radii the transit probability is p ∼ 10−3 –10−2 . Transit searches must therefore observe large numbers of stars in order to detect planets, and are very strongly biased towards short-period planets3 . Note also that transits provi ...
PowerPoint
... Average relative proper motion of lens and source star: μ=6±4mas/yr Resolution: •1.2x2.2μm/8.2m= 66mas (~80mass in VLT/NACO and Keck AO) •1.2x2.2μm/30m=18mass ...
... Average relative proper motion of lens and source star: μ=6±4mas/yr Resolution: •1.2x2.2μm/8.2m= 66mas (~80mass in VLT/NACO and Keck AO) •1.2x2.2μm/30m=18mass ...
Solar System`s Age - Empyrean Quest Publishers
... slowly and so easily captured by the gravity of the massive cores. • The result was a huge planet with an enormously thick, hydrogen-rich envelope surrounding a rocky core with 5-10 times the mass of the Earth ...
... slowly and so easily captured by the gravity of the massive cores. • The result was a huge planet with an enormously thick, hydrogen-rich envelope surrounding a rocky core with 5-10 times the mass of the Earth ...
Extrasolar Planets - University of Maryland Astronomy
... At that point the race was on. As of October 30, 2009, 403 extrasolar planets had been discovered (for an indication of the pace of discovery, a year ago there were 313 known!). There are 45 multiple-planet systems (20 were known a year ago), with the current record holder (the system around 55 Canc ...
... At that point the race was on. As of October 30, 2009, 403 extrasolar planets had been discovered (for an indication of the pace of discovery, a year ago there were 313 known!). There are 45 multiple-planet systems (20 were known a year ago), with the current record holder (the system around 55 Canc ...
Search for Life in the Universe
... • Indirect detection of effect on parent star – Extrasolar planets around main sequence stars discovered in 1995 – Planets around neutron stars discovered previously – Spectroscopy (>100 cases): detect Doppler shift of stellar motion around center of mass – Astrometry (1 case): detect angular motion ...
... • Indirect detection of effect on parent star – Extrasolar planets around main sequence stars discovered in 1995 – Planets around neutron stars discovered previously – Spectroscopy (>100 cases): detect Doppler shift of stellar motion around center of mass – Astrometry (1 case): detect angular motion ...
File1 - School of Astronomy, IPM
... Overall mass of planets ~ 450 Earth mass Overall mass of metals ~ 50 Earth mass metals compose 1/100 of interstellar medium. So the mass of proto-planetary disk should be ~ 5000 Earth mass or at least 0.01 solar mass if condensation efficiency is 100 percent. Disk might be much lighter than star. ...
... Overall mass of planets ~ 450 Earth mass Overall mass of metals ~ 50 Earth mass metals compose 1/100 of interstellar medium. So the mass of proto-planetary disk should be ~ 5000 Earth mass or at least 0.01 solar mass if condensation efficiency is 100 percent. Disk might be much lighter than star. ...
