Planet Formation and Dynamics of Planetesimal Disks
... onto a preexisting massive (~ 10 M ) solid core. Formation of the Earth-like planets have likely been an important stage of the giant planet genesis. ...
... onto a preexisting massive (~ 10 M ) solid core. Formation of the Earth-like planets have likely been an important stage of the giant planet genesis. ...
lec14_15_07nov2007
... Idea #2: Do not use linearity assumptions! Non-linearities in the gas flow ...
... Idea #2: Do not use linearity assumptions! Non-linearities in the gas flow ...
So, what`s the problem for high
... IRAS 19410+2336. The clumpmass bins are [1.7(3),4], [4,6], [6,8], [8,10], and [10,25] M, and the axes are in logarithmic units. The error bars represent the standard deviation of a Poisson distribution . The solid line shows the best fit to the data N/M M–a, with a = 2.5. The dashed and dotted lines ...
... IRAS 19410+2336. The clumpmass bins are [1.7(3),4], [4,6], [6,8], [8,10], and [10,25] M, and the axes are in logarithmic units. The error bars represent the standard deviation of a Poisson distribution . The solid line shows the best fit to the data N/M M–a, with a = 2.5. The dashed and dotted lines ...
Detecting Extrasolar Planets
... The Kepler mission has been designed to specifically detect Earth-like (and smaller) planets orbiting other stars. These types of planets have not really been investigated, as it is very hard to detect them. Measurements to date have been of large, Jupiter-mass planets. Our previous calculation show ...
... The Kepler mission has been designed to specifically detect Earth-like (and smaller) planets orbiting other stars. These types of planets have not really been investigated, as it is very hard to detect them. Measurements to date have been of large, Jupiter-mass planets. Our previous calculation show ...
Using Protoplanetary Disks To Weigh The Youngest Stars
... and width of an observed gap on a protoplanetary disk In a protoplanetary disk, a large planet is able to create the so-called disk gap, which is a low gas density region along the planet's orbit, due to the gravitational interaction between the disc and the planet. The gap formation induced by the ...
... and width of an observed gap on a protoplanetary disk In a protoplanetary disk, a large planet is able to create the so-called disk gap, which is a low gas density region along the planet's orbit, due to the gravitational interaction between the disc and the planet. The gap formation induced by the ...
Looking for Extra
... Astrometric results are biased towards finding large planets with long periods, but now Doppler methods were biasing towards ‘hot Jupiters’ – large planets with short periods. Theoreticians debated the ‘natural’ progress of solar system evolution. The discovery of retrograde and highly inclined hot- ...
... Astrometric results are biased towards finding large planets with long periods, but now Doppler methods were biasing towards ‘hot Jupiters’ – large planets with short periods. Theoreticians debated the ‘natural’ progress of solar system evolution. The discovery of retrograde and highly inclined hot- ...
Kein Folientitel - tls
... Expectations of Exoplanetary Systems from our Solar System • Solar proto-planetary disk was viscous. Any eccentric orbits would rapidly be damped out – Exoplanets should be in circular orbits – Orbital axes should be aligned and prograde ...
... Expectations of Exoplanetary Systems from our Solar System • Solar proto-planetary disk was viscous. Any eccentric orbits would rapidly be damped out – Exoplanets should be in circular orbits – Orbital axes should be aligned and prograde ...
Meet the Neighbors: Planets Around Nearby Stars
... The radius of the Earth is 6.38 x 103 km, and Jupiter’s radius is 10.8 times the Earth’s radius. How large is this planet compared to Earth? To Jupiter? Finally, from your measurement of the period of the orbit of the planet, estimate the orbital distance from its star. Since the masses of the star ...
... The radius of the Earth is 6.38 x 103 km, and Jupiter’s radius is 10.8 times the Earth’s radius. How large is this planet compared to Earth? To Jupiter? Finally, from your measurement of the period of the orbit of the planet, estimate the orbital distance from its star. Since the masses of the star ...
Planet migration
... After ~1 Myr end up with a star and protoplanetary disk extending ~100 AU This disk disappears in ~10 Myr and is the site of planet formation ...
... After ~1 Myr end up with a star and protoplanetary disk extending ~100 AU This disk disappears in ~10 Myr and is the site of planet formation ...
Transiting “Hot Jupiters” near the Galactic Center
... formation envisions enough material to build a Jupiter-size planet so close to a young star—yet here one exists. It must have migrated inwards after forming farther out. In the decade since the planet around 51 Pegasi was discovered, astronomers have been actively searching for more. More than 200 e ...
... formation envisions enough material to build a Jupiter-size planet so close to a young star—yet here one exists. It must have migrated inwards after forming farther out. In the decade since the planet around 51 Pegasi was discovered, astronomers have been actively searching for more. More than 200 e ...
A report of the SEEDS Direct Imaging Survey
... Instrument development for “2nd Earths” on TMT and future space telescopes ...
... Instrument development for “2nd Earths” on TMT and future space telescopes ...
A. Some review questions. There are also four
... 9. For which of the following methods of detecting exoplanets is spatial resolution a severe problem? a. direct or reflected light detection b. radial velocity c. transits d. timing 10. How do we know that a “hot Jupiter” is not a “hot Earth,” i.e. a giant rocky planet? a. A rocky planet would evapo ...
... 9. For which of the following methods of detecting exoplanets is spatial resolution a severe problem? a. direct or reflected light detection b. radial velocity c. transits d. timing 10. How do we know that a “hot Jupiter” is not a “hot Earth,” i.e. a giant rocky planet? a. A rocky planet would evapo ...
Physics Today
... stars than Mercury is to our sun. As a result, their temperatures can approach those of cool stars and their atmospheric properties are correspondingly exotic. From measurements of the amount of light blocked by the planet when it transits its star, we can determine the planet’s radius. We can estim ...
... stars than Mercury is to our sun. As a result, their temperatures can approach those of cool stars and their atmospheric properties are correspondingly exotic. From measurements of the amount of light blocked by the planet when it transits its star, we can determine the planet’s radius. We can estim ...
Habitability of planets on eccentric orbits: limits of the mean flux
... around stars of luminosity ranging from L? = 1 L to 10−4 L and of orbital eccentricity from 0 to 0.9. The atmosphere is composed of N2 , CO2 and H2 O (gas, liquid, solid) in Earth-like proportions. First, for the different eccentricities, we scaled the orbital period of the planet (the duration of ...
... around stars of luminosity ranging from L? = 1 L to 10−4 L and of orbital eccentricity from 0 to 0.9. The atmosphere is composed of N2 , CO2 and H2 O (gas, liquid, solid) in Earth-like proportions. First, for the different eccentricities, we scaled the orbital period of the planet (the duration of ...
Giant Planet Formation: Theory vs. Observations The Formation of
... photoevaporated away by nearby O stars. • Photoevaporation converts gas giant protoplanets into ice giants if the protoplanet orbits outside a critical radius, which depends on the mass of the host star. • For solar-mass stars, the critical radius is > 5 AU, while for a 0.3 MSun M dwarf star, the cr ...
... photoevaporated away by nearby O stars. • Photoevaporation converts gas giant protoplanets into ice giants if the protoplanet orbits outside a critical radius, which depends on the mass of the host star. • For solar-mass stars, the critical radius is > 5 AU, while for a 0.3 MSun M dwarf star, the cr ...
Looking for Other Worlds
... 1 AU: 35% of them are less than 0.4 AU, although there is a growing number with larger radius, including one ‘beyond Jupiter’. ...
... 1 AU: 35% of them are less than 0.4 AU, although there is a growing number with larger radius, including one ‘beyond Jupiter’. ...
Alien Earths Floorplan (3,000 sq. ft) Major Exhibit Areas
... But what about more distant worlds? Thousands of years ago, Greek philosophers speculated. “There are infinite worlds both like and unlike this world of ...
... But what about more distant worlds? Thousands of years ago, Greek philosophers speculated. “There are infinite worlds both like and unlike this world of ...
Solar System Origins PowerPoint print-off
... Formation of Any Solar System • Presence of a nebula (gas & dust cloud) – Typically ~ 1.0 light year in diameter – Typically ~ 99% gas & ~1% dust ...
... Formation of Any Solar System • Presence of a nebula (gas & dust cloud) – Typically ~ 1.0 light year in diameter – Typically ~ 99% gas & ~1% dust ...
Extrasolar Planets - Astrophysikalisches Institut und Universitäts
... mass of the companion (planet or brown dwarf), but also from mass and radius its density. The first case, where this was successfully observed was HD 209458 in the year 2000, the first radial velocity planet candidate confirmed to be a true planet (and found to be a gas giant planet with low density ...
... mass of the companion (planet or brown dwarf), but also from mass and radius its density. The first case, where this was successfully observed was HD 209458 in the year 2000, the first radial velocity planet candidate confirmed to be a true planet (and found to be a gas giant planet with low density ...
A0620-00 poster
... The orbital light curve of SS Cyg shows an ellipsoidal variation diluted by light from the disk and white dwarf. From an analysis of the ellipsoidal variations we limit the orbital inclination to the range 45° < i < 56°. The derived masses of the K star and white dwarf are MK = 0.55 ± 0.13 M and MW ...
... The orbital light curve of SS Cyg shows an ellipsoidal variation diluted by light from the disk and white dwarf. From an analysis of the ellipsoidal variations we limit the orbital inclination to the range 45° < i < 56°. The derived masses of the K star and white dwarf are MK = 0.55 ± 0.13 M and MW ...
NASA Just Discovered Seven New Exoplanets... So What?
... What do the planets and solar system look like? As well as being in tight orbits, the TRAPPIST-1 planets are unusually close to one another, conjuring an image straight out of science fiction. If Trappist-1 were our sun, all seven planets would be inside Mercury's orbit. Mercury is the innermost pla ...
... What do the planets and solar system look like? As well as being in tight orbits, the TRAPPIST-1 planets are unusually close to one another, conjuring an image straight out of science fiction. If Trappist-1 were our sun, all seven planets would be inside Mercury's orbit. Mercury is the innermost pla ...
Document
... (i.e. inflated radius) 6. Transiting planets have been discovered around stars fainter than those from radial velocity surveys ...
... (i.e. inflated radius) 6. Transiting planets have been discovered around stars fainter than those from radial velocity surveys ...
S T A R S
... Aldebaran is Alpha Tauri. It means the Follower as it follows the Pleiades across the sky. It was involved in numerous Roman, Greek , Persian and Eastern stories. Arcturus in the book of Job is thought to be Aldebaran. It is about 40 times our sun’s diameter and is about 68 light years away. Aldeba ...
... Aldebaran is Alpha Tauri. It means the Follower as it follows the Pleiades across the sky. It was involved in numerous Roman, Greek , Persian and Eastern stories. Arcturus in the book of Job is thought to be Aldebaran. It is about 40 times our sun’s diameter and is about 68 light years away. Aldeba ...
ppt
... 1. Migration of a giant planet through an inner disk partitions the mass of that disk into internal and external remnants. The mass of the interior and exterior disk depends on the age of the disk. The concept that giant planet migration would eliminate all the mass in its swept zone is not supporte ...
... 1. Migration of a giant planet through an inner disk partitions the mass of that disk into internal and external remnants. The mass of the interior and exterior disk depends on the age of the disk. The concept that giant planet migration would eliminate all the mass in its swept zone is not supporte ...
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.