Exoplanets
... rotation of their host star — challenging theories of planet formation. (eso1016) 2010: With HARPS, astronomers have discovered the first “normal” exoplanet that can be studied in great detail. (eso1011) 2010: VLT captures first direct spectrum of an exoplanet. (eso1002) 2009: Astronomers discove ...
... rotation of their host star — challenging theories of planet formation. (eso1016) 2010: With HARPS, astronomers have discovered the first “normal” exoplanet that can be studied in great detail. (eso1011) 2010: VLT captures first direct spectrum of an exoplanet. (eso1002) 2009: Astronomers discove ...
Lecture
... The Solar System contains only the Sun, Moon, and planets. Meteors are falling stars. Comets sweep across the sky like meteors. Comet tails stream behind the comet as the comet moves. Comets are burning. Planets are close together or are large compared with the distances between ...
... The Solar System contains only the Sun, Moon, and planets. Meteors are falling stars. Comets sweep across the sky like meteors. Comet tails stream behind the comet as the comet moves. Comets are burning. Planets are close together or are large compared with the distances between ...
CONSTELLATION DELPHINUS, THE DOLPHIN
... 1) After Zeus, Poseidon, and Hades had overthrown their father Cronus, they divided up the sky, the sea and the underworld between them, with Poseidon inheriting the sea. He built himself a magnificent underwater palace off the island of Euboea. For all its opulence, the palace felt empty without a ...
... 1) After Zeus, Poseidon, and Hades had overthrown their father Cronus, they divided up the sky, the sea and the underworld between them, with Poseidon inheriting the sea. He built himself a magnificent underwater palace off the island of Euboea. For all its opulence, the palace felt empty without a ...
PowerPoint 簡報
... Kepler-20e and 20f Kepler-20 (also designated as KOI 070, KIC 6850504 and 2MASS J19104752+4220194) is a G8V star of Kepler magnitude 12.497 and celestial coordinates right ascension α = 19 h 10 min 47.5 s and declination δ = +42° 20′ 19.38′′. The stellar properties are listed in Table 1. The photom ...
... Kepler-20e and 20f Kepler-20 (also designated as KOI 070, KIC 6850504 and 2MASS J19104752+4220194) is a G8V star of Kepler magnitude 12.497 and celestial coordinates right ascension α = 19 h 10 min 47.5 s and declination δ = +42° 20′ 19.38′′. The stellar properties are listed in Table 1. The photom ...
ph709-11
... metallicity, or UV flux, will provide insight into the fundamentals of planetary formation, migration, and evolution. The transit method of planet detection is biased toward finding planets that orbit relatively close to their parent stars. This means that radial velocity follow-up will be possible ...
... metallicity, or UV flux, will provide insight into the fundamentals of planetary formation, migration, and evolution. The transit method of planet detection is biased toward finding planets that orbit relatively close to their parent stars. This means that radial velocity follow-up will be possible ...
AUI CA science talk - National Radio Astronomy Observatory
... • Cool universe: thermal emission from gas, dust = fuel for star and galaxy formation • as astrometry • sub-mas imaging • m/s velocity resolution • Accurate polarimetry -- magnetic fields on all scales • Chemistry and bio-tracers VLA polarization ...
... • Cool universe: thermal emission from gas, dust = fuel for star and galaxy formation • as astrometry • sub-mas imaging • m/s velocity resolution • Accurate polarimetry -- magnetic fields on all scales • Chemistry and bio-tracers VLA polarization ...
The surface composition of Beta Pictoris
... Why does the signature of accretion not show up in the surface composition of β Pic? Accretion of gas depleted in refractory elements is thought to be responsible for the deficiency pattern of λ Boo stars, and direct evidence for the presence of CS matter is accumulating (e.g. Stürenburg 1993; HRH9 ...
... Why does the signature of accretion not show up in the surface composition of β Pic? Accretion of gas depleted in refractory elements is thought to be responsible for the deficiency pattern of λ Boo stars, and direct evidence for the presence of CS matter is accumulating (e.g. Stürenburg 1993; HRH9 ...
PLANETS
... Infrared (IR). Because the grains have larger surface area per unit mass compared to larger bodies, they (re)radiate more energy and therefore are more easily detected in the infrared compared to their parent bodies. In the absence of gas drag, a 10 m sized dust grain from the primordial, proto–plan ...
... Infrared (IR). Because the grains have larger surface area per unit mass compared to larger bodies, they (re)radiate more energy and therefore are more easily detected in the infrared compared to their parent bodies. In the absence of gas drag, a 10 m sized dust grain from the primordial, proto–plan ...
Proto-planetary disks
... fast (~0.1Myr) compared with disk lifetime (~10Myr) (Hartmann et al. 2005; Silverstone et al. 2006) • Transition objects are seen at higher rate in old clusters (Megeath et al. 2006) • Very few CTTS are diskless, while most WTTS are diskless (Padgett et al. 2006), meaning more likely for dust to p ...
... fast (~0.1Myr) compared with disk lifetime (~10Myr) (Hartmann et al. 2005; Silverstone et al. 2006) • Transition objects are seen at higher rate in old clusters (Megeath et al. 2006) • Very few CTTS are diskless, while most WTTS are diskless (Padgett et al. 2006), meaning more likely for dust to p ...
lec13_28oct2011
... Boss (2003) disk instability model after 429 yrs, 30 AU radius GI clumps form rapidly, the key questions about planet formation are whether such clumps can cool efficiently enough to continue their contraction or whether they “bounce” and thus dissipate… Much like envelope collapse in coreaccretion ...
... Boss (2003) disk instability model after 429 yrs, 30 AU radius GI clumps form rapidly, the key questions about planet formation are whether such clumps can cool efficiently enough to continue their contraction or whether they “bounce” and thus dissipate… Much like envelope collapse in coreaccretion ...
lec13_28oct2009
... Boss (2003) disk instability model after 429 yrs, 30 AU radius GI clumps form rapidly, the key questions about planet formation are whether such clumps can cool efficiently enough to continue their contraction or whether they “bounce” and thus dissipate… Much like envelope collapse in coreaccretion ...
... Boss (2003) disk instability model after 429 yrs, 30 AU radius GI clumps form rapidly, the key questions about planet formation are whether such clumps can cool efficiently enough to continue their contraction or whether they “bounce” and thus dissipate… Much like envelope collapse in coreaccretion ...
TWO EXTRASOLAR PLANETS FROM THE ANGLO
... by this group of planets (which we will call the Ret-like group, after the first such planet found) is highlighted in Figure 4. It is worth remembering that prior to about 12 months ago, this highlighted region of orbital phase space was empty (Butler et al. 2001b), though many extrasolar planets h ...
... by this group of planets (which we will call the Ret-like group, after the first such planet found) is highlighted in Figure 4. It is worth remembering that prior to about 12 months ago, this highlighted region of orbital phase space was empty (Butler et al. 2001b), though many extrasolar planets h ...
PLANETS
... Because the grains have larger surface area per unit mass compared to larger bodies, they (re)radiate more energy and therefore are more easily detected in the infrared compared to their parent bodies. In the absence of gas drag, a 10 m sized dust grain from the primordial, proto–planetary nebula ca ...
... Because the grains have larger surface area per unit mass compared to larger bodies, they (re)radiate more energy and therefore are more easily detected in the infrared compared to their parent bodies. In the absence of gas drag, a 10 m sized dust grain from the primordial, proto–planetary nebula ca ...
Article PDF - IOPscience
... Our observations of HD 142527 indicate that the inner rim of its outer disk is roughly elliptical, and composed of an overlapping set of spiral arm segments. We confirm that the star is offset by 0. 17 ± 0. 02 from the centroid of the cavity. No companion is detected in the range of 14–35 AU, wi ...
... Our observations of HD 142527 indicate that the inner rim of its outer disk is roughly elliptical, and composed of an overlapping set of spiral arm segments. We confirm that the star is offset by 0. 17 ± 0. 02 from the centroid of the cavity. No companion is detected in the range of 14–35 AU, wi ...
ph709-10
... metallicity, or UV flux, will provide insight into the fundamentals of planetary formation, migration, and evolution. The transit method of planet detection is biased toward finding planets that orbit relatively close to their parent stars. This means that radial velocity follow-up will be possible ...
... metallicity, or UV flux, will provide insight into the fundamentals of planetary formation, migration, and evolution. The transit method of planet detection is biased toward finding planets that orbit relatively close to their parent stars. This means that radial velocity follow-up will be possible ...
The (Super)Wasp Factory Finds 10 New Planets In The Last 6 Months
... In the last 6 months an international team of astronomers have used two batteries of cameras, one in the Canary Islands and one in South Africa, to discover 10 new planets in orbit around other stars (commonly known as extrasolar planets). The results from the Wide Area Search for Planets (SuperWASP ...
... In the last 6 months an international team of astronomers have used two batteries of cameras, one in the Canary Islands and one in South Africa, to discover 10 new planets in orbit around other stars (commonly known as extrasolar planets). The results from the Wide Area Search for Planets (SuperWASP ...
ph709-08
... metallicity, or UV flux, will provide insight into the fundamentals of planetary formation, migration, and evolution. The transit method of planet detection is biased toward finding planets that orbit relatively close to their parent stars. This means that radial velocity follow-up will be possible ...
... metallicity, or UV flux, will provide insight into the fundamentals of planetary formation, migration, and evolution. The transit method of planet detection is biased toward finding planets that orbit relatively close to their parent stars. This means that radial velocity follow-up will be possible ...
lec13_05nov2007
... Boss (2003) disk instability model after 429 yrs, 30 AU radius GI clumps form rapidly, the key questions about planet formation are whether such clumps can cool efficiently enough to continue their contraction or whether they “bounce” and thus dissipate… Much like envelope collapse in coreaccretion ...
... Boss (2003) disk instability model after 429 yrs, 30 AU radius GI clumps form rapidly, the key questions about planet formation are whether such clumps can cool efficiently enough to continue their contraction or whether they “bounce” and thus dissipate… Much like envelope collapse in coreaccretion ...
AST 105 HW #13 Solution
... (1) It will not shake the very foundations of the nebular theory. It is possible that, in this star system, the nebula was very hot even at the orbital distance of Jupiter. Given that assumption, the nebular theory can reasonably explain the presence of such extra solar planet. (2) It is an inte ...
... (1) It will not shake the very foundations of the nebular theory. It is possible that, in this star system, the nebula was very hot even at the orbital distance of Jupiter. Given that assumption, the nebular theory can reasonably explain the presence of such extra solar planet. (2) It is an inte ...
NASA Kepler EPO
... What would the transit of a planet look like if you made a graph of light intensity vs time? ...
... What would the transit of a planet look like if you made a graph of light intensity vs time? ...
Last Time: Planet Finding
... Planetary Migration • A young planet’s motion can create waves in a planetforming disk. • Models show that matter in these waves can tug on a planet, causing its orbit to migrate inward. ...
... Planetary Migration • A young planet’s motion can create waves in a planetforming disk. • Models show that matter in these waves can tug on a planet, causing its orbit to migrate inward. ...
to latest version of Skywatcher
... images of pasta or meat-filled delicacies. But scientists are just as intrigued because they have no idea how it formed. The 1300-kilometer-long ridge circles almost the entirety of Iapetus’s equator.In 2004, NASA’s Cassini spacecraft revealed Iapetus’s ridge to be some 20 kilometers high (that’s mo ...
... images of pasta or meat-filled delicacies. But scientists are just as intrigued because they have no idea how it formed. The 1300-kilometer-long ridge circles almost the entirety of Iapetus’s equator.In 2004, NASA’s Cassini spacecraft revealed Iapetus’s ridge to be some 20 kilometers high (that’s mo ...
Inti didn`t form in the X wind (and neither did most CAIs)
... Steady-state alpha decretion disk, like steady-state alpha accretion disk, experiences radial diffusion on timescales ~ (r/H)2 ()-1 In accretion disks, outward radial diffusion still occurs, on same timescale as net flow of gas inward: crystalline silicates (Gail 2001) or CAIs (Cuzzi et al. 2003). ...
... Steady-state alpha decretion disk, like steady-state alpha accretion disk, experiences radial diffusion on timescales ~ (r/H)2 ()-1 In accretion disks, outward radial diffusion still occurs, on same timescale as net flow of gas inward: crystalline silicates (Gail 2001) or CAIs (Cuzzi et al. 2003). ...
Why are so many extra-solar planets eccentric?
... Interaction with a distant companion star Binary stars A weak tidal force can excited large ecc. Force needs to be stronger than other effect Problems Expected: multi-planet system have low ecc. Expected: high ecc. in binary system. Unseen companions? ...
... Interaction with a distant companion star Binary stars A weak tidal force can excited large ecc. Force needs to be stronger than other effect Problems Expected: multi-planet system have low ecc. Expected: high ecc. in binary system. Unseen companions? ...
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.