Dust and molecular gas in the most distant quasars
... • How the most massive black hole – bulge systems evolve at their early stage. • Can we see active building via massive star formation co-eval with rapid black hole accretion? • Dynamical mass; • Black hole – bulge ratios; ...
... • How the most massive black hole – bulge systems evolve at their early stage. • Can we see active building via massive star formation co-eval with rapid black hole accretion? • Dynamical mass; • Black hole – bulge ratios; ...
Proto-planetary disks
... Disk composition There are two components in a disk: • gas • range of species (e.g., CO, H2) • detected by line emission or in absorption in front of the star • dust • range of compositions (silicate/graphite/PAHs/ices) • range of sizes (sub-µm to planets) • detected by scattered starlight, ...
... Disk composition There are two components in a disk: • gas • range of species (e.g., CO, H2) • detected by line emission or in absorption in front of the star • dust • range of compositions (silicate/graphite/PAHs/ices) • range of sizes (sub-µm to planets) • detected by scattered starlight, ...
Lokal fulltext - Chalmers Publication Library
... and a semi-major axis of 0.05 AU. The star 51 Pegasi (HR 8729, HD 217014, or Gliese 882) is a G5 V star at a 13.7 pc distance. The proximity between the planet and star is why this planet is also considered to be the first hot Jupiter found. However, it is worth noting that already in 1988 a planet ...
... and a semi-major axis of 0.05 AU. The star 51 Pegasi (HR 8729, HD 217014, or Gliese 882) is a G5 V star at a 13.7 pc distance. The proximity between the planet and star is why this planet is also considered to be the first hot Jupiter found. However, it is worth noting that already in 1988 a planet ...
Internal structure of a cold dark molecular cloud inferred
... ³ Astronomy Department, University of Florida, Gainsville, Florida 32608, USA ...
... ³ Astronomy Department, University of Florida, Gainsville, Florida 32608, USA ...
Open access - ORBi
... One of the most interesting results of the FLUOR survey so far is the possible correlation between the presence of cold dust and hot dust for solar-type stars. Another interesting result is the difference in hot exozodi occurence rate between A-type stars and solar-type stars. In order to explore the ...
... One of the most interesting results of the FLUOR survey so far is the possible correlation between the presence of cold dust and hot dust for solar-type stars. Another interesting result is the difference in hot exozodi occurence rate between A-type stars and solar-type stars. In order to explore the ...
Dakota Limestone Products
... Reactivity: 0 HMIS® is a registered trademark of the National Paint and Coatings Association ...
... Reactivity: 0 HMIS® is a registered trademark of the National Paint and Coatings Association ...
Material Safety Data Sheet Marble Chips MSDS# 88723 Section 1
... Do not induce vomiting. If victim is conscious and alert, give 2-4 cupfuls of milk or water. Get medical aid. Inhalation: Remove from exposure and move to fresh air immediately. If not breathing, give artificial respiration. If breathing is difficult, give oxygen. Get medical aid if cough or other s ...
... Do not induce vomiting. If victim is conscious and alert, give 2-4 cupfuls of milk or water. Get medical aid. Inhalation: Remove from exposure and move to fresh air immediately. If not breathing, give artificial respiration. If breathing is difficult, give oxygen. Get medical aid if cough or other s ...
Why there are apparently so few debris disks among post
... core of the order of ~15 Earth masses, the surrounding gas is captured quiet rapidly to form a giant planet. The giant planet and disk interaction produces an inward migration of the planet. ...
... core of the order of ~15 Earth masses, the surrounding gas is captured quiet rapidly to form a giant planet. The giant planet and disk interaction produces an inward migration of the planet. ...
Setting the stage
... measured spectra of PAHs ranging in size from C10H8 to C130H28. Spectra of PAHs in neutral and singly charged (+/–) states. Spectra of a few multiply charged ...
... measured spectra of PAHs ranging in size from C10H8 to C130H28. Spectra of PAHs in neutral and singly charged (+/–) states. Spectra of a few multiply charged ...
The SMC as a probe of dust in the early Universe
... which we anticipate will lead to the production of different pre-silicate grains. These observations will help constrain the dust condensation sequence in the outflows from evolved stars. Post-AGB Sources — The existing samples of SMC spectra from Spitzer include only one postAGB object. This badly ...
... which we anticipate will lead to the production of different pre-silicate grains. These observations will help constrain the dust condensation sequence in the outflows from evolved stars. Post-AGB Sources — The existing samples of SMC spectra from Spitzer include only one postAGB object. This badly ...
Mid-infrared imaging of the dust shell around the post
... mass loss occurs at the end of the AGB. The cause of the shift to axisymmetric outflow is not known, although a number of possible models have been advanced. Most involve a binary companion to the mass-losing AGB star, in either a detached or a common-envelope configuration (e.g. Mastrodemos & Morri ...
... mass loss occurs at the end of the AGB. The cause of the shift to axisymmetric outflow is not known, although a number of possible models have been advanced. Most involve a binary companion to the mass-losing AGB star, in either a detached or a common-envelope configuration (e.g. Mastrodemos & Morri ...
Prospects for detection of protoplanets
... only in the near to mid-infrared wavelength range. This spectral region is influenced also by the warm upper layers of the disk and the inner disk structure, the planetary contribution. => The presence of a planet + the temperature / luminosity of the planet cannot be derived from the SED alone. In ...
... only in the near to mid-infrared wavelength range. This spectral region is influenced also by the warm upper layers of the disk and the inner disk structure, the planetary contribution. => The presence of a planet + the temperature / luminosity of the planet cannot be derived from the SED alone. In ...
T640, T642, T644 High Yield Return Program Print
... Like many finely divided materials, toner dust, in high concentrations can form an explosive mixture in air which, if ignited, could result in a dust explosion. ...
... Like many finely divided materials, toner dust, in high concentrations can form an explosive mixture in air which, if ignited, could result in a dust explosion. ...
Lecture 30 Solar System Formation and Early Evolution
... (so CAI’s would be refractory residues). In either case they also require very high temperatures, probably in the inner-most solar system. Some CAI’s cooled rapidly (0.5-50 K/hr), whereas others remained longer at high temperatures. ...
... (so CAI’s would be refractory residues). In either case they also require very high temperatures, probably in the inner-most solar system. Some CAI’s cooled rapidly (0.5-50 K/hr), whereas others remained longer at high temperatures. ...
Debris disks: dynamics of small particles in
... e.g., for Vega (54Lsun, 2.5Msun, r=90AU, D=100μm, ρ=2700kg/m3): tpr=15Myr (4) They also have short lifetimes due to collisions tcoll = r1.5 / 12 Mstar0.5 τ years e.g., for Vega (τ≈f=2.5x10-5): tcoll=2Myr ...
... e.g., for Vega (54Lsun, 2.5Msun, r=90AU, D=100μm, ρ=2700kg/m3): tpr=15Myr (4) They also have short lifetimes due to collisions tcoll = r1.5 / 12 Mstar0.5 τ years e.g., for Vega (τ≈f=2.5x10-5): tcoll=2Myr ...
Milky Way
... •Approximate black body spectrum – color tells you temperature •Red is cool, blue is hot •Spectral lines tell you a lot about the star •Different lines for each element (and ionization state) •Strength tells you about composition and temperature ...
... •Approximate black body spectrum – color tells you temperature •Red is cool, blue is hot •Spectral lines tell you a lot about the star •Different lines for each element (and ionization state) •Strength tells you about composition and temperature ...
m, a, e
... telescopes with those obtained while combining several such telescopes into an interferometric array (this technique, long practiced by radio astronomers, allows us to achieve very good, low-angular resolution, observations). ...
... telescopes with those obtained while combining several such telescopes into an interferometric array (this technique, long practiced by radio astronomers, allows us to achieve very good, low-angular resolution, observations). ...
The astrobiological case for our cosmic ancestry
... which had remained a mystery for over four decades (Wickramasinghe 1967). These dust particles make up about 1 % of the mass of the entire galaxy and exist in the form of ...
... which had remained a mystery for over four decades (Wickramasinghe 1967). These dust particles make up about 1 % of the mass of the entire galaxy and exist in the form of ...
suggested
... and NH3 . But it was not until the advent of infrared astronomical techniques, making it possible to observe silicate particles emitting at their characteristic 10 lm wavelength in the atmospheres of cool stars, that we had the cores (surfaces) on which the matter could form. TBD was now determined. ...
... and NH3 . But it was not until the advent of infrared astronomical techniques, making it possible to observe silicate particles emitting at their characteristic 10 lm wavelength in the atmospheres of cool stars, that we had the cores (surfaces) on which the matter could form. TBD was now determined. ...
Radiative transfer in the interstellar / circumstellar medium
... a disk can acquire. The surface density of a disk at 1 AU distance from the star can easily reach Σg =1000 gram/cm2. With Σd " 0.01Σg we get Σd " 10 gram/cm2. If the dust completely consists of grains smaller than 1 µm, then the opacity at optical and near-infrared wavelengths can easily be between ...
... a disk can acquire. The surface density of a disk at 1 AU distance from the star can easily reach Σg =1000 gram/cm2. With Σd " 0.01Σg we get Σd " 10 gram/cm2. If the dust completely consists of grains smaller than 1 µm, then the opacity at optical and near-infrared wavelengths can easily be between ...
Optra S High Yield Return Program Print Cartridge for Label
... Like many finely divided materials, toner dust, in high concentrations can form an explosive mixture in air which, if ignited, could result in a dust explosion. ...
... Like many finely divided materials, toner dust, in high concentrations can form an explosive mixture in air which, if ignited, could result in a dust explosion. ...
The Interstellar Medium
... c. molecular hydrogen. d. emission nebulae. e. b and d _______________ require(s) that a young hot star (T 25,000 K) be relatively nearby. a. HII regions b. HI regions c. Molecular clouds d. The hot gas of the interstellar medium e. 21 cm radiation Elements such as iron, calcium, and titanium are le ...
... c. molecular hydrogen. d. emission nebulae. e. b and d _______________ require(s) that a young hot star (T 25,000 K) be relatively nearby. a. HII regions b. HI regions c. Molecular clouds d. The hot gas of the interstellar medium e. 21 cm radiation Elements such as iron, calcium, and titanium are le ...
CHP 10
... b. dense molecular clouds. c. HII regions. d. the intercloud medium. e. the local bubble. _______________ is/are believed to make up 50 percent of the mass of the interstellar medium. a. The intercloud medium b. HI clouds c. Coronal gas d. Molecular clouds e. Dark nebulae Absorption lines due to int ...
... b. dense molecular clouds. c. HII regions. d. the intercloud medium. e. the local bubble. _______________ is/are believed to make up 50 percent of the mass of the interstellar medium. a. The intercloud medium b. HI clouds c. Coronal gas d. Molecular clouds e. Dark nebulae Absorption lines due to int ...
Chapter 3 The Interstellar Medium
... The interstellar medium in a galaxy is a mixture of gas remaining from the formation of the galaxy, gas ejected by stars, and gas accreted from outside (such as infalling diffuse gas or the interstellar medium of other galaxies that have been accreted). The ISM is very important to the evolution of ...
... The interstellar medium in a galaxy is a mixture of gas remaining from the formation of the galaxy, gas ejected by stars, and gas accreted from outside (such as infalling diffuse gas or the interstellar medium of other galaxies that have been accreted). The ISM is very important to the evolution of ...
Cosmic dust
Cosmic dust is dust which exists in space. It is for the most part a type of small dust particles which are a few molecules to 0.1 µm in size. A smaller fraction of all dust in space consists of larger refractory minerals that condensed as matter left the stars. It is called ""stardust"" and is included in a separate section below. The dust density in the local interstellar medium of the Local Bubble is approximately 10−6 × dust grain/m3 with each grain having a mass of approximately 10−17 kg.Cosmic dust can be further distinguished by its astronomical location: intergalactic dust, interstellar dust, interplanetary dust (such as in the zodiacal cloud) and circumplanetary dust (such as in a planetary ring). In the Solar System, interplanetary dust causes the zodiacal light. Sources of Solar System dust include comet dust, asteroidal dust, dust from the Kuiper belt, and interstellar dust passing through the Solar System. The terminology has no specific application for describing materials found on the planet Earth except for dust that has demonstrably fallen to Earth. By one estimate, as much as 40,000 tons of cosmic dust reaches the Earth's surface every year. In October 2011, scientists reported that cosmic dust contains complex organic matter (""amorphous organic solids with a mixed aromatic–aliphatic structure"") that could be created naturally, and rapidly, by stars.On August 14, 2014, scientists announced the collection of possible interstellar dust particles from the Stardust spacecraft since returning to Earth in 2006.