LOW MASS STAR FORMATION
... large number of UCHII in the galaxy. Combining VLA and IRAS observations, estimated some 1,000 UCHII in the galaxy ionized by an O star. • However, lifetime of HII region as UC should be of order 104 years and assuming 1 O star forms every 100 year, you would expect only about 100 UCHII in the galax ...
... large number of UCHII in the galaxy. Combining VLA and IRAS observations, estimated some 1,000 UCHII in the galaxy ionized by an O star. • However, lifetime of HII region as UC should be of order 104 years and assuming 1 O star forms every 100 year, you would expect only about 100 UCHII in the galax ...
Great Migrations & other natural history tales
... 1995: Radial Velocity Planets were found around normal, nearby stars, via the Doppler spectroscopy of the host starlight, starting with Mayor & Queloz, continuing wth Marcy & Butler, et al. ...
... 1995: Radial Velocity Planets were found around normal, nearby stars, via the Doppler spectroscopy of the host starlight, starting with Mayor & Queloz, continuing wth Marcy & Butler, et al. ...
An Evolutionary Model of KB
... FEPS is allowing a more complete database of debris systems 5 sources have excess emission at 70m, indicating exo-KBs SED modeling indicated log(LIR/L*)-5.2, color temperatures 55 to 58 K, Rin 18 to 46 AU Solar system model within a few factors of observed fluxes HD 13974 either doesn’t have KB-li ...
... FEPS is allowing a more complete database of debris systems 5 sources have excess emission at 70m, indicating exo-KBs SED modeling indicated log(LIR/L*)-5.2, color temperatures 55 to 58 K, Rin 18 to 46 AU Solar system model within a few factors of observed fluxes HD 13974 either doesn’t have KB-li ...
Merak
... How Far Away: 62 light years away How Bright: About 50 times brighter than the Sun Where to View: In the constellation Ursa Major. When to View:All year round in the Northern Hemisphere ...
... How Far Away: 62 light years away How Bright: About 50 times brighter than the Sun Where to View: In the constellation Ursa Major. When to View:All year round in the Northern Hemisphere ...
Evening sky in OCTOBER 2011 Many constellations representing
... the Toucan (Tucana) that do not have bright stars to help identify them easily, can be found somewhat lower in the South. Tucana lies close to Achernar, the bright star in the River (Eridanus). Two bright stars above the south-western horizon point downwards to the Southern Cross (Crux) and are know ...
... the Toucan (Tucana) that do not have bright stars to help identify them easily, can be found somewhat lower in the South. Tucana lies close to Achernar, the bright star in the River (Eridanus). Two bright stars above the south-western horizon point downwards to the Southern Cross (Crux) and are know ...
Review Game
... 11) Refering to Diagram 1, compared to the original planet (Graph 1) which graph shows a planet orbiting faster? 12) Refering to Diagram 1, compared to the original planet graph (Graph 1) which graph shows a larger planet? 13) About how long ago were the first planets around other Sun-like stars we ...
... 11) Refering to Diagram 1, compared to the original planet (Graph 1) which graph shows a planet orbiting faster? 12) Refering to Diagram 1, compared to the original planet graph (Graph 1) which graph shows a larger planet? 13) About how long ago were the first planets around other Sun-like stars we ...
March 2016
... Clif Ashcraft and his night assistant Boomer. A triple star system A 597 at 1.4 arc seconds separation resolved by spatial Fourier analysis. ...
... Clif Ashcraft and his night assistant Boomer. A triple star system A 597 at 1.4 arc seconds separation resolved by spatial Fourier analysis. ...
Proposed Plan - Department of Earth and Planetary Sciences
... Solar neighborhood-like region Orbit: • Earth-trailing, (372.5 days) • Off-ecliptic 6 year mission • 3 transits for significance ...
... Solar neighborhood-like region Orbit: • Earth-trailing, (372.5 days) • Off-ecliptic 6 year mission • 3 transits for significance ...
Lecture11
... Eventually T becomes high enough that molecular hydrogen dissociates; this absorbs some of the energy supporting the protostar, so the core begins to collapse further, until it becomes ~30% larger than the present Solar radius (but still much less massive). The protostar continues to accrete materia ...
... Eventually T becomes high enough that molecular hydrogen dissociates; this absorbs some of the energy supporting the protostar, so the core begins to collapse further, until it becomes ~30% larger than the present Solar radius (but still much less massive). The protostar continues to accrete materia ...
Student notes part 2
... From NASA detecting transiting planets. http://kepler.nasa.gov/Science/transitDetectionAndSimulation/ When a planet crosses in front of its star as viewed by an observer, the event is called a transit. Transits by terrestrial planets produce a small change in a star's brightness of about 1/10,000 (1 ...
... From NASA detecting transiting planets. http://kepler.nasa.gov/Science/transitDetectionAndSimulation/ When a planet crosses in front of its star as viewed by an observer, the event is called a transit. Transits by terrestrial planets produce a small change in a star's brightness of about 1/10,000 (1 ...
Objects in Space
... extending just beyond the orbit of Neptune from about 30 to 55 AU. Named for astronomer Gerard Kuiper. Short period comets originate from the Kuiper Belt (those with orbital periods less than 200 years) It is also the host of many icy dwarf planets including Pluto (also known as KBO’s (Kuiper ...
... extending just beyond the orbit of Neptune from about 30 to 55 AU. Named for astronomer Gerard Kuiper. Short period comets originate from the Kuiper Belt (those with orbital periods less than 200 years) It is also the host of many icy dwarf planets including Pluto (also known as KBO’s (Kuiper ...
Extrasolar Planets
... (A) Its radius (B) Its mass (C) Its orbital period (D) Both its radius and its orbital period ...
... (A) Its radius (B) Its mass (C) Its orbital period (D) Both its radius and its orbital period ...
Extrasolar Planets
... Extrasolar Planet = Exoplanet = Planet orbiting a star other than the Sun. ...
... Extrasolar Planet = Exoplanet = Planet orbiting a star other than the Sun. ...
PPV_hd169142
... Fig. 1: Despite a wealth of stars in the field of HD 169142 (left) , only 3 objects have net H emission (right), including the Herbig Ae star, a star at the bottom of the field and 2MASS 18242929-2946559, which lies 8” SW of HD 169142. Data obtained with the Goddard Fabry-Perot at the Apache Point ...
... Fig. 1: Despite a wealth of stars in the field of HD 169142 (left) , only 3 objects have net H emission (right), including the Herbig Ae star, a star at the bottom of the field and 2MASS 18242929-2946559, which lies 8” SW of HD 169142. Data obtained with the Goddard Fabry-Perot at the Apache Point ...
Untitled - Dommelroute
... of growing from the size of a large pinhead to a mountain may have taken one hundred thousand years or so. Then the process began to slow down. The original dust and gas had been used up, and the cloud thinned. Several stars—such as Beta Pictoris—have been observed with large, thin disks of dust sur ...
... of growing from the size of a large pinhead to a mountain may have taken one hundred thousand years or so. Then the process began to slow down. The original dust and gas had been used up, and the cloud thinned. Several stars—such as Beta Pictoris—have been observed with large, thin disks of dust sur ...
Solar Systems - South Florida Museum
... (b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and (c) has cleared the neighborhood around its orbit. 2) A "dwarf planet" is a celestial body that: (a) is in orbit around the Sun, (b) has sufficient mass f ...
... (b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and (c) has cleared the neighborhood around its orbit. 2) A "dwarf planet" is a celestial body that: (a) is in orbit around the Sun, (b) has sufficient mass f ...
Document
... •1211 planets in 680 planetary systems / 358 multiple planet systems •Thousands of candidates from Kepler spacecraft – statistical studies say almost all of these planets ...
... •1211 planets in 680 planetary systems / 358 multiple planet systems •Thousands of candidates from Kepler spacecraft – statistical studies say almost all of these planets ...
30_transits
... happen to observe the system edge on. Then we can observe a transit. Star’s light will drop slightly because a small amount of it is blocked by planet. Need to very carefully observe brightness of star as a function of time looking for a small dip. ...
... happen to observe the system edge on. Then we can observe a transit. Star’s light will drop slightly because a small amount of it is blocked by planet. Need to very carefully observe brightness of star as a function of time looking for a small dip. ...
Planetary system
... It might seem natural that the rotation nebula would collapse into an ever smaller ball under it’s self gravity, but…… The cloud’s own angular momentum causes it to flatten out, like pizza dough being spun through the air. ...
... It might seem natural that the rotation nebula would collapse into an ever smaller ball under it’s self gravity, but…… The cloud’s own angular momentum causes it to flatten out, like pizza dough being spun through the air. ...
No Slide Title
... must be either close to us or far from each other. Long orbital periods indicate they are far from ...
... must be either close to us or far from each other. Long orbital periods indicate they are far from ...
Other Worlds - UC Berkeley Astronomy w
... Notable Extra-solar Planets! • OGLE-2005-BLG-390Lb: First planet found using microlensing. Mass of 5.5MEarth and distance of 2.6 AU. • HD 209458 b and HD 189733 b: First spectra of extrasolar planets. Found water vapor and other mysterious absorption lines. Also first transiting planet. • TrES-4: ...
... Notable Extra-solar Planets! • OGLE-2005-BLG-390Lb: First planet found using microlensing. Mass of 5.5MEarth and distance of 2.6 AU. • HD 209458 b and HD 189733 b: First spectra of extrasolar planets. Found water vapor and other mysterious absorption lines. Also first transiting planet. • TrES-4: ...
Lecture 19 – Detection of Extrasolar Planets
... • When the lensing star passes in front of the source star, the light from the source star is amplified by a factor of as much as 10-20 • The typical duration of a microlensing event is minutes to hours http://www.nasa.gov/topics/universe/features/planet20110518-video.html ...
... • When the lensing star passes in front of the source star, the light from the source star is amplified by a factor of as much as 10-20 • The typical duration of a microlensing event is minutes to hours http://www.nasa.gov/topics/universe/features/planet20110518-video.html ...
Masers and high mass star formation Claire Chandler
... • Our understanding of low-mass (solar type with masses between 0.1 and 10 MSUN) star formation has improved greatly in the last few decades. • Can we extend the model to high mass stars and to brown dwarfs? • Presentation that emphasizes radio results. ...
... • Our understanding of low-mass (solar type with masses between 0.1 and 10 MSUN) star formation has improved greatly in the last few decades. • Can we extend the model to high mass stars and to brown dwarfs? • Presentation that emphasizes radio results. ...
Habitability - Department of Physics and Astronomy
... • How does the habitable zone around a star of spectral type M compare to that around a star of spectral type G? –A –B –C ...
... • How does the habitable zone around a star of spectral type M compare to that around a star of spectral type G? –A –B –C ...
Part 1 Notes on Stars - Department of Physics and Astronomy
... • How does the habitable zone around a star of spectral type M compare to that around a star of spectral type G? –A –B –C ...
... • How does the habitable zone around a star of spectral type M compare to that around a star of spectral type G? –A –B –C ...
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.