![Planetary Nebulae: Observational Properties, Mimics, and Diagnostics](http://s1.studyres.com/store/data/017529171_1-f740d39862bdbe08e87214b09fe25957-300x300.png)
Chapter 16--Properties of Stars
... Once we have measured a star’s apparent brightness, the next step in determining its luminosity is to measure its distance. The most direct way to measure the distances to stars is with stellar parallax, the small annual shifts in a star’s apparent position caused by Earth’s motion around the Sun [S ...
... Once we have measured a star’s apparent brightness, the next step in determining its luminosity is to measure its distance. The most direct way to measure the distances to stars is with stellar parallax, the small annual shifts in a star’s apparent position caused by Earth’s motion around the Sun [S ...
Galaxies * Island universes
... Galaxies formed by gravitational infall of proto-galactic clumps which were already forming stars by the time they came together, forming spheroid, and bulge Disk formed from later infalling gas of higher angular momentum, which dissipates against itself to settle into a thin disk A Galaxy’s color e ...
... Galaxies formed by gravitational infall of proto-galactic clumps which were already forming stars by the time they came together, forming spheroid, and bulge Disk formed from later infalling gas of higher angular momentum, which dissipates against itself to settle into a thin disk A Galaxy’s color e ...
1. INTRODUCTION
... as these stars often show several distinct stochastic events. We have focused our analysis on young, active stars that do not display rotationally modulated light curves and that can be considered as single X-ray sources. Some stars in the sample are detected or known binary systems, in which only o ...
... as these stars often show several distinct stochastic events. We have focused our analysis on young, active stars that do not display rotationally modulated light curves and that can be considered as single X-ray sources. Some stars in the sample are detected or known binary systems, in which only o ...
Influence of the Gould Belt on Interstellar Extinction
... B, and A0 types (the latter were retained, because they could actually belong to the B type due to the classification errors) were excluded from our sample. As a result of our analysis of the dependence of extinction on the effective wavelength, we adopted the following relation between the extincti ...
... B, and A0 types (the latter were retained, because they could actually belong to the B type due to the classification errors) were excluded from our sample. As a result of our analysis of the dependence of extinction on the effective wavelength, we adopted the following relation between the extincti ...
dark matter - University of Texas Astronomy Home Page
... Work through the following with your groups and hand in one sheet per group with answers. 1. Here’s a table listing each planet, the mass inside each planet’s orbit, and the speed at which that planet orbits the sun. Where is the vast majority of mass in the solar system located? 2. How do the orbi ...
... Work through the following with your groups and hand in one sheet per group with answers. 1. Here’s a table listing each planet, the mass inside each planet’s orbit, and the speed at which that planet orbits the sun. Where is the vast majority of mass in the solar system located? 2. How do the orbi ...
Interactive 4 - Hertzsprung-Russell Diagram Explorer
... b) Gamma rays are released in the core of red giant stars, in a set of nuclear fusion reactions known as the triple-alpha process. Two helium atoms fuse to create one beryllium atom and gamma radiation with energy of -0.0918 MeV. The beryllium atom then fuses with another helium atom to create a car ...
... b) Gamma rays are released in the core of red giant stars, in a set of nuclear fusion reactions known as the triple-alpha process. Two helium atoms fuse to create one beryllium atom and gamma radiation with energy of -0.0918 MeV. The beryllium atom then fuses with another helium atom to create a car ...
Night Photography
... Problem: Capturing star trails in urban areas is impossible with conventional photography because lights and light pollution makes it impossible to take a long enough exposure to capture the motion of the stars Solution: “Image Stacking” ...
... Problem: Capturing star trails in urban areas is impossible with conventional photography because lights and light pollution makes it impossible to take a long enough exposure to capture the motion of the stars Solution: “Image Stacking” ...
PPT - Chandra X-Ray Observatory
... Four processes can disturb equilibrium between gravitation and levitation; potentially responsible for metal-poor hot DAs: • Mass-loss tends to homogenize chemical stratification. However, M-dot drops below critical limit (10-16 M/yr) for Teff<70,000 K (Unglaub & Bues 1998). So, LB1919 should not b ...
... Four processes can disturb equilibrium between gravitation and levitation; potentially responsible for metal-poor hot DAs: • Mass-loss tends to homogenize chemical stratification. However, M-dot drops below critical limit (10-16 M/yr) for Teff<70,000 K (Unglaub & Bues 1998). So, LB1919 should not b ...
Living Things - Fairfield-Suisun Unified School District
... at different wavelengths. Astronomers are able to learn a great deal about the Crab Nebula by examining these different images. The images are shown at different scales. ...
... at different wavelengths. Astronomers are able to learn a great deal about the Crab Nebula by examining these different images. The images are shown at different scales. ...
Nebula
... Originally nebula was a general name for any extended astronomical object, including galaxies beyond the Milky Way (some examples of the older usage survive; for example, the Andromeda Galaxy was referred to as the Andromeda Nebula before galaxies were discovered by Edwin Hubble). ...
... Originally nebula was a general name for any extended astronomical object, including galaxies beyond the Milky Way (some examples of the older usage survive; for example, the Andromeda Galaxy was referred to as the Andromeda Nebula before galaxies were discovered by Edwin Hubble). ...
Article PDF - IOPscience
... the positions of these six GCs on a ∼2.9 × 2.9 deg2 image of M31. They span distances in the range of ∼45 arcmin (G76) to ∼4 deg (B514) from the center of M31, thus allowing us to probe different areas of Andromeda, from the galaxy’s unperturbed halo to regions close to the giant stream. We are awar ...
... the positions of these six GCs on a ∼2.9 × 2.9 deg2 image of M31. They span distances in the range of ∼45 arcmin (G76) to ∼4 deg (B514) from the center of M31, thus allowing us to probe different areas of Andromeda, from the galaxy’s unperturbed halo to regions close to the giant stream. We are awar ...
The Evening Sky Map
... Diffuse Nebula – A cloud of gas illuminated by nearby stars. Double Star – Two stars that appear close to each other in the sky; either linked by gravity so that they orbit each other (binary star) or lying at different distances from Earth (optical double). Apparent separation of stars is given in ...
... Diffuse Nebula – A cloud of gas illuminated by nearby stars. Double Star – Two stars that appear close to each other in the sky; either linked by gravity so that they orbit each other (binary star) or lying at different distances from Earth (optical double). Apparent separation of stars is given in ...
E3 – Stellar distances
... spectroscopic parallax can be relied upon to measure the distance to a star. • When we observe another galaxy, all of the stars in that galaxy are approximately the same distance away from the earth. What we really need is a light source of known luminosity in the galaxy. If we had this then we coul ...
... spectroscopic parallax can be relied upon to measure the distance to a star. • When we observe another galaxy, all of the stars in that galaxy are approximately the same distance away from the earth. What we really need is a light source of known luminosity in the galaxy. If we had this then we coul ...
The physics of white dwarfs
... have been constructed in various parts of the world, and several other groups have also begun white-dwarf observations. As a result, detailed spectroscopic information has now been acquired for more than 400 of these stars. More recently, satellite and rocket-borne observations have begun to open up ...
... have been constructed in various parts of the world, and several other groups have also begun white-dwarf observations. As a result, detailed spectroscopic information has now been acquired for more than 400 of these stars. More recently, satellite and rocket-borne observations have begun to open up ...
CHAPTER 1 The Formation and Structure of Stars
... – Temperature is a measure of the motion of the atoms or molecules in a material—in a hot gas, the atoms move more rapidly than do those in a cool gas. – Although the interstellar clouds are very cold, even at a temperature of only 10 K, the average hydrogen atom moves about 0.5 km/s (1,100 mph). – ...
... – Temperature is a measure of the motion of the atoms or molecules in a material—in a hot gas, the atoms move more rapidly than do those in a cool gas. – Although the interstellar clouds are very cold, even at a temperature of only 10 K, the average hydrogen atom moves about 0.5 km/s (1,100 mph). – ...
HR DIAGRAMS OF STAR CLUSTERS
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
hr diagrams of star clusters
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
THE PERIOD OF ROTATION OF THE SUN
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
Chemical Composition and Evolutionary Status of the Ap Star HD
... adopt the same isotopic composition in our calculations. The isotopic shifts were taken from Lawler et al. (2001). Simultaneous allowance for the hyperfine splitting and the isotopic composition in the case of europium causes its abundance in the atmosphere of HD 138633 to decrease by 0.25 dex. We av ...
... adopt the same isotopic composition in our calculations. The isotopic shifts were taken from Lawler et al. (2001). Simultaneous allowance for the hyperfine splitting and the isotopic composition in the case of europium causes its abundance in the atmosphere of HD 138633 to decrease by 0.25 dex. We av ...
Girardi
... NO. 6 Gyr old RC stars are ∼ 1.4 times more frequent than the 10-Gyr old, mainly because they leave the MS at a faster rate, and despite the IMF favouring old stars. Similar conclusions will apply to RGB stars. ...
... NO. 6 Gyr old RC stars are ∼ 1.4 times more frequent than the 10-Gyr old, mainly because they leave the MS at a faster rate, and despite the IMF favouring old stars. Similar conclusions will apply to RGB stars. ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.