A6 - Vicphysics
... with Galileo is The Galileo Project (http://galileo.rice.edu/). It is an amazing resource that encompasses many aspects of his life, work and times. Follow the links in the Science section to obtain details about his telescopic observations, including his drawings. A handy exercise is to loan studen ...
... with Galileo is The Galileo Project (http://galileo.rice.edu/). It is an amazing resource that encompasses many aspects of his life, work and times. Follow the links in the Science section to obtain details about his telescopic observations, including his drawings. A handy exercise is to loan studen ...
Standards
... statement. The students will have to find their match. After finding their match – they will present their statement to the class. If they did not make a correct match – try again later!! This will lead to discussion about each statement. The students will need to write down the terms and concepts t ...
... statement. The students will have to find their match. After finding their match – they will present their statement to the class. If they did not make a correct match – try again later!! This will lead to discussion about each statement. The students will need to write down the terms and concepts t ...
AST1100 Lecture Notes
... of the universe). A star with two times the mass of the Sun will live only 1/8 or roughly 109 years. The most massive stars only live for a few million years. We see from equation 3 that this can be explained by the fact that massive stars are much more luminous than less massive stars and therefore ...
... of the universe). A star with two times the mass of the Sun will live only 1/8 or roughly 109 years. The most massive stars only live for a few million years. We see from equation 3 that this can be explained by the fact that massive stars are much more luminous than less massive stars and therefore ...
The Properties of Super Star Clusters in A Sample of
... regimes. Using optical photometry, I estimate the ages and masses, as well as construct luminosity functions for the super star cluster systems. Additional H observations allow me to place tighter constraints on the burst ages and trace very recent star formation. The super star clusters ...
... regimes. Using optical photometry, I estimate the ages and masses, as well as construct luminosity functions for the super star cluster systems. Additional H observations allow me to place tighter constraints on the burst ages and trace very recent star formation. The super star clusters ...
Edwin Hubble (1889
... Writing in his doctoral thesis in 1917, Hubble noted that catalogs already included some 17,000 small, faint nebulous objects that could ultimately be resolved into groupings of stars. Perhaps 150,000 were within the reach of existing telescopes. Yet, he wrote, "Extremely little is known of the natu ...
... Writing in his doctoral thesis in 1917, Hubble noted that catalogs already included some 17,000 small, faint nebulous objects that could ultimately be resolved into groupings of stars. Perhaps 150,000 were within the reach of existing telescopes. Yet, he wrote, "Extremely little is known of the natu ...
Eye in the sky - Academy of Science of South Africa
... like 10 – 20 millisecond chunks actually). Because of its size, and the long-exposure ability, SALT can see objects that are billions of times fainter than our naked eye can detect. And there’s still more to it. In astronomy resolution is essential. It is important that things can be resolved, or di ...
... like 10 – 20 millisecond chunks actually). Because of its size, and the long-exposure ability, SALT can see objects that are billions of times fainter than our naked eye can detect. And there’s still more to it. In astronomy resolution is essential. It is important that things can be resolved, or di ...
The physics of white dwarfs
... color of the first few to be discovered, occupy a key position in astrophysical theory. Together with neutron stars and black holes, they are the terminal points of stellar evolution. Their properties thus provide clues to the physical processes that take place during the rapid and often spectacular ...
... color of the first few to be discovered, occupy a key position in astrophysical theory. Together with neutron stars and black holes, they are the terminal points of stellar evolution. Their properties thus provide clues to the physical processes that take place during the rapid and often spectacular ...
Astronomy Astrophysics NGC 7419 as a template for red supergiant clusters &
... Context. The open cluster NGC 7419 is known to contain five red supergiants and a very high number of Be stars. However, there are conflicting reports about its age and distance that prevent a useful comparison with other clusters. Aims. We intend to obtain more accurate parameters for NGC 7419, usi ...
... Context. The open cluster NGC 7419 is known to contain five red supergiants and a very high number of Be stars. However, there are conflicting reports about its age and distance that prevent a useful comparison with other clusters. Aims. We intend to obtain more accurate parameters for NGC 7419, usi ...
distribution and properties of a sample of massive young stars
... Galactic Ring Survey (GRS), and by applying a Galactic scaleheight cut-off of 120 pc, we solve the distance ambiguity for RMS sources located within 18◦ |l| 54◦ . These two steps yield kinematic distances to 291 sources out of a possible 326, located within the GRS longitude range. Combining dista ...
... Galactic Ring Survey (GRS), and by applying a Galactic scaleheight cut-off of 120 pc, we solve the distance ambiguity for RMS sources located within 18◦ |l| 54◦ . These two steps yield kinematic distances to 291 sources out of a possible 326, located within the GRS longitude range. Combining dista ...
Sample pages 1 PDF
... with 30 m diameter or more has begun. In recent years, our capabilities to find very distant, and thus very dim, objects and to examine them in detail have improved immensely thanks to the capability of these large optical telescopes. A second example is the technical evolution and size of optical d ...
... with 30 m diameter or more has begun. In recent years, our capabilities to find very distant, and thus very dim, objects and to examine them in detail have improved immensely thanks to the capability of these large optical telescopes. A second example is the technical evolution and size of optical d ...
Investigating the Spectral Energy Distribution TARA JILL PARKIN
... of star formation rates can be found in the various stellar populations within the galaxy (Tielens, 1995). Low-mass stars with long lifetimes were formed in earlier star formation episodes and the ejected material from the outer layers of these stars (ejecta) contributes more hydrogen (H) gas to the ...
... of star formation rates can be found in the various stellar populations within the galaxy (Tielens, 1995). Low-mass stars with long lifetimes were formed in earlier star formation episodes and the ejected material from the outer layers of these stars (ejecta) contributes more hydrogen (H) gas to the ...
Chapter 7 Elliptical Galaxies Chapter 16 Elliptical Galaxies
... Gases and plasmas (in laboratories, in stars) are collisional where collisions are dominated by electromagnetic forces which are mostly negligible on scales larger than a few times the typical separation of the particles. Stellar systems are collisional where collisions are gravitational and therefo ...
... Gases and plasmas (in laboratories, in stars) are collisional where collisions are dominated by electromagnetic forces which are mostly negligible on scales larger than a few times the typical separation of the particles. Stellar systems are collisional where collisions are gravitational and therefo ...
A Second Shell in the Fornax dSph Galaxy
... two core radii from the centre of the system. Such structure would arise from the interaction between Fornax and a companion object. Another possibility is that the two large lobes of material extending to either side of the dSph represent tidal tails. They qualitatively match simulations of tidal t ...
... two core radii from the centre of the system. Such structure would arise from the interaction between Fornax and a companion object. Another possibility is that the two large lobes of material extending to either side of the dSph represent tidal tails. They qualitatively match simulations of tidal t ...
ULTRA-COMPACT HII REGIONS AND MASSIVE STAR FORMATION
... HII regions must be equivalent to a B3 or hotter main sequence star. At midinfrared wavelengths where warm circumstellar dust, stellar photospheres, and nebular fine structure lines are bright, it will be possible to detect even cooler, less luminous, embedded, newly formed stars using sensitive mod ...
... HII regions must be equivalent to a B3 or hotter main sequence star. At midinfrared wavelengths where warm circumstellar dust, stellar photospheres, and nebular fine structure lines are bright, it will be possible to detect even cooler, less luminous, embedded, newly formed stars using sensitive mod ...
The colour–magnitude relation of early
... with those of F98, again with jDzj , 0:1. So-called catastrophic redshift errors can occur when the spectra of the model templates are a poor match to the observed colours (Yee 1998; Kodama et al. 1999), which happens predominantly with star-forming late-type galaxy spectra. In this analysis, we exp ...
... with those of F98, again with jDzj , 0:1. So-called catastrophic redshift errors can occur when the spectra of the model templates are a poor match to the observed colours (Yee 1998; Kodama et al. 1999), which happens predominantly with star-forming late-type galaxy spectra. In this analysis, we exp ...
Super-solar Metal Abundances in Two Galaxies at ζ ∼ 3.57
... can be underestimated. If this problem affected our measurements, the true metallicities would be even larger than those reported here. The H i column densities are derived from the Lyman-α spectral absorptions (Figure 4). These are strongly blended and show the characteristic damping wing typical f ...
... can be underestimated. If this problem affected our measurements, the true metallicities would be even larger than those reported here. The H i column densities are derived from the Lyman-α spectral absorptions (Figure 4). These are strongly blended and show the characteristic damping wing typical f ...
MillionaireGame__Science_Review
... TRUE! Some matter remains after the explosion, and the shrunken core can become either a neutron star or a black hole. ...
... TRUE! Some matter remains after the explosion, and the shrunken core can become either a neutron star or a black hole. ...
25 Years of the Hubble Space Telescope - Speaker
... Creation” in the Eagle Nebula. This image was the first Hubble image to fascinate the public, and still remains one of Hubble’s most popular images. It was obtained in 1995 with the Wide Field and Planetary Camera 2 (WFPC2). Inside the gaseous towers, which are light-years long, the interstellar gas ...
... Creation” in the Eagle Nebula. This image was the first Hubble image to fascinate the public, and still remains one of Hubble’s most popular images. It was obtained in 1995 with the Wide Field and Planetary Camera 2 (WFPC2). Inside the gaseous towers, which are light-years long, the interstellar gas ...
@let@token Stellar Oscillations: Pulsations of Stars Throughout the
... decreases upon compression and the amplitude of the Lagrangian pressure perturbation increases outward. The convective envelope is the seat of mode excitation, because it acts as an insulating blanket with respect to the perturbed Ñux that enters it from below. A crucial point is that the convective ...
... decreases upon compression and the amplitude of the Lagrangian pressure perturbation increases outward. The convective envelope is the seat of mode excitation, because it acts as an insulating blanket with respect to the perturbed Ñux that enters it from below. A crucial point is that the convective ...
White Dwarf Stars - Stellar Physics Department
... H for magnetic white dwarfs that do show any detectable polarization. P for polarized magnetic white dwarfs. V for variable white dwarfs. And finally to complete the classification, a temperature index can follow their spectral classification. This index is defined as θ = 50400/Teff . Therefore, a w ...
... H for magnetic white dwarfs that do show any detectable polarization. P for polarized magnetic white dwarfs. V for variable white dwarfs. And finally to complete the classification, a temperature index can follow their spectral classification. This index is defined as θ = 50400/Teff . Therefore, a w ...
Spectroscopy: Unlocking the Secrets of Star Light
... A 10,000 K star would have its peak wavelength in the ultraviolet part of the em spectrum whilst a 3,000 K star would emit most of its radiation in the infrared part. Not only does the shape of the curve determine the relative intensity of the different components of the continuous spectrum produced ...
... A 10,000 K star would have its peak wavelength in the ultraviolet part of the em spectrum whilst a 3,000 K star would emit most of its radiation in the infrared part. Not only does the shape of the curve determine the relative intensity of the different components of the continuous spectrum produced ...
Spectroscopy: Unlocking the Secrets of Star Light
... A 10,000 K star would have its peak wavelength in the ultraviolet part of the em spectrum whilst a 3,000 K star would emit most of its radiation in the infrared part. Not only does the shape of the curve determine the relative intensity of the different components of the continuous spectrum produced ...
... A 10,000 K star would have its peak wavelength in the ultraviolet part of the em spectrum whilst a 3,000 K star would emit most of its radiation in the infrared part. Not only does the shape of the curve determine the relative intensity of the different components of the continuous spectrum produced ...
Spectral classification of O–M stars on the basis of UBV photometry
... Once the star spectrum Sp is determined, more accurate E(U −B)/E(B−V ) and Q0UBV values are recomputed and a final spectral type SpUBV of the star is determined with the help of transition tables by Strayzis (1977). In the cases to be discussed below, when two spectral estimates Sp are equally possi ...
... Once the star spectrum Sp is determined, more accurate E(U −B)/E(B−V ) and Q0UBV values are recomputed and a final spectral type SpUBV of the star is determined with the help of transition tables by Strayzis (1977). In the cases to be discussed below, when two spectral estimates Sp are equally possi ...
Weakened magnetic braking as the origin of anomalously
... in these stars, which implies at least small-scale magnetic activity. The starspot properties may or may not directly reflect changes in the largescale magnetic field that governs spin-down. A change in field geometry from a simple dipole to higher-order fields could produce weakened braking18,19, a ...
... in these stars, which implies at least small-scale magnetic activity. The starspot properties may or may not directly reflect changes in the largescale magnetic field that governs spin-down. A change in field geometry from a simple dipole to higher-order fields could produce weakened braking18,19, a ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.