Document
... • The gravitational formation of large scale structure is dominated by dark matter • Ordinary matter forms the stars, galaxies, and intergalactic gas. It is what we see. • As the universe expands and the matter density drops, dark energy is increasingly taking over and causing the expansion to accel ...
... • The gravitational formation of large scale structure is dominated by dark matter • Ordinary matter forms the stars, galaxies, and intergalactic gas. It is what we see. • As the universe expands and the matter density drops, dark energy is increasingly taking over and causing the expansion to accel ...
The Hertzsprung-Russell Diagram
... In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...
... In general the hotter the star is the brighter it will be. Thus you would expect stars of the same size but different temperatures to form a diagonal line called an equal radius line. Equal Radius lines can be added to an H-R diagram ...
Slide 1
... Globular clusters are systems of between 0.1-1 million stars, gravitationallybound into a single structure about 100 light-years across. This is a picture of a typical globular cluster (GC), NGC 104. Notice the strongly peaked distribution of stars and spherical symmetry - both indicating a stable g ...
... Globular clusters are systems of between 0.1-1 million stars, gravitationallybound into a single structure about 100 light-years across. This is a picture of a typical globular cluster (GC), NGC 104. Notice the strongly peaked distribution of stars and spherical symmetry - both indicating a stable g ...
Problem Set No. 5
... sun only burns a fraction (about 10%) of its hydrogen before leaving the main sequence. While a 0.4 M⊙ star may burn a larger fraction of its hydrogen, we do not think it would burn it all before leaving the main sequence. If, however, it were fully mixed, it would burn all its hydrogen and could th ...
... sun only burns a fraction (about 10%) of its hydrogen before leaving the main sequence. While a 0.4 M⊙ star may burn a larger fraction of its hydrogen, we do not think it would burn it all before leaving the main sequence. If, however, it were fully mixed, it would burn all its hydrogen and could th ...
HIERARCHICAL GALAXY ASSEMBLY AND ITS MANIFESTATIONS
... gas, which turns into stars The formation mechanism is going to be imprinted in the bulge distribution. The distribution of bulge types seem to indicate that secular and classical channels are well separated. ...
... gas, which turns into stars The formation mechanism is going to be imprinted in the bulge distribution. The distribution of bulge types seem to indicate that secular and classical channels are well separated. ...
Properties of Stars
... 5. The stars located in the lower right portion of your chart are cool and dim. What are the characteristics of a star in the upper left portion of the diagram? 6. What are the characteristics of a star located in the upper right portion of the diagram? 7. Compare your graph with the H-R diagram on ...
... 5. The stars located in the lower right portion of your chart are cool and dim. What are the characteristics of a star in the upper left portion of the diagram? 6. What are the characteristics of a star located in the upper right portion of the diagram? 7. Compare your graph with the H-R diagram on ...
Stellar Explosions
... mass of the star Nothing stopping the star from collapsing further; it does so very rapidly, in a giant ...
... mass of the star Nothing stopping the star from collapsing further; it does so very rapidly, in a giant ...
Lecture 39
... Stars on the main sequence produce energy by “hydrogen burning”, fusion of hydrogen to produce helium. The relationship results from the rate of hydrogen burning: large stars have hot, dense interiors and burn hydrogen much faster than smaller stars. Consequently there is an inverse relationship bet ...
... Stars on the main sequence produce energy by “hydrogen burning”, fusion of hydrogen to produce helium. The relationship results from the rate of hydrogen burning: large stars have hot, dense interiors and burn hydrogen much faster than smaller stars. Consequently there is an inverse relationship bet ...
How Big Is Our Universe? - Harvard
... The image at left is the oldest and youngest picture of the universe ever taken. Oldest, because it has taken the light nearly 14 billion years to reach us. Youngest, because it is a snapshot of our newborn universe, long before the first stars and galaxies formed. The bright patterns show clumps of ...
... The image at left is the oldest and youngest picture of the universe ever taken. Oldest, because it has taken the light nearly 14 billion years to reach us. Youngest, because it is a snapshot of our newborn universe, long before the first stars and galaxies formed. The bright patterns show clumps of ...
![[WC 6] nucleus with other emission-lines nuclei of planetary nebulae](http://s1.studyres.com/store/data/004159324_1-0806f9baff29e598ec0946db112c7fad-300x300.png)
[WC 6] nucleus with other emission-lines nuclei of planetary nebulae
... Fig. 1 - Spectrum of M 1-25 (central part), taken with the 1.5 m telescope of the ESO at La Silla, using the B&C spectrograph equipped with a 2048 pixels CCD (exposure time : 60 min). Fig. 2 - Histogram of objects in a given [WC] subclass. Uncertain class are not shown (two WC3-4, three WC4-5, 6 WC4 ...
... Fig. 1 - Spectrum of M 1-25 (central part), taken with the 1.5 m telescope of the ESO at La Silla, using the B&C spectrograph equipped with a 2048 pixels CCD (exposure time : 60 min). Fig. 2 - Histogram of objects in a given [WC] subclass. Uncertain class are not shown (two WC3-4, three WC4-5, 6 WC4 ...
Mr. Traeger`s Light and Stars PowerPoint
... Cepheid Variable Stars can be used to measure long distances to stars. Cycles of brightness range from 1 to 50 days. A star with a cycle of 50 days would be brighter than a star with a brightness range of 1 day. Astronomers can calculate long distances by comparing a Cepheid’s apparent and absolute ...
... Cepheid Variable Stars can be used to measure long distances to stars. Cycles of brightness range from 1 to 50 days. A star with a cycle of 50 days would be brighter than a star with a brightness range of 1 day. Astronomers can calculate long distances by comparing a Cepheid’s apparent and absolute ...
Atoms and Starlight Generating light
... hydrogen and helium form strong lines only at very high temperature the Sun is in fact 73% H, 25% He, 2% everything else (Cecilia Payne, 1924) ...
... hydrogen and helium form strong lines only at very high temperature the Sun is in fact 73% H, 25% He, 2% everything else (Cecilia Payne, 1924) ...
pptx
... hydrogen and helium form strong lines only at very high temperature the Sun is in fact 73% H, 25% He, 2% everything else (Cecilia Payne, 1924) ...
... hydrogen and helium form strong lines only at very high temperature the Sun is in fact 73% H, 25% He, 2% everything else (Cecilia Payne, 1924) ...
Formation and Evolution of Infalling Disks Around Protostars
... Formation of massive metal-free stars Similar to present-day SF ...
... Formation of massive metal-free stars Similar to present-day SF ...
AAS Plenary Talk, May 2011 - National Radio Astronomy Observatory
... EVLA observations of the Barnard 5 star forming cloud: embedded filaments revealed (Pineda) The mm colors of a young binary disk system in the Orion Nebular Cluster (Ricci) Microwave observations of edge-on protoplanetary disks (Melis) First results from a 1.3cm EVLA survey of massive protos ...
... EVLA observations of the Barnard 5 star forming cloud: embedded filaments revealed (Pineda) The mm colors of a young binary disk system in the Orion Nebular Cluster (Ricci) Microwave observations of edge-on protoplanetary disks (Melis) First results from a 1.3cm EVLA survey of massive protos ...
The Observer Newsletter - the TriState Astronomers
... the eclipse such as ball fields, local parks, open fields. He also talked about techniques for photographing the eclipse and what you could expect to see. Fortunately, I had the presentation that George Michael created for the 2006 Eclipse in Adeta, Togo with me, and I was able to share the pictures ...
... the eclipse such as ball fields, local parks, open fields. He also talked about techniques for photographing the eclipse and what you could expect to see. Fortunately, I had the presentation that George Michael created for the 2006 Eclipse in Adeta, Togo with me, and I was able to share the pictures ...
Powerpoint for today
... How big are stars? How far away are they? How bright are they? How hot? How old, and how long do they live? What is their chemical composition? How are they moving? Are they isolated or in clusters? By answering these questions, we not only learn about stars, but about the structure and evolution of ...
... How big are stars? How far away are they? How bright are they? How hot? How old, and how long do they live? What is their chemical composition? How are they moving? Are they isolated or in clusters? By answering these questions, we not only learn about stars, but about the structure and evolution of ...
The 100-billion-body problem A full-scale computer simulation of the
... The number of time steps can also present a computational challenge. Each step should be brief enough that the distance between pairs of stars does not change by more than a few percent. For stars that are many lightyears apart, time steps of several thousand years give acceptable results, but close ...
... The number of time steps can also present a computational challenge. Each step should be brief enough that the distance between pairs of stars does not change by more than a few percent. For stars that are many lightyears apart, time steps of several thousand years give acceptable results, but close ...
Spectroscopic Investigation of Companion Stars in Herbig
... the spectral type and surface gravity of the companion star in the system allow it to be placed on the H-R diagram, where theoretical evolutionary model tracks can then constrain its mass and age, and comparisons can be made between these low mass stars and those formed without the presence of a hig ...
... the spectral type and surface gravity of the companion star in the system allow it to be placed on the H-R diagram, where theoretical evolutionary model tracks can then constrain its mass and age, and comparisons can be made between these low mass stars and those formed without the presence of a hig ...
4550-15Lecture33
... Stars on the main sequence produce energy by “hydrogen burning”, fusion of hydrogen to produce helium. The relationship results from the rate of hydrogen burning: large stars have hot, dense interiors and burn hydrogen much faster than smaller stars. Consequently there is an inverse relationship bet ...
... Stars on the main sequence produce energy by “hydrogen burning”, fusion of hydrogen to produce helium. The relationship results from the rate of hydrogen burning: large stars have hot, dense interiors and burn hydrogen much faster than smaller stars. Consequently there is an inverse relationship bet ...
PowerPoint File
... Measure the distance over which the density of stars significantly falls off with height above, or distance below, the galactic plane. The distance depends on the type of objects considered, but is roughly 100 – 200 parsecs. The galactic plane is much thinner than it is wide. ...
... Measure the distance over which the density of stars significantly falls off with height above, or distance below, the galactic plane. The distance depends on the type of objects considered, but is roughly 100 – 200 parsecs. The galactic plane is much thinner than it is wide. ...
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.