Life Cycle of Stars
... Facts: The term „double star“ is used for binary star systems, but also for stars that optically just appear close to each other. Binary star systems are very important references for astronomers: Their orbits allow to determine their masses, which again allows to calculate radius and density. Resul ...
... Facts: The term „double star“ is used for binary star systems, but also for stars that optically just appear close to each other. Binary star systems are very important references for astronomers: Their orbits allow to determine their masses, which again allows to calculate radius and density. Resul ...
PowerPoint - Chandra X
... IC 443: A Supernova Remnant with a Newly Discovered Neutron Star 5,000 light years from Earth This Chandra image shows a point-like source of X-rays inside a cloud of high energy particles which is embedded in the supernova remnant IC443. Using this image, along with radio data from the Very Large A ...
... IC 443: A Supernova Remnant with a Newly Discovered Neutron Star 5,000 light years from Earth This Chandra image shows a point-like source of X-rays inside a cloud of high energy particles which is embedded in the supernova remnant IC443. Using this image, along with radio data from the Very Large A ...
NASAexplores 9-12 Lesson: Classified Stars - Science
... American Henry Russell, determined a pattern in the life of stars. They arranged stars on a chart according to their color and brightness. The most amazing thing is that they did not even know one other, and did their experiments completely independent of each other. Therefore, this chart is called ...
... American Henry Russell, determined a pattern in the life of stars. They arranged stars on a chart according to their color and brightness. The most amazing thing is that they did not even know one other, and did their experiments completely independent of each other. Therefore, this chart is called ...
EVOLUTION OF A SOLAR
... The Life and Death of a Sun-like Star These notes describe the evolutionary path taken by a Sun-like star, one with an initial mass comparable to the Sun’s mass. Stars can be thought of as a series of nested shells, surrounding a core. The core is more dense, hotter, and at higher pressure than the ...
... The Life and Death of a Sun-like Star These notes describe the evolutionary path taken by a Sun-like star, one with an initial mass comparable to the Sun’s mass. Stars can be thought of as a series of nested shells, surrounding a core. The core is more dense, hotter, and at higher pressure than the ...
Star Show FACILITATOR NOTES
... either method yields much clearer distinctions than those available to the naked eye. Students may be familiar with line spectra and confused about the fact that star color has almost nothing to do with a star’s composition. (Astronomers were confused for a long while too.) Stars really are “black b ...
... either method yields much clearer distinctions than those available to the naked eye. Students may be familiar with line spectra and confused about the fact that star color has almost nothing to do with a star’s composition. (Astronomers were confused for a long while too.) Stars really are “black b ...
ASTR 553/554 (1) : Questions
... Notice: solar type stars live so long for two reasons: (a) their fuel is indeed very energy rich; but (b) they burn it at an extremely frugal rate -their furnaces are surprisingly feeble, per kg, well below even to your own metabolic rate. d. Finally, use the stellar mass-luminosity relation (L ...
... Notice: solar type stars live so long for two reasons: (a) their fuel is indeed very energy rich; but (b) they burn it at an extremely frugal rate -their furnaces are surprisingly feeble, per kg, well below even to your own metabolic rate. d. Finally, use the stellar mass-luminosity relation (L ...
RIPL Radio Interferometric Planet Search
... Sensitivity is limited by the short lever arm of VLBA observations: ~10 days RIPL will extend this lever arm by factor of 100 ...
... Sensitivity is limited by the short lever arm of VLBA observations: ~10 days RIPL will extend this lever arm by factor of 100 ...
Measuring stars Part I
... Astronomers still use an ancient method for measuring stellar brightness which was proposed by the Greek astronomer Hipparchus (c. 190 – 120 B.C.) ...
... Astronomers still use an ancient method for measuring stellar brightness which was proposed by the Greek astronomer Hipparchus (c. 190 – 120 B.C.) ...
1 Ay 124 Winter 2016 – HOMEWORK #3
... Due Friday, Feb 5, 2016 by 5pm, in Denise’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about t ...
... Due Friday, Feb 5, 2016 by 5pm, in Denise’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about t ...
PHY111 Stellar Evolution
... some 4He also in stars, some 7Li also by spallation 6Li, 9Be, 10Be and 11B are made by cosmic ray spallation Elements between carbon and the iron peak are made ...
... some 4He also in stars, some 7Li also by spallation 6Li, 9Be, 10Be and 11B are made by cosmic ray spallation Elements between carbon and the iron peak are made ...
The Galaxies
... Somehow it drives a repulsive force that acts on all matter. It gets stronger the more space there is between two globs of matter. It is extremely weak on “local” scales (millions of light years), but gets overwhelmingly strong on “cosmological” scales (tens of billions of light ...
... Somehow it drives a repulsive force that acts on all matter. It gets stronger the more space there is between two globs of matter. It is extremely weak on “local” scales (millions of light years), but gets overwhelmingly strong on “cosmological” scales (tens of billions of light ...
Chapter 12 Stellar Evolution
... burns hydrogen in the surrounding shell. The core contracts and heats; the outer atmosphere expands and cools. • Helium begins to fuse in the core, as a helium flash. The star expands into a red giant as the core continues to collapse. The envelope blows ...
... burns hydrogen in the surrounding shell. The core contracts and heats; the outer atmosphere expands and cools. • Helium begins to fuse in the core, as a helium flash. The star expands into a red giant as the core continues to collapse. The envelope blows ...
Lecture 15
... • Dust absorbs light from stars and reradiates it like a blackbody with a temperature of T=10-100K ...
... • Dust absorbs light from stars and reradiates it like a blackbody with a temperature of T=10-100K ...
Through Hubble`s Eye - Arizona State University
... Astronomers cannot see the very edge of the universe. Not yet. What light may exist there is so young that it comes from a time when the universe was not much more than a warm bath of neutral hydrogen gas. The first few stars and galaxies formed in this period are concealed from us today by this gas ...
... Astronomers cannot see the very edge of the universe. Not yet. What light may exist there is so young that it comes from a time when the universe was not much more than a warm bath of neutral hydrogen gas. The first few stars and galaxies formed in this period are concealed from us today by this gas ...
milkyway - University of Pittsburgh
... visible light • Canva-Paper is much closer than e.g. copier paper ...
... visible light • Canva-Paper is much closer than e.g. copier paper ...
1 Ay 124 Winter 2014 – HOMEWORK #3
... Due Friday, Feb 14, 2014 by 5pm, in Steidel’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about ...
... Due Friday, Feb 14, 2014 by 5pm, in Steidel’s mailbox in 249 Cahill Problem 1 The nearest spiral galaxy to the Milky Way, M31, has a very concentrated nucleus. At a projected radius of 1 arcsec, stars in the nucleus have a line of sight velocity dispersion of 150 km s−1 , and are also rotating about ...
As far as - Sangeeta Malhotra
... census of galaxies at redshift 6. The light we see left these galaxies within the Big Bang’s first billion years. But astronomers remain split on whether these are the first galaxies. We can find some answers by looking at the diffuse gas surrounding galaxies, rather than at the galaxies themselves. ...
... census of galaxies at redshift 6. The light we see left these galaxies within the Big Bang’s first billion years. But astronomers remain split on whether these are the first galaxies. We can find some answers by looking at the diffuse gas surrounding galaxies, rather than at the galaxies themselves. ...
H-R Diagram Lab
... information about them. Together, they created a diagram on which they mapped stars by magnitude and spectral class. After the astronomers had completed graphing the stars, they noticed that several patterns appeared. First, they noticed that ninety per cent of the stars fell along a diagonal line f ...
... information about them. Together, they created a diagram on which they mapped stars by magnitude and spectral class. After the astronomers had completed graphing the stars, they noticed that several patterns appeared. First, they noticed that ninety per cent of the stars fell along a diagonal line f ...
27.1: Characteristics of Stars
... Approximately 6000 stars are visible to the unaided eye from earth About 3 billion can be seen through ground-based telescopes Over 1 trillion can be observed from the Hubble Space Telescope The visibility of a star depends on its brightness and its distance from the Earth. Astronomers use two scale ...
... Approximately 6000 stars are visible to the unaided eye from earth About 3 billion can be seen through ground-based telescopes Over 1 trillion can be observed from the Hubble Space Telescope The visibility of a star depends on its brightness and its distance from the Earth. Astronomers use two scale ...
Lecture17
... Used to classify stars by type: OBAFKM (from hottest to coldest). All stars have spectra lines or “gaps” in their continuous spectrum, just like the sun, but the lines differ, and depend on how hot the star is. Recently cool stellar types “L” and “T” were added, down to 700K at their surface! ...
... Used to classify stars by type: OBAFKM (from hottest to coldest). All stars have spectra lines or “gaps” in their continuous spectrum, just like the sun, but the lines differ, and depend on how hot the star is. Recently cool stellar types “L” and “T” were added, down to 700K at their surface! ...
More detailed notes - Particle Physics and Particle Astrophysics
... Mdisc is the mass of the circumstellar disc. Hα is a spectral line of hydrogen: Hα emission is a sign of the presence of ionised hydrogen. Heavily obscured, very young objects (Class 0) aren’t really recognisable as stars, but can be observed in the millimetre region of the electromagnetic spectrum; ...
... Mdisc is the mass of the circumstellar disc. Hα is a spectral line of hydrogen: Hα emission is a sign of the presence of ionised hydrogen. Heavily obscured, very young objects (Class 0) aren’t really recognisable as stars, but can be observed in the millimetre region of the electromagnetic spectrum; ...
Oscillating White Dwarf Stars Background on White Dwarfs
... temperatures of 100.000.000 K. 8Be is unstable and decays back into He in 2.6 × 10–16 secs, but in the stellar interior a small equilibrium of 8Be exists. The 8Be ground state has almost exactly the energy of two alpha particles. In the second step, 8Be + 4He has almost exactly the energy of an exci ...
... temperatures of 100.000.000 K. 8Be is unstable and decays back into He in 2.6 × 10–16 secs, but in the stellar interior a small equilibrium of 8Be exists. The 8Be ground state has almost exactly the energy of two alpha particles. In the second step, 8Be + 4He has almost exactly the energy of an exci ...
RR animation
... and consequently, they were once stars with similar or slightly less mass than the Sun, around 0.8 solar masses. RR Lyrae stars pulse in a manner similar to Cepheid variables, so the mechanism for the pulsation is thought to be similar, but the nature and histories of these stars is thought to be ra ...
... and consequently, they were once stars with similar or slightly less mass than the Sun, around 0.8 solar masses. RR Lyrae stars pulse in a manner similar to Cepheid variables, so the mechanism for the pulsation is thought to be similar, but the nature and histories of these stars is thought to be ra ...
here - British Astronomical Association
... • Variations caused by star physically pulsating – like a balloon blowing up and down – only outer layers involved. • Periods range from hours to years, depending type. ...
... • Variations caused by star physically pulsating – like a balloon blowing up and down – only outer layers involved. • Periods range from hours to years, depending type. ...
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.