Today`s Powerpoint
... Mass of end products is less than mass of 4 protons by 0.7%. Mass converted to energy. 600 millions of tons per second fused. Takes billions of years to convert p's to 4He in Sun's core. Process sets lifetime of stars. Hydrostatic Equilibrium: pressure from fusion reactions balances gravity. Sun is ...
... Mass of end products is less than mass of 4 protons by 0.7%. Mass converted to energy. 600 millions of tons per second fused. Takes billions of years to convert p's to 4He in Sun's core. Process sets lifetime of stars. Hydrostatic Equilibrium: pressure from fusion reactions balances gravity. Sun is ...
Constellations - Sierra Star Gazers
... original mass at least eight times that of our Sun. As the fusion process eventually progressed to the element, Iron, all fusion stopped, gravity took over, and in seconds, the star collapsed into a sphere approximately 10 km across. The blast destroyed the star and spewed its remains outward into d ...
... original mass at least eight times that of our Sun. As the fusion process eventually progressed to the element, Iron, all fusion stopped, gravity took over, and in seconds, the star collapsed into a sphere approximately 10 km across. The blast destroyed the star and spewed its remains outward into d ...
Constellations - Mayo Dark Sky Park
... firing the arrow that killed Orion. The story goes like this… Apollo, her jealous brother, observed the giant Orion wading through the sea with his head just above water and challenged Diana to hit the black island in the distance. Diana took fatal aim and discharged the arrow, killing her beloved O ...
... firing the arrow that killed Orion. The story goes like this… Apollo, her jealous brother, observed the giant Orion wading through the sea with his head just above water and challenged Diana to hit the black island in the distance. Diana took fatal aim and discharged the arrow, killing her beloved O ...
Beyond the Solar System Homework for Geology 8
... 20. A collection or cluster of stars and solar systems such as the Milky Way or Andromeda. 21. This type of nebula is a cloud of glowing gas excited by ultraviolet radiation from hot stars. ...
... 20. A collection or cluster of stars and solar systems such as the Milky Way or Andromeda. 21. This type of nebula is a cloud of glowing gas excited by ultraviolet radiation from hot stars. ...
Lecture 9: Post-main sequence evolution of stars Lifespan on the
... left with a white dwarf. The outer envelope is illuminated by the white dwarf producing a planetary nebula. ...
... left with a white dwarf. The outer envelope is illuminated by the white dwarf producing a planetary nebula. ...
HST Key Project to Measure the Hubble Constant from
... in size (get brighter as they grow larger, dim as they shrink) Can’t achieve balance of power welling up from core and power radiating from surface ...
... in size (get brighter as they grow larger, dim as they shrink) Can’t achieve balance of power welling up from core and power radiating from surface ...
IB_Op_F_04 - Effectsmeister
... early 1900's. It is sometimes called a color - magnitude diagram. Why is this ( or why is this not) an appropriate name for a plot of magnitude versus spectral class? Our star, the Sun, is a G2 spectral class star with an absolute magnitude of 4.8 . How does it compare to the locations of the near s ...
... early 1900's. It is sometimes called a color - magnitude diagram. Why is this ( or why is this not) an appropriate name for a plot of magnitude versus spectral class? Our star, the Sun, is a G2 spectral class star with an absolute magnitude of 4.8 . How does it compare to the locations of the near s ...
ALMA_BoJun605_Gruppioni
... High resolution CO imaging to determine morphology (mergers?), derive rotation curves → Mdyn, density, temperature, ... (1h per source) • Observe sources in HCN to trace dense regions of star-formation. (10h per source, 20 sources) • Total: 12h per source, 170h for sample of 50 sources. ...
... High resolution CO imaging to determine morphology (mergers?), derive rotation curves → Mdyn, density, temperature, ... (1h per source) • Observe sources in HCN to trace dense regions of star-formation. (10h per source, 20 sources) • Total: 12h per source, 170h for sample of 50 sources. ...
The Hertzsprung-Russell Diagram
... To get orbital semimajor axis, you need either the parallax to a visual system or the velocity from a spectroscopic system. In a spectroscopic system, you only have a lower limit unless you know the system tilt. In an eclipsing system, you know everything, including the sizes of the stars. Visual sy ...
... To get orbital semimajor axis, you need either the parallax to a visual system or the velocity from a spectroscopic system. In a spectroscopic system, you only have a lower limit unless you know the system tilt. In an eclipsing system, you know everything, including the sizes of the stars. Visual sy ...
Astronomy 100—Exam 2
... 16. Which of the following statements is not true for a supernova explosion A. it is the final stage of the evolution of a massive star. B. material that later formed the earth and human beings was distributed between the stars. C. the star may shine as brightly as billions of stars. D. matter is ej ...
... 16. Which of the following statements is not true for a supernova explosion A. it is the final stage of the evolution of a massive star. B. material that later formed the earth and human beings was distributed between the stars. C. the star may shine as brightly as billions of stars. D. matter is ej ...
May
... NGC4656 is a type SBm barred spiral galaxy in the constellation Canes Venatici (KAY-neez- vë-NAT-ih-si). Popularly known as the Hockey Stick Galaxy, the key features are the angled tilt of the disk and the apparent offset of the core. If observing at low magnification look in the same field of view ...
... NGC4656 is a type SBm barred spiral galaxy in the constellation Canes Venatici (KAY-neez- vë-NAT-ih-si). Popularly known as the Hockey Stick Galaxy, the key features are the angled tilt of the disk and the apparent offset of the core. If observing at low magnification look in the same field of view ...
Spectroscopy, the Doppler Shift and Masses of Binary Stars
... Stellar winds and magnetic torques are thought to be involved in slowing the rotation of stars of class G, K, and M. Stars hotter than F5 have stable surfaces and perhaps low magnetic fields. The sun rotates at 2 km/s ...
... Stellar winds and magnetic torques are thought to be involved in slowing the rotation of stars of class G, K, and M. Stars hotter than F5 have stable surfaces and perhaps low magnetic fields. The sun rotates at 2 km/s ...
Classifying the Spectra of Stars:
... M-stars are very cool and typically have broad features. They usually have strong sodium but it’s broader than it is in a K star. M-stars are a complicated mess that often has very large areas of absorption due to molecules in their atmospheres. We will not be dealing with this spectral type. ...
... M-stars are very cool and typically have broad features. They usually have strong sodium but it’s broader than it is in a K star. M-stars are a complicated mess that often has very large areas of absorption due to molecules in their atmospheres. We will not be dealing with this spectral type. ...
FUN THINGS TO DO
... When you look straight down, the pom poms look like the familiar stars of the Big Dipper. But look at the model from different angles. Notice how the shape of the Big Dipper changes as your perspective changes. Imagine that you are a resident of a planet that is light years away from our Sun. From y ...
... When you look straight down, the pom poms look like the familiar stars of the Big Dipper. But look at the model from different angles. Notice how the shape of the Big Dipper changes as your perspective changes. Imagine that you are a resident of a planet that is light years away from our Sun. From y ...
Chapter 9 / Adobe Acrobat Document
... space suddenly and rapidly expanded to an immense size. 4. George Gamow predicted that the background radiation in the universe should have cooled to about −269°C. The cosmic background radiation detected by Robert Wilson and Arno Penzias and later confirmed by the COBE and WMAP satellites correspon ...
... space suddenly and rapidly expanded to an immense size. 4. George Gamow predicted that the background radiation in the universe should have cooled to about −269°C. The cosmic background radiation detected by Robert Wilson and Arno Penzias and later confirmed by the COBE and WMAP satellites correspon ...
More on Cluster HR diagrams - University of Texas Astronomy
... During the entire RG and AGB phases, significant mass loss is occurring (observed) by a wind. (Probably the radiation pressure and shock waves from pulsations driving matter away—see Discovery 20-2, p. 564.) The star is also pulsating (period ~years); see Fig. 20.9. These bloated envelopes are not v ...
... During the entire RG and AGB phases, significant mass loss is occurring (observed) by a wind. (Probably the radiation pressure and shock waves from pulsations driving matter away—see Discovery 20-2, p. 564.) The star is also pulsating (period ~years); see Fig. 20.9. These bloated envelopes are not v ...
Stars
... • After billions of years, these stars eventually use up most of their nuclear fuel used for fusion and collapse to form a ____________ ...
... • After billions of years, these stars eventually use up most of their nuclear fuel used for fusion and collapse to form a ____________ ...
RED “O Big Red
... Kara reset the star reader. Where had she heard that unusual name before? then she remembered—aldebaran (all-deB-er-on) was one of the brightest stars in earth’s sky. soon the Stella was bathed in red light. “this star is enormous!” manolo shouted. “it’s 44 times wider than the sun, but its temperat ...
... Kara reset the star reader. Where had she heard that unusual name before? then she remembered—aldebaran (all-deB-er-on) was one of the brightest stars in earth’s sky. soon the Stella was bathed in red light. “this star is enormous!” manolo shouted. “it’s 44 times wider than the sun, but its temperat ...
doc
... significant mass loss is occurring (observed) by a wind. (Probably the radiation pressure and shock waves from pulsations driving matter away—see Discovery 20-2, p. 564.) The star is also pulsating (period ~years); see Fig. 20.9. These bloated envelopes are not very stable! Eventually so much of the ...
... significant mass loss is occurring (observed) by a wind. (Probably the radiation pressure and shock waves from pulsations driving matter away—see Discovery 20-2, p. 564.) The star is also pulsating (period ~years); see Fig. 20.9. These bloated envelopes are not very stable! Eventually so much of the ...
M = 5.5 - The Millstone
... degenerate matter where a higher temperature does not correspond to an increase in pressure. So the core is tiny and remains so. Mass Loss: Over time the outer layers of the AGB star are almost totally ejected and may initially appear as a circumstellar shell. With the ejection of the outer layers o ...
... degenerate matter where a higher temperature does not correspond to an increase in pressure. So the core is tiny and remains so. Mass Loss: Over time the outer layers of the AGB star are almost totally ejected and may initially appear as a circumstellar shell. With the ejection of the outer layers o ...
34ReviewNuclear
... A. Studying the continuous spectrum of stars B. Studying absorption lines in stars C. Studying binary star orbits D. Studying the brightnesses of stars E. Only by estimation Hotter stars will be bluer, cooler stars will be redder. However, there’s a possibility you might get confused by intervening ...
... A. Studying the continuous spectrum of stars B. Studying absorption lines in stars C. Studying binary star orbits D. Studying the brightnesses of stars E. Only by estimation Hotter stars will be bluer, cooler stars will be redder. However, there’s a possibility you might get confused by intervening ...
Life Cycles of Stars
... dense stable star about the size of the Earth weighing three tons per cubic centimeter. • It radiates its left-over heat for billions of years. • When its heat is all dispersed, it will be a cold, dark black dwarf essentially a dead star ...
... dense stable star about the size of the Earth weighing three tons per cubic centimeter. • It radiates its left-over heat for billions of years. • When its heat is all dispersed, it will be a cold, dark black dwarf essentially a dead star ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... The existence of a superwind is suggested by two independent variables. The high density observed within the observed shells in stellar ejecta, and relative paucity of very bright stars on the AGB. The latter (Prialnik P. 161) comes from the number of AGB stars expected compared to observed is >10. ...
... The existence of a superwind is suggested by two independent variables. The high density observed within the observed shells in stellar ejecta, and relative paucity of very bright stars on the AGB. The latter (Prialnik P. 161) comes from the number of AGB stars expected compared to observed is >10. ...
Starlight & Stars - Wayne State University Physics and Astronomy
... The Doppler effect doesn’t affect the overall color of an object, unless it is moving at a significant fraction of the speed of light (VERY fast!) For an object moving toward us, the red colors will be shifted to the orange and the near-infrared will be shifted to the red, etc. All of the colors shi ...
... The Doppler effect doesn’t affect the overall color of an object, unless it is moving at a significant fraction of the speed of light (VERY fast!) For an object moving toward us, the red colors will be shifted to the orange and the near-infrared will be shifted to the red, etc. All of the colors shi ...
L10 - QUB Astrophysics Research Centre
... The existence of a superwind is suggested by two independent variables. The high density observed within the observed shells in stellar ejecta, and relative paucity of very bright stars on the AGB. The latter (Prialnik P. 161) comes from the number of AGB stars expected compared to observed is >10. ...
... The existence of a superwind is suggested by two independent variables. The high density observed within the observed shells in stellar ejecta, and relative paucity of very bright stars on the AGB. The latter (Prialnik P. 161) comes from the number of AGB stars expected compared to observed is >10. ...
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.