History of Star Formation in Local Galaxies
... The Stellar Populations of the SMC Full analysis of the CMDs is not complete yet, but simply from comparing the CMDs to isochrones, we find that the SMC does have 10-12 Gyr old stars. Just not that many. Thus the SMC had a slow start to its formation… which maybe a reason so few globular clusters f ...
... The Stellar Populations of the SMC Full analysis of the CMDs is not complete yet, but simply from comparing the CMDs to isochrones, we find that the SMC does have 10-12 Gyr old stars. Just not that many. Thus the SMC had a slow start to its formation… which maybe a reason so few globular clusters f ...
Characteristics of Stars
... • White dwarfs are about the size of Earth • Neutrons stars are only about 20 km in ...
... • White dwarfs are about the size of Earth • Neutrons stars are only about 20 km in ...
LISENFELD Ute: Suppression of star formation in compact groups
... interes/ng systems to study galaxy transforma/on because interac/ons between galaxies and with the intragroup medium are frequent. • A gap/canyon was found in their Spitzer IR colors between ac/ve and quiescent galaxies, indica/ng a fast transi/on between both phases (Johnson+07, Walker+1 ...
... interes/ng systems to study galaxy transforma/on because interac/ons between galaxies and with the intragroup medium are frequent. • A gap/canyon was found in their Spitzer IR colors between ac/ve and quiescent galaxies, indica/ng a fast transi/on between both phases (Johnson+07, Walker+1 ...
astronomy webquest…… explore the universe
... Stars and planets are made from gases in a __________________. The Milky Way Galaxy is approximately _______________ light years across. How much longer will our Sun last? _________________________ Lifetimes of stars range from ___________ to ____________ years. Our star orbits the centre of our gal ...
... Stars and planets are made from gases in a __________________. The Milky Way Galaxy is approximately _______________ light years across. How much longer will our Sun last? _________________________ Lifetimes of stars range from ___________ to ____________ years. Our star orbits the centre of our gal ...
Neutron Stars
... • All heavy elements are created and dispersed through the galaxy by stars • Without high mass stars, no heavy elements • Our atoms were once parts of stars that died more than 4.6 billion years ago, whose remains were swept up into the solar system when the Sun formed ...
... • All heavy elements are created and dispersed through the galaxy by stars • Without high mass stars, no heavy elements • Our atoms were once parts of stars that died more than 4.6 billion years ago, whose remains were swept up into the solar system when the Sun formed ...
1. absolute brightness -
... lines observed, originally the amount of Hydrogen the lines seemed to indicate. • Today they are ranked in order of surface temperature. O, B, A, F, G, K, M from ...
... lines observed, originally the amount of Hydrogen the lines seemed to indicate. • Today they are ranked in order of surface temperature. O, B, A, F, G, K, M from ...
HR diagram
... located here are about 10 times larger than the Sun, and many time more luminous. Supergiants: A band extending across the top of the HR diagram from blue to red. These are extremely large and luminous stars. White dwarfs: A region in the lower left of the diagram. These are faint, hot, very sma ...
... located here are about 10 times larger than the Sun, and many time more luminous. Supergiants: A band extending across the top of the HR diagram from blue to red. These are extremely large and luminous stars. White dwarfs: A region in the lower left of the diagram. These are faint, hot, very sma ...
Star Types - University of Massachusetts Amherst
... Where does the energy come from in a star like the Sun? Why? Nuclear fusion. What elements can such a star produce? Carbon and Oxygen. Why cannot the star produce heavier element? not enough mass to reach the temperature. Why more massive stars have higher central temperatures? high pressure to bal ...
... Where does the energy come from in a star like the Sun? Why? Nuclear fusion. What elements can such a star produce? Carbon and Oxygen. Why cannot the star produce heavier element? not enough mass to reach the temperature. Why more massive stars have higher central temperatures? high pressure to bal ...
Neutron Stars
... • All heavy elements are created and dispersed through the galaxy by stars • Without high mass stars, no heavy elements • Our atoms were once parts of stars that died more than 4.6 billion years ago, whose remains were swept up into the solar system when the Sun formed ...
... • All heavy elements are created and dispersed through the galaxy by stars • Without high mass stars, no heavy elements • Our atoms were once parts of stars that died more than 4.6 billion years ago, whose remains were swept up into the solar system when the Sun formed ...
Study Guide for 3RD Astronomy Exam
... and lifetime of an O main sequence star, the Sun and an M main sequence star. State the impact of convection in the envelope of very low mass stars on the stars main sequence lifetime. Describe or identify changes in a star during its main sequence lifetime. Unit 63: Giant Stars Describe how shell f ...
... and lifetime of an O main sequence star, the Sun and an M main sequence star. State the impact of convection in the envelope of very low mass stars on the stars main sequence lifetime. Describe or identify changes in a star during its main sequence lifetime. Unit 63: Giant Stars Describe how shell f ...
Cold atomic matter in the Universe Circmstellar shells around
... The star is now a red giant on the Asymptotic Giant Branch (AGB). The atmosphere becomes unstable, so that the luminosity and the radius vary in time. It is also during this phase, that these stars undergo mass loss at a large rate, which may reach 10-5 Mo per year, and with an expansion velocity in ...
... The star is now a red giant on the Asymptotic Giant Branch (AGB). The atmosphere becomes unstable, so that the luminosity and the radius vary in time. It is also during this phase, that these stars undergo mass loss at a large rate, which may reach 10-5 Mo per year, and with an expansion velocity in ...
Elliptical Galaxies
... M-82 Galaxy M-82 is also known as the "Cigar Galaxy". It is not exactly edge-on, but it is very close. The galaxy is rich in star birth activities and shows a nice dark dusk region. The galaxy is located near the Big dipper and can only be seen from the northern ...
... M-82 Galaxy M-82 is also known as the "Cigar Galaxy". It is not exactly edge-on, but it is very close. The galaxy is rich in star birth activities and shows a nice dark dusk region. The galaxy is located near the Big dipper and can only be seen from the northern ...
UNIT 4 - Rowan County Schools
... Radio Waves (RF) Radio waves • Have very low energy • Used to gather information about: – Supernova – Quasars/blazars (activie galaxies) – Pulsars – The interstellar medium – The big bang ...
... Radio Waves (RF) Radio waves • Have very low energy • Used to gather information about: – Supernova – Quasars/blazars (activie galaxies) – Pulsars – The interstellar medium – The big bang ...
Galaxies - Mike Brotherton
... Measuring the Mass of the Black Hole in the Center of the Milky Way By following the orbits of individual stars near the center of the Milky Way, the mass of the central black hole could be determined to be ~ 2.6 million ...
... Measuring the Mass of the Black Hole in the Center of the Milky Way By following the orbits of individual stars near the center of the Milky Way, the mass of the central black hole could be determined to be ~ 2.6 million ...
The Milky Way and other Galaxies
... Measuring the Mass of the Black Hole in the Center of the Milky Way By following the orbits of individual stars near the center of the Milky Way, the mass of the central black hole could be determined to be ~ 4 million ...
... Measuring the Mass of the Black Hole in the Center of the Milky Way By following the orbits of individual stars near the center of the Milky Way, the mass of the central black hole could be determined to be ~ 4 million ...
White Dwarfs
... fusion goes into re-expanding and cooling the core. Takes only a few seconds! This slows fusion, so star gets dimmer again. - Then stable He -> C burning. Still have H -> He shell burning ...
... fusion goes into re-expanding and cooling the core. Takes only a few seconds! This slows fusion, so star gets dimmer again. - Then stable He -> C burning. Still have H -> He shell burning ...
Stars - Academic Computer Center
... can determine its luminosity. • A stars luminosity is related to both its temperature and its radius. • So if we also know a star’s temperature we can determine its ...
... can determine its luminosity. • A stars luminosity is related to both its temperature and its radius. • So if we also know a star’s temperature we can determine its ...
The H-R Diagram
... muons), and many more particles you don’t hear about much because they decay rapidly in ordinary circumstances… • Radioactive carbon-14 is also created (in trace amounts) by cosmic ray collisions producing free neutrons acting on ordinary nitrogen in our atmosphere. This C14 has a half-life of 5,730 ...
... muons), and many more particles you don’t hear about much because they decay rapidly in ordinary circumstances… • Radioactive carbon-14 is also created (in trace amounts) by cosmic ray collisions producing free neutrons acting on ordinary nitrogen in our atmosphere. This C14 has a half-life of 5,730 ...
astrocoursespring2012lec1-1-5
... Course time: 19:30 – 22:00 formally with priority given to observing when clear 5 lectures covering observing the night sky: I Celestial Sphere and our place in it II Stars within our galaxy, binary systems, variable stars, dying stars (‘planetary nebula’) III Star clusters Open Clusters within the ...
... Course time: 19:30 – 22:00 formally with priority given to observing when clear 5 lectures covering observing the night sky: I Celestial Sphere and our place in it II Stars within our galaxy, binary systems, variable stars, dying stars (‘planetary nebula’) III Star clusters Open Clusters within the ...
SECTION 30.2 Measuring the Stars 1. Constellations are a. the
... d. found only in the northern hemisphere. 2. Ursa Major, or the big dipper, is an example of a a. circumpolar constellation. b. constellation that can be seen only in winter. c. constellation that can be seen only in summer. d. constellation that can be seen only in the fall. 3. Scientists measure d ...
... d. found only in the northern hemisphere. 2. Ursa Major, or the big dipper, is an example of a a. circumpolar constellation. b. constellation that can be seen only in winter. c. constellation that can be seen only in summer. d. constellation that can be seen only in the fall. 3. Scientists measure d ...
Stellar Astronomy Sample Questions for Exam 3
... 3. Describe the hunt for extra-solar planets. What kinds of techniques are used, what kinds of planets have been found, how many planets have been found, what kind of orbits do the planets have? 4. Most of the exoplanets that have been found are “hot Jupiter’s”: large gas giants orbiting very close ...
... 3. Describe the hunt for extra-solar planets. What kinds of techniques are used, what kinds of planets have been found, how many planets have been found, what kind of orbits do the planets have? 4. Most of the exoplanets that have been found are “hot Jupiter’s”: large gas giants orbiting very close ...
Astronomy Study Guide
... Apparent brightness—the brightness of a star as seen from Earth Absolute brightness—a star’s brightness as if it were a standard distance from Earth Constellation—an imaginary pattern of stars (example—Orion) Hertzsprung - Russell diagram (H-R diagram)—a graph of stars showing surface temperature on ...
... Apparent brightness—the brightness of a star as seen from Earth Absolute brightness—a star’s brightness as if it were a standard distance from Earth Constellation—an imaginary pattern of stars (example—Orion) Hertzsprung - Russell diagram (H-R diagram)—a graph of stars showing surface temperature on ...
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.