Study Guide for the 4TH Astronomy Exam
... Stellar Evolution The successful student will be able to… 1. Star Formation a. Describe the physical characteristics of a giant molecular cloud b. Identify the source of heating (energy production) in protostars c. Explain why more low-mass K & M main sequence stars form rather than the high-mass O ...
... Stellar Evolution The successful student will be able to… 1. Star Formation a. Describe the physical characteristics of a giant molecular cloud b. Identify the source of heating (energy production) in protostars c. Explain why more low-mass K & M main sequence stars form rather than the high-mass O ...
Lecture 2
... much longer than that (it is about half way through its 10 billion year life) because it gets energy from nuclear reactions in its core, but when this source runs it will contract to become a white dwarf. It is the same for all other stars and in fact the more massive ones have much shorter lives wh ...
... much longer than that (it is about half way through its 10 billion year life) because it gets energy from nuclear reactions in its core, but when this source runs it will contract to become a white dwarf. It is the same for all other stars and in fact the more massive ones have much shorter lives wh ...
The Solar System
... systems), outflows and jets. • Disperse their cocoon to become visible. • Typically form in clusters, dominated by light from 1–2 brightest members. GENS4001 Astronomy ...
... systems), outflows and jets. • Disperse their cocoon to become visible. • Typically form in clusters, dominated by light from 1–2 brightest members. GENS4001 Astronomy ...
Topic 3 – Waves and the Universe
... objects (by pointing the telescope at a fixed point for hours) As already mentioned in earlier topics, most objects give out energy in all parts of the electromagnetic spectrum Modern telescopes can be designed to detect almost any part of the spectrum, showing us things that can’t be detected usin ...
... objects (by pointing the telescope at a fixed point for hours) As already mentioned in earlier topics, most objects give out energy in all parts of the electromagnetic spectrum Modern telescopes can be designed to detect almost any part of the spectrum, showing us things that can’t be detected usin ...
Topic 3 notes - WordPress.com
... objects (by pointing the telescope at a fixed point for hours) As already mentioned in earlier topics, most objects give out energy in all parts of the electromagnetic spectrum Modern telescopes can be designed to detect almost any part of the spectrum, showing us things that can’t be detected usin ...
... objects (by pointing the telescope at a fixed point for hours) As already mentioned in earlier topics, most objects give out energy in all parts of the electromagnetic spectrum Modern telescopes can be designed to detect almost any part of the spectrum, showing us things that can’t be detected usin ...
HNRS 227 Lecture #2 Chapters 2 and 3
... Young star clusters give insight into star formation and evolution Newborn stars may form an open or galactic cluster Stars are held together in such a cluster by gravity Occasionally a star moving more rapidly than average will escape, or leave the cluster A stellar association is a group ...
... Young star clusters give insight into star formation and evolution Newborn stars may form an open or galactic cluster Stars are held together in such a cluster by gravity Occasionally a star moving more rapidly than average will escape, or leave the cluster A stellar association is a group ...
Chapter 20 The Universe
... Sirius (Dog star) only 9 light years away Proxima Centauri (closest) 4.25 light yrs Other than sun Galaxy- large grouping of stars -our solar system is part of Milky Way Galaxy - what we see as the Milky Way is only the edge (spiral galaxy) ...
... Sirius (Dog star) only 9 light years away Proxima Centauri (closest) 4.25 light yrs Other than sun Galaxy- large grouping of stars -our solar system is part of Milky Way Galaxy - what we see as the Milky Way is only the edge (spiral galaxy) ...
This link is in pdf format for ease of reading
... stars to form -- enough to produce a few hundred to a few thousand new stars. Giant molecular clouds last for 10 to 100 million years before they dissipate. ...
... stars to form -- enough to produce a few hundred to a few thousand new stars. Giant molecular clouds last for 10 to 100 million years before they dissipate. ...
6. Molecules other than CO, high density tracers
... The molecular component is much more important in starbursts and ULIRGs; it is not the case for the HI component It explains the considerable enhancement in star forming efficiency Not only a problem of gas excitation, density or temperature, since all gas density tracers confirm the large H2 abunda ...
... The molecular component is much more important in starbursts and ULIRGs; it is not the case for the HI component It explains the considerable enhancement in star forming efficiency Not only a problem of gas excitation, density or temperature, since all gas density tracers confirm the large H2 abunda ...
WIRO: Spectral Analysis P1
... proximity to the University of Wyoming, and (5) pre-existing road, electricity and phone lines since Jelm was formerly used by the US Forest Service and BLM as a fire lookout station. ...
... proximity to the University of Wyoming, and (5) pre-existing road, electricity and phone lines since Jelm was formerly used by the US Forest Service and BLM as a fire lookout station. ...
Star Study Guide Chapter 21 Test
... shows the relationship between absolute brightness and surface temperature of a star ...
... shows the relationship between absolute brightness and surface temperature of a star ...
THE HR DIAGRAM
... stars and came up with very similar results. A Danish astronomer, Ejnar Hertzsprung, plotted stars according to their absolute magnitudes and spectral classes. An American astronomer, Henry Norris Russell, created a plot of luminosity vs. temperature for many stars. Their investigations were seen as ...
... stars and came up with very similar results. A Danish astronomer, Ejnar Hertzsprung, plotted stars according to their absolute magnitudes and spectral classes. An American astronomer, Henry Norris Russell, created a plot of luminosity vs. temperature for many stars. Their investigations were seen as ...
Characteristics of Stars
... Use pages 793-799 in the textbook to find the answers to the questions below. Use the back of this page or a separate pieced of binder paper if you need more room. 1. How long would it take to travel to the Sun at light speed? How long would it take to travel to the nearest star if you could travel ...
... Use pages 793-799 in the textbook to find the answers to the questions below. Use the back of this page or a separate pieced of binder paper if you need more room. 1. How long would it take to travel to the Sun at light speed? How long would it take to travel to the nearest star if you could travel ...
Module G - U1_ L3 - Life Cycle of Stars
... • Energy is transferred to a thin shell of hydrogen surrounding the core, where hydrogen fusion continues and the shell expands. • When fusion ends completely, the star begins to eject matter, until only the core remains. What is the life cycle of a low-mass star? • The outward pressure generated by ...
... • Energy is transferred to a thin shell of hydrogen surrounding the core, where hydrogen fusion continues and the shell expands. • When fusion ends completely, the star begins to eject matter, until only the core remains. What is the life cycle of a low-mass star? • The outward pressure generated by ...
A Universe of Dwarfs and Giants
... (or HR diagram). It is a very important tool in Astrophysics. You can see that the diagram is divided into several groups. The most important one being the ‘main sequence’ which runs from the top left to the bottom right. Our Sun is a G type main sequence star. Only about 8% of all stars are G type ...
... (or HR diagram). It is a very important tool in Astrophysics. You can see that the diagram is divided into several groups. The most important one being the ‘main sequence’ which runs from the top left to the bottom right. Our Sun is a G type main sequence star. Only about 8% of all stars are G type ...
Main Sequence Star
... – Concave mirror reflects light to a flat mirror – Ex. Hubble Space Telescope • Hale telescope ...
... – Concave mirror reflects light to a flat mirror – Ex. Hubble Space Telescope • Hale telescope ...
Astronomy Review
... 28. The ___________________________ planets are relatively small and rocky. 29. True or False The Jovian planets are huge, rocky giants. 30. A(n) _______________________________ is a cloud of dust and gas in space. 31. The Jovian planets contain large quantities of ices because it was ______________ ...
... 28. The ___________________________ planets are relatively small and rocky. 29. True or False The Jovian planets are huge, rocky giants. 30. A(n) _______________________________ is a cloud of dust and gas in space. 31. The Jovian planets contain large quantities of ices because it was ______________ ...
Electromagnetic Radiation from the Sun
... 6. Why is information about many stars contained in absorption rather than emission spectra? If there is a cloud of gas at a cooler temperature directly between a denser source producing a continuous spectrum (i.e. a star) and a telescope, the gas will absorb light at specific wavelengths that are ...
... 6. Why is information about many stars contained in absorption rather than emission spectra? If there is a cloud of gas at a cooler temperature directly between a denser source producing a continuous spectrum (i.e. a star) and a telescope, the gas will absorb light at specific wavelengths that are ...
Fingerprints in Starlight: Spectroscopy of Stars Inquiry Questions
... atoms in cool stars only have electrons in the ground state. Very hot stars contain hydrogen that that is either ionized or with electrons excited to higher energy levels. In both cases the stars will have weak Balmer absorption lines. 6. Why is information about many stars contained in absorption ...
... atoms in cool stars only have electrons in the ground state. Very hot stars contain hydrogen that that is either ionized or with electrons excited to higher energy levels. In both cases the stars will have weak Balmer absorption lines. 6. Why is information about many stars contained in absorption ...
Stars - TeacherWeb
... how bright a star would be if all of the stars were the same distance from Earth. ...
... how bright a star would be if all of the stars were the same distance from Earth. ...
The Life Cycle of the Stars
... atoms to begin fusing into helium, thereby releasing energy and raising the temperature at the core to over 15 million degrees. Another star was born, and the Sun began to glow. The birth of all stars is much like that of the Sun, but the mass of the gas and dust comprising the star will determine i ...
... atoms to begin fusing into helium, thereby releasing energy and raising the temperature at the core to over 15 million degrees. Another star was born, and the Sun began to glow. The birth of all stars is much like that of the Sun, but the mass of the gas and dust comprising the star will determine i ...
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.