The Milky Way Galaxy
... Shapley determined the distances to a number of globular clusters using the period-luminosity law for Cepheids. He noted that most globular clusters had linear diameters of about 25 pc. He could then use their angular diameters to get approximate distance for clusters whose stars were too faint to ...
... Shapley determined the distances to a number of globular clusters using the period-luminosity law for Cepheids. He noted that most globular clusters had linear diameters of about 25 pc. He could then use their angular diameters to get approximate distance for clusters whose stars were too faint to ...
The Sun and Other Stars - Tuslaw Local School District
... Life of a star • How long a star lives depends on its mass *small mass stars use up their fuel more slowly than large mass stars, so they have much longer lives • Medium mass stars like the sun live about 10 by • Small mass stars may live 200 by • A large mass star 15 x’s as massive as the sun may ...
... Life of a star • How long a star lives depends on its mass *small mass stars use up their fuel more slowly than large mass stars, so they have much longer lives • Medium mass stars like the sun live about 10 by • Small mass stars may live 200 by • A large mass star 15 x’s as massive as the sun may ...
ph607-14-a3uni - University of Kent
... in solar masses per year. 3. Describe the colour, stellar population and gas content of E, SO and Irr galaxies. 4. Explain the difference between the monolithic and hierarchical theories for the ...
... in solar masses per year. 3. Describe the colour, stellar population and gas content of E, SO and Irr galaxies. 4. Explain the difference between the monolithic and hierarchical theories for the ...
Objects in the Sky
... • GLE 0107.6.1 Compare and describe features of the day and night sky. • GLE 0107.6.2 Realize that the sun can only be seen during the day, while the moon can be seen at night and sometimes during the day. • 0107.6.2 Identify objects in the sky and describe their observable similarities and differen ...
... • GLE 0107.6.1 Compare and describe features of the day and night sky. • GLE 0107.6.2 Realize that the sun can only be seen during the day, while the moon can be seen at night and sometimes during the day. • 0107.6.2 Identify objects in the sky and describe their observable similarities and differen ...
Cosmic Survey PowerPoint
... Telescope is beyond the orbit of the Moon...but it’s actually only 350 miles high. That’s high enough for a clear view above the Earth’s atmosphere...but low enough to enable it to be serviced by the astronauts aboard the space shuttle. Many people think the beautiful Pleiades cluster of stars must ...
... Telescope is beyond the orbit of the Moon...but it’s actually only 350 miles high. That’s high enough for a clear view above the Earth’s atmosphere...but low enough to enable it to be serviced by the astronauts aboard the space shuttle. Many people think the beautiful Pleiades cluster of stars must ...
Study Guide Ch10,11 and 12
... 8. Be able to identify a galaxy by its shape, according to the Hubble sequence. 9. Compare and contrast elliptical galaxies and spiral galaxies. 10. Describe the different types of active galaxies, and the mechanisms proposed to explain their energy output and other characteristics. 11. Briefly rela ...
... 8. Be able to identify a galaxy by its shape, according to the Hubble sequence. 9. Compare and contrast elliptical galaxies and spiral galaxies. 10. Describe the different types of active galaxies, and the mechanisms proposed to explain their energy output and other characteristics. 11. Briefly rela ...
Stellar Evolution and the HR Diagram – Study Guide
... phosphorus, magnesium, iron, and calcium that make up our bodies. So we really are made of atoms that were formed first in the dying explosions of long dead stars. 30. MINI-Essay: How is a supernova both a beginning and an end? Supernovae are the result of the death of a star that can no longer car ...
... phosphorus, magnesium, iron, and calcium that make up our bodies. So we really are made of atoms that were formed first in the dying explosions of long dead stars. 30. MINI-Essay: How is a supernova both a beginning and an end? Supernovae are the result of the death of a star that can no longer car ...
30-2 Directed Reading
... c. the main-sequence stage d. the nebula stage _____ 16. A star that has the same mass as the sun’s mass a. stays on the main sequence for about 10 million years. b. stays on the main sequence for about 10 billion years. c. stays on the main sequence for about 14 billion years. d. stays on the main ...
... c. the main-sequence stage d. the nebula stage _____ 16. A star that has the same mass as the sun’s mass a. stays on the main sequence for about 10 million years. b. stays on the main sequence for about 10 billion years. c. stays on the main sequence for about 14 billion years. d. stays on the main ...
Clase-06_Star_Formation - Departamento de Astronomía
... SF galaxies also emit in cm radio waveband, much of which must be connected, directly or no, with SF Mechanism: emission is nonthermal, from synchrotron process (accelerated particles, perhaps in SNe remnants, radiating while spiralling through large-scale magnetic fields) radio emission is a ...
... SF galaxies also emit in cm radio waveband, much of which must be connected, directly or no, with SF Mechanism: emission is nonthermal, from synchrotron process (accelerated particles, perhaps in SNe remnants, radiating while spiralling through large-scale magnetic fields) radio emission is a ...
The Hidden Lives of Galaxies NSTA 2001
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
life cycle of stars
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
... • Under collapse, protons and electrons combine to form neutrons. • 10 Km across Black Hole (If mass of core > 5 x Solar) • Not even compacted neutrons can support weight of very massive stars. ...
PH607 – Galaxies 1
... regions, or is produced by energetic electrons moving in magnetic fields Near Infrared: Most of the emission at these wavelengths is from relatively cool giant K stars in the disk and bulge X-rays: extended soft X-ray emission is detected from hot, shocked gas. At the lower energies especially, the ...
... regions, or is produced by energetic electrons moving in magnetic fields Near Infrared: Most of the emission at these wavelengths is from relatively cool giant K stars in the disk and bulge X-rays: extended soft X-ray emission is detected from hot, shocked gas. At the lower energies especially, the ...
Earths Place in the Universe
... 2. Explain the theory dealing with the origin of the solar system. 3. Using the following words; identify, explain, name, what, and discuss to ...
... 2. Explain the theory dealing with the origin of the solar system. 3. Using the following words; identify, explain, name, what, and discuss to ...
Types of Stars
... The brightness of a star as viewed from Earth is dependent on many factors such as color intensity and distance. Apparent Brightness – is the brightness of a star as it appears from Earth. The apparent brightness decreases as its distance from you increases Absolute Brightness – is how bright a star ...
... The brightness of a star as viewed from Earth is dependent on many factors such as color intensity and distance. Apparent Brightness – is the brightness of a star as it appears from Earth. The apparent brightness decreases as its distance from you increases Absolute Brightness – is how bright a star ...
PHYSICS 113 Assignment #9 SOLUTIONS Chapter 17 13. Starting
... clusters all have approximately the same absolute brightness (i.e. luminosity). These methods work up to distances of nearly one Gpc (= 1,000 Mpc). (vii) The distances to the most remote objects in the universe (e.g. quasars) are found by measuring the redshift of those objects and then by convertin ...
... clusters all have approximately the same absolute brightness (i.e. luminosity). These methods work up to distances of nearly one Gpc (= 1,000 Mpc). (vii) The distances to the most remote objects in the universe (e.g. quasars) are found by measuring the redshift of those objects and then by convertin ...
PART 3 Galaxies
... Compared to stars like the Sun in the disk of the Milky Way, stars that populate the extended spheroidal halo of the galaxy were born a) earlier, so have had time to accumulate more heavy elements. b) later, so have used up their heavy elements. c) earlier, from more nearly primordial material, so h ...
... Compared to stars like the Sun in the disk of the Milky Way, stars that populate the extended spheroidal halo of the galaxy were born a) earlier, so have had time to accumulate more heavy elements. b) later, so have used up their heavy elements. c) earlier, from more nearly primordial material, so h ...
White Dwarf Stars - University of California Observatories
... • These objects act as cosmic clocks and are useful for ...
... • These objects act as cosmic clocks and are useful for ...
PH607lec10
... regions, or is produced by energetic electrons moving in magnetic fields Near Infrared: Most of the emission at these wavelengths is from relatively cool giant K stars in the disk and bulge X-rays: extended soft X-ray emission is detected from hot, shocked gas. At the lower energies especially, the ...
... regions, or is produced by energetic electrons moving in magnetic fields Near Infrared: Most of the emission at these wavelengths is from relatively cool giant K stars in the disk and bulge X-rays: extended soft X-ray emission is detected from hot, shocked gas. At the lower energies especially, the ...
Constellations Jeopardy
... “Distances from the sun to the inner planets are like the distance from city hall to other businesses in town, while distances from the sun to the outer planets are like the distance between city hall and other distance cities within the state” is an example of this. C 500 ...
... “Distances from the sun to the inner planets are like the distance from city hall to other businesses in town, while distances from the sun to the outer planets are like the distance between city hall and other distance cities within the state” is an example of this. C 500 ...
Topic E: Astrophysics E1 Introduction to the Universe.
... Defined by making a triangle between the Earth, the Sun and a distant object. If the angle at the distant object is 1 arcsec then it would be 1 parsec away. (more later) E.1.2 - Distinguish between a stellar cluster and a constellation E.1.4 - Compare the relative distances between stars within a ...
... Defined by making a triangle between the Earth, the Sun and a distant object. If the angle at the distant object is 1 arcsec then it would be 1 parsec away. (more later) E.1.2 - Distinguish between a stellar cluster and a constellation E.1.4 - Compare the relative distances between stars within a ...
Stellar Evolution: After the Main Sequence
... surrounded by a shell through which hydrogen fusion works its way outward in the star • The core shrinks and becomes hotter, while the star’s outer layers expand and cool • The result is a red giant star ...
... surrounded by a shell through which hydrogen fusion works its way outward in the star • The core shrinks and becomes hotter, while the star’s outer layers expand and cool • The result is a red giant star ...
The Scale of the Cosmos
... a star, large enough to be spherical and to have cleared its orbital zone of other objects 7. Star – a self-luminous ball of has gas that generates its own energy by nuclear fusion ...
... a star, large enough to be spherical and to have cleared its orbital zone of other objects 7. Star – a self-luminous ball of has gas that generates its own energy by nuclear fusion ...
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.