Study Guide_galaxies, Tools, and Stars Test
... 6. Name and describe the 3 types of galaxies. 7. Where is our solar system located in the Milky Way galaxy? 8. What is a light year? 9. What contains all the matter and energy that exists? 10. Name two types of optical telescopes. 11. What do radio telescopes receive and where do they come from? 12. ...
... 6. Name and describe the 3 types of galaxies. 7. Where is our solar system located in the Milky Way galaxy? 8. What is a light year? 9. What contains all the matter and energy that exists? 10. Name two types of optical telescopes. 11. What do radio telescopes receive and where do they come from? 12. ...
1 - Pitt County Schools
... 3. What factors determine a star’s apparent magnitude? ___________________________________________________________________________ ___________________________________________________________________________ 4. The H-R diagram shows the relationship between what two factors? _________________________ ...
... 3. What factors determine a star’s apparent magnitude? ___________________________________________________________________________ ___________________________________________________________________________ 4. The H-R diagram shows the relationship between what two factors? _________________________ ...
Chapter 30.1
... horizon. (Circling stars). Different stars become visible during different seasons. Three actual motions: ...
... horizon. (Circling stars). Different stars become visible during different seasons. Three actual motions: ...
2014 Joseph E. Pesce, Ph.D. 1 Astro 113 Final Exam Review 1. What
... 26. Are galaxies distributed evenly through space? 27. Why does the region of the sky called the “Milky Way” have a larger concentration of stars than other regions? 28. What is an effect of a ...
... 26. Are galaxies distributed evenly through space? 27. Why does the region of the sky called the “Milky Way” have a larger concentration of stars than other regions? 28. What is an effect of a ...
Decimal Prefixes and Multiples, Powers of Ten
... Decimal Prefixes and Multiples, Powers of Ten AND Partners Chart! Try to fill in the empty boxes for all columns EXCEPT the partners box! ...
... Decimal Prefixes and Multiples, Powers of Ten AND Partners Chart! Try to fill in the empty boxes for all columns EXCEPT the partners box! ...
Document
... And we know how bright it should be, Result Distance We do this everyday with size. ...
... And we know how bright it should be, Result Distance We do this everyday with size. ...
Parallax, angular size
... between the two telescopes (if both of them have to be on Earth – no spacecraft). ...
... between the two telescopes (if both of them have to be on Earth – no spacecraft). ...
Characteristics of Stars
... • Astronomers use a unit called the light year to measure distances between the stars • Light travels at a speed of 300,000 km/s • Light year- distance that light travels in one year =9.5 trillion km • Light year=unit of distance ...
... • Astronomers use a unit called the light year to measure distances between the stars • Light travels at a speed of 300,000 km/s • Light year- distance that light travels in one year =9.5 trillion km • Light year=unit of distance ...
The Distance Ladder I - Sierra College Astronomy Home Page
... Calibrating Cepheids The period-luminosity relationship must be calibrated by Cepheids of a known distance. It was first done by Leavitt, using stars in the LMC and SMC. In modern times, techniques such as trigonometric parallax from Hipparcos are used to refine the relationship. Happily, Cepheids ...
... Calibrating Cepheids The period-luminosity relationship must be calibrated by Cepheids of a known distance. It was first done by Leavitt, using stars in the LMC and SMC. In modern times, techniques such as trigonometric parallax from Hipparcos are used to refine the relationship. Happily, Cepheids ...
The magnitude scale, parallax, the parsec, and Cepheid distances
... • Confusingly, log10 and linear systems are both in common usage – linear e.g. Jy, makes sense for detectors that respond linearly to light (typically used in Radio astronomy) – log10 makes sense for a ...
... • Confusingly, log10 and linear systems are both in common usage – linear e.g. Jy, makes sense for detectors that respond linearly to light (typically used in Radio astronomy) – log10 makes sense for a ...
Our Place in the Universe: Sizing up the Heavens
... temperature, distance. •Color (spectrum) and apparent variations through time composition, temperature, direction of motion and velocity relative to observer. •Apparent Size and shape and variations through time stars, galaxies, nebula (clouds of dust and gas), comets, planets, etc. ...
... temperature, distance. •Color (spectrum) and apparent variations through time composition, temperature, direction of motion and velocity relative to observer. •Apparent Size and shape and variations through time stars, galaxies, nebula (clouds of dust and gas), comets, planets, etc. ...
Pre-lab 12: Galaxies and the Expansion of the Universe So far we
... galaxies becomes buried in unfathomably big numbers. So again we turn to a larger unit of measure. For distances across the universe, astronomers often measure in Megaparsecs. A Megaparsec is 1 million (106) Parsecs, and a Parsec is 3.26 light years. To get a better sense of scale of the layout of o ...
... galaxies becomes buried in unfathomably big numbers. So again we turn to a larger unit of measure. For distances across the universe, astronomers often measure in Megaparsecs. A Megaparsec is 1 million (106) Parsecs, and a Parsec is 3.26 light years. To get a better sense of scale of the layout of o ...
Measuring the distance to Galaxies
... luminous but appears only as bright as the one on the left. It must be further away The period is doubled so it is twice as luminous but its brightness is halved. It is less than twice as far away. (It will be 1.4 times as far away). ...
... luminous but appears only as bright as the one on the left. It must be further away The period is doubled so it is twice as luminous but its brightness is halved. It is less than twice as far away. (It will be 1.4 times as far away). ...
Document
... • How do we know the distance to stars and clusters in our galaxy? • Trigonometric parallax good out to 100 pc. • We believe galaxy is ~30 kpc wide. • How do we know? ...
... • How do we know the distance to stars and clusters in our galaxy? • Trigonometric parallax good out to 100 pc. • We believe galaxy is ~30 kpc wide. • How do we know? ...
Milky Way
... • From variable stars we know distances. • From Doppler shift we know rotation velocity. • Use Kepler’s Third Law (again) to get mass of the Milky Way. More than what we see. • M = 1011 x Msun ...
... • From variable stars we know distances. • From Doppler shift we know rotation velocity. • Use Kepler’s Third Law (again) to get mass of the Milky Way. More than what we see. • M = 1011 x Msun ...
Observing the Universe 3
... 8. What two things does the intrinsic (actual) brightness of a star depend on? (i) ……………………………….………………………….. (ii) ……………………………………….………………….. 9. Two stars are of the same actual brightness but one looks fainter than the other when seen from the Earth. Why is this? ...
... 8. What two things does the intrinsic (actual) brightness of a star depend on? (i) ……………………………….………………………….. (ii) ……………………………………….………………….. 9. Two stars are of the same actual brightness but one looks fainter than the other when seen from the Earth. Why is this? ...
Lecture 24 - Empyrean Quest Publishers
... How bright (L in watts)? Luminosity at the source is determined from apparent brightness and distance (d). Apparent magnitude (old way). We can see about 1,000 stars in Northern Hemisphere with naked eye. Hipparchus rated them from 1 to 6. A '1' is 2.52 x brighter than a '2', etc. Range in brightnes ...
... How bright (L in watts)? Luminosity at the source is determined from apparent brightness and distance (d). Apparent magnitude (old way). We can see about 1,000 stars in Northern Hemisphere with naked eye. Hipparchus rated them from 1 to 6. A '1' is 2.52 x brighter than a '2', etc. Range in brightnes ...
Lecture 22 - Cosmic distance scale
... • Measure and record the distances from cluster A to each of the other 5 clusters. • Measure and record the distances from cluster D to each of the other 5 clusters. • Blow up the balloon up more, to a diameter of about 6 inches. Measure the distances between the same clusters again and record them. ...
... • Measure and record the distances from cluster A to each of the other 5 clusters. • Measure and record the distances from cluster D to each of the other 5 clusters. • Blow up the balloon up more, to a diameter of about 6 inches. Measure the distances between the same clusters again and record them. ...
Measuring Distances - Stockton University
... appears to follow a fairly consistent light-curve, peaking at an absolute magnitude of about Mv -19. This makes them 23.8 magnitudes more luminous than the Sun, equivalent to a factor of 1023.8/2.5 = 3.3 x 109 . • These are now playing an important role in modern cosmology as there are large proje ...
... appears to follow a fairly consistent light-curve, peaking at an absolute magnitude of about Mv -19. This makes them 23.8 magnitudes more luminous than the Sun, equivalent to a factor of 1023.8/2.5 = 3.3 x 109 . • These are now playing an important role in modern cosmology as there are large proje ...
SO FAR:
... Observed MW rotation curve • In principle, for stars, clusters, etc: • measure distance d and vr • assume circular orbit ...
... Observed MW rotation curve • In principle, for stars, clusters, etc: • measure distance d and vr • assume circular orbit ...
TAP 705-3: The parsec - Teaching Advanced Physics
... TAP 705-3: The parsec A unit of distance in common use amongst astronomers is the parsec. As the Earth moves in its orbit around the Sun, the position of nearby stars against the background of very distant stars seems to change. ...
... TAP 705-3: The parsec A unit of distance in common use amongst astronomers is the parsec. As the Earth moves in its orbit around the Sun, the position of nearby stars against the background of very distant stars seems to change. ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.