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Measuring Distance in our Universe. Due Tue 1 Dec 2009 Imagine
... Imagine that you could travel to the stars at the speed of light. It would take 8 minutes to get to the Sun from Earth. To get to the next nearest star, Proxima Centauri, it would take 4.2 years traveling at the speed of light. Distances on earth are often measured in kilometers but distances to the ...
... Imagine that you could travel to the stars at the speed of light. It would take 8 minutes to get to the Sun from Earth. To get to the next nearest star, Proxima Centauri, it would take 4.2 years traveling at the speed of light. Distances on earth are often measured in kilometers but distances to the ...
How Far? - Science A 2 Z
... As light moves away, the waves stretch out Longer waves are shifted towards the red As light moves towards us, the waves condense Shorter waves are shifted towards the blue ...
... As light moves away, the waves stretch out Longer waves are shifted towards the red As light moves towards us, the waves condense Shorter waves are shifted towards the blue ...
Abs-Apar Mag
... – A ranking system – Brightest stars = 1st class, then 2nd, 3rd… – 6th magnitude are faintest stars seen at night – Result: lower number = brighter “There is no other rule for classing the stars but the estimation of the observer; and hence it is that some astronomers reckon those stars of the first ...
... – A ranking system – Brightest stars = 1st class, then 2nd, 3rd… – 6th magnitude are faintest stars seen at night – Result: lower number = brighter “There is no other rule for classing the stars but the estimation of the observer; and hence it is that some astronomers reckon those stars of the first ...
The measure of Cosmological distances
... 1917: Shapley & Hertzsprung measured the distance to a Cepheid allow the use of Cepheids as “Standard candles” 1918: Harlow Shapely measures the milky way ...
... 1917: Shapley & Hertzsprung measured the distance to a Cepheid allow the use of Cepheids as “Standard candles” 1918: Harlow Shapely measures the milky way ...
Characteristics of Stars
... Classification • H-R diagram • Absolute magnitude vs. temperature • For most stars the brightness increases as surface temp increases • Main sequence stars are band in center ...
... Classification • H-R diagram • Absolute magnitude vs. temperature • For most stars the brightness increases as surface temp increases • Main sequence stars are band in center ...
Distances in Space
... Andromeda have exploded as a supernova or gone out long ago. The message of these star finishing events just has not gotten to us yet! ...
... Andromeda have exploded as a supernova or gone out long ago. The message of these star finishing events just has not gotten to us yet! ...
properties of stars 2012
... So… if apparent brightness is determined (by using a light meter) and d is known (perhaps by parallax), luminosity can be determined. Apparent Magnitude: Hipparchus, in 150 B.C. classified stars by magnitude, with 1 being the brightest, and six being the dimmest. With the advent of technology, brigh ...
... So… if apparent brightness is determined (by using a light meter) and d is known (perhaps by parallax), luminosity can be determined. Apparent Magnitude: Hipparchus, in 150 B.C. classified stars by magnitude, with 1 being the brightest, and six being the dimmest. With the advent of technology, brigh ...
The Diversity and Unity of Life- A Paradox
... that, by comparison, planets and stars and galaxies seem achingly rare and lovely. If we were randomly inserted into the Cosmos, the chance that we would find ourselves on or near a planet would be less than one in a billion trillion trillion. In everyday life such odds are called compelling. Worlds ...
... that, by comparison, planets and stars and galaxies seem achingly rare and lovely. If we were randomly inserted into the Cosmos, the chance that we would find ourselves on or near a planet would be less than one in a billion trillion trillion. In everyday life such odds are called compelling. Worlds ...
Study Guide
... Name: ___________________ Period: ___________________ Date: ___________________ What is a Black Hole and how do Black Holes form? ...
... Name: ___________________ Period: ___________________ Date: ___________________ What is a Black Hole and how do Black Holes form? ...
Stellar Masses
... Problems in measuring Distances • Zero Point Error:-If we make a mistake in measuring the distance to a primary indicator then this error is propagated up the chain of distance measurements[The Cosmological Distance Ladder] since the value of M for the secondary indicator has been derived assuming ...
... Problems in measuring Distances • Zero Point Error:-If we make a mistake in measuring the distance to a primary indicator then this error is propagated up the chain of distance measurements[The Cosmological Distance Ladder] since the value of M for the secondary indicator has been derived assuming ...
The extragalactic universe and distance measurements
... parallax out to 50pc. • Hipparcos satellite – Designed to measure parallax of stars – Can detect wobble out to distance of about 1kpc (1000pc) – Used to map out locations of nearby stars. ...
... parallax out to 50pc. • Hipparcos satellite – Designed to measure parallax of stars – Can detect wobble out to distance of about 1kpc (1000pc) – Used to map out locations of nearby stars. ...
PHY 150
... Astronomers conclude that there are vast quantities of dark matter surrounding our Galaxy because the rotation curve is fairly flat. This curve requires that a large amount of dark matter lies outside of the Sun’s orbit. ...
... Astronomers conclude that there are vast quantities of dark matter surrounding our Galaxy because the rotation curve is fairly flat. This curve requires that a large amount of dark matter lies outside of the Sun’s orbit. ...
Problem set 1 1. The binding energy per nucleon for 56Fe is 8.8MeV
... 1. The binding energy per nucleon for 56 Fe is 8.8 MeV per nucleon. Estimate the total energy released per kilogram of matter by the sequence of reactions which fuse hydrogen to iron. 2. The main sequence of the Pleiades cluster of stars consists of stars with mass less than 6M ; the more massive s ...
... 1. The binding energy per nucleon for 56 Fe is 8.8 MeV per nucleon. Estimate the total energy released per kilogram of matter by the sequence of reactions which fuse hydrogen to iron. 2. The main sequence of the Pleiades cluster of stars consists of stars with mass less than 6M ; the more massive s ...
PDF Version
... square of the distance from us to the star. Astronomers used Cepheid variables in a nearby galaxy, which are all about the same distance from us, to find the correlation between the period and the intrinsic brightness. They also measured the distances to the nearest Cepheid variables using the paral ...
... square of the distance from us to the star. Astronomers used Cepheid variables in a nearby galaxy, which are all about the same distance from us, to find the correlation between the period and the intrinsic brightness. They also measured the distances to the nearest Cepheid variables using the paral ...
Absolute Magnitudes of Supernovae
... Determining Absolute Magnitudes. On the accompanying pages are the light curves of nine Type Ia supernovae that appear in galaxies during the years 1994-1996 (Type 1a supernovae are a particular type of exploding star that contains no hydrogen lines in its spectrum). The units on the x-axis are days ...
... Determining Absolute Magnitudes. On the accompanying pages are the light curves of nine Type Ia supernovae that appear in galaxies during the years 1994-1996 (Type 1a supernovae are a particular type of exploding star that contains no hydrogen lines in its spectrum). The units on the x-axis are days ...
Earth in the Solar System - San Diego Unified School District
... d. ____________________ are the source of ______________________ for all bright objects in outer space and that the ____________________ and _________________ shine by _________________________________, NOT their own _________________. ...
... d. ____________________ are the source of ______________________ for all bright objects in outer space and that the ____________________ and _________________ shine by _________________________________, NOT their own _________________. ...
Distance measures - ScienceEducationatNewPaltz
... The closer a star is to us, the larger its angle of parallax will be. Astronomers have defined a standard unit of distance to be the parsec (pc). One parsec is the distance to a point in space that subtends a parallax angle of one arc second. This produces the simple but effective relationship: dist ...
... The closer a star is to us, the larger its angle of parallax will be. Astronomers have defined a standard unit of distance to be the parsec (pc). One parsec is the distance to a point in space that subtends a parallax angle of one arc second. This produces the simple but effective relationship: dist ...
distmeasures
... As you may have guessed in your answer to the previous question, the basic units of distance you use everyday can be unwieldy when describing the distances to celestial objects. You will not become familiar with some common astronomical distances measures. In the solar system, it is convenient to us ...
... As you may have guessed in your answer to the previous question, the basic units of distance you use everyday can be unwieldy when describing the distances to celestial objects. You will not become familiar with some common astronomical distances measures. In the solar system, it is convenient to us ...
DISTANCE MEASURES EXERCISE The goal of this exercise is to
... As you may have guessed in your answer to the previous question, the basic units of distance you use everyday can be unwieldy when describing the distances to celestial objects. You will not become familiar with some common astronomical distances measures. In the solar system, it is convenient to us ...
... As you may have guessed in your answer to the previous question, the basic units of distance you use everyday can be unwieldy when describing the distances to celestial objects. You will not become familiar with some common astronomical distances measures. In the solar system, it is convenient to us ...
21structure1i
... photometry to get the spectral type and the apparent magnitude (m) of a star We can estimate the absolute magnitude (M) from the spectral type With the two magnitudes we can get the distance: m-M = 5 log d - 5 Example: We know how bright an A0 should be, so we can find its distance by how bright ...
... photometry to get the spectral type and the apparent magnitude (m) of a star We can estimate the absolute magnitude (M) from the spectral type With the two magnitudes we can get the distance: m-M = 5 log d - 5 Example: We know how bright an A0 should be, so we can find its distance by how bright ...
ppt
... objects actually are; it measures how bright they appear to us, which also depends on how close they are eg Sun has m = -26.74 • Absolute magnitude - measures how bright objects actually are -- it is defined as the apparent magnitude that an object would have if it were located at a distance of 10 p ...
... objects actually are; it measures how bright they appear to us, which also depends on how close they are eg Sun has m = -26.74 • Absolute magnitude - measures how bright objects actually are -- it is defined as the apparent magnitude that an object would have if it were located at a distance of 10 p ...
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.