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The Universe and Galaxies - West Jefferson Local Schools
... - time is required for light to travel through space - light travels a little over 8 minutes from the sun to earth - the farther away an object/star is, the longer it takes for light to get to us, and the older the light is when it gets to us = “Light is OLD” - we see the past of other stars in the ...
... - time is required for light to travel through space - light travels a little over 8 minutes from the sun to earth - the farther away an object/star is, the longer it takes for light to get to us, and the older the light is when it gets to us = “Light is OLD” - we see the past of other stars in the ...
Spectroscopy – the study of the colors of light (the spectrum) given
... they are very visible. The distribution of types of known stars: 90% of all stars are on the main sequence, 9% of all stars are white dwarfs, 1% of all stars are red giants. ...
... they are very visible. The distribution of types of known stars: 90% of all stars are on the main sequence, 9% of all stars are white dwarfs, 1% of all stars are red giants. ...
Challenging our Understanding of Stellar Structure and Evolution
... Why? First, the ’tops’ of both stellar maps contain relatively rare objects, for which large populations are not found until the observing horizon reaches hundreds or thousands of parsecs. Second, the ’bottoms’ and ’sides’ of both maps contain stars, either intrinsically faint, or whose rarity guara ...
... Why? First, the ’tops’ of both stellar maps contain relatively rare objects, for which large populations are not found until the observing horizon reaches hundreds or thousands of parsecs. Second, the ’bottoms’ and ’sides’ of both maps contain stars, either intrinsically faint, or whose rarity guara ...
The Milky Way Galaxy
... clusters are plotted, using correct magnitudes, they form a halo around the galactic plane. • This helps us determine that the center is 8 kpc from the Solar System and that the galaxy is 30 kpc in width. HALO ...
... clusters are plotted, using correct magnitudes, they form a halo around the galactic plane. • This helps us determine that the center is 8 kpc from the Solar System and that the galaxy is 30 kpc in width. HALO ...
at A-stars?
... Are the variables plotted here related to each other? A. Yes, they show a relationship B. You can’t be sure – you don’t know what they are! C. They are related to each other or else both are related to a third variable D. Either A or C ...
... Are the variables plotted here related to each other? A. Yes, they show a relationship B. You can’t be sure – you don’t know what they are! C. They are related to each other or else both are related to a third variable D. Either A or C ...
Beyond the Solar System Homework for Geology 8
... 62. The brightness of a star when viewed from Earth is called its ____________ magnitude. 63. The true brightness of a star, which takes into account the distance from the Earth by using a standard distance, is called its ____________ magnitude. 64. A 1st (first) magnitude star is approximately ____ ...
... 62. The brightness of a star when viewed from Earth is called its ____________ magnitude. 63. The true brightness of a star, which takes into account the distance from the Earth by using a standard distance, is called its ____________ magnitude. 64. A 1st (first) magnitude star is approximately ____ ...
How We Know the Earth Revolves Activity
... How do scientists know that the Earth actually orbits (revolves about) the sun? Have you ever thought about this? For thousands of years it was thought that the Earth was at the center of the universe and that everything moved around the Earth at different rates. Today, scientists know that the Eart ...
... How do scientists know that the Earth actually orbits (revolves about) the sun? Have you ever thought about this? For thousands of years it was thought that the Earth was at the center of the universe and that everything moved around the Earth at different rates. Today, scientists know that the Eart ...
Society News - Bristol Astronomical Society
... One of the other highlights in Leo is the lovely double star gamma (γ) Leonis (Algieba), this is a great double for small telescopes. The primary is a magnitude +2.2 K-class yellow-orange giant, it’s companion is a magnitude +2.5 yellow Gclass star. The pair are separated by 4.4 arcseconds. Just to ...
... One of the other highlights in Leo is the lovely double star gamma (γ) Leonis (Algieba), this is a great double for small telescopes. The primary is a magnitude +2.2 K-class yellow-orange giant, it’s companion is a magnitude +2.5 yellow Gclass star. The pair are separated by 4.4 arcseconds. Just to ...
The Sun and the Stars
... Edmund Halley in 1716 suggested that the transit of Venus could be used to provide an accurate estimate of the Earth-Sun distance. Transits occur when the planet passes between the Earth and Sun. NB. Transits of Venus are rare, because the orbit of Venus is inclined to the ecliptic (the plane of the ...
... Edmund Halley in 1716 suggested that the transit of Venus could be used to provide an accurate estimate of the Earth-Sun distance. Transits occur when the planet passes between the Earth and Sun. NB. Transits of Venus are rare, because the orbit of Venus is inclined to the ecliptic (the plane of the ...
Lecture 3
... Edmund Halley in 1716 suggested that the transit of Venus could be used to provide an accurate estimate of the Earth-Sun distance. Transits occur when the planet passes between the Earth and Sun. NB. Transits of Venus are rare, because the orbit of Venus is inclined to the ecliptic (the plane of the ...
... Edmund Halley in 1716 suggested that the transit of Venus could be used to provide an accurate estimate of the Earth-Sun distance. Transits occur when the planet passes between the Earth and Sun. NB. Transits of Venus are rare, because the orbit of Venus is inclined to the ecliptic (the plane of the ...
Spectra of Star Clusters
... stars in many phases of life, just as we might study how humans age by observing the humans living in a village at one time. • What two basic physical properties do astronomers use to classify stars? • Stars are classified by their luminosity and surface temperature. These properties, in turn, d ...
... stars in many phases of life, just as we might study how humans age by observing the humans living in a village at one time. • What two basic physical properties do astronomers use to classify stars? • Stars are classified by their luminosity and surface temperature. These properties, in turn, d ...
Measuring Stars` Properties - Test 1 Study Guide
... • There are also stars with cool surface temperature but very large radius: RED GIANTS • Stars with hot surface temperature but very small radius: WHITE DWARVES PHYS 162 ...
... • There are also stars with cool surface temperature but very large radius: RED GIANTS • Stars with hot surface temperature but very small radius: WHITE DWARVES PHYS 162 ...
Logarithms and Earthquake Magnitude
... Earthquakes are generated by slip on a fault and this slip can range from a very small displacement on a very small patch of a fault to a slip of 10’s of meters over a fault with dimensions of 100’s of kilometers! Seismometers can measure the amplitude of the ground vibrations generated by an earthq ...
... Earthquakes are generated by slip on a fault and this slip can range from a very small displacement on a very small patch of a fault to a slip of 10’s of meters over a fault with dimensions of 100’s of kilometers! Seismometers can measure the amplitude of the ground vibrations generated by an earthq ...
Basic Properties of Stars
... If the Doppler shift of a star’s absorption lines changes with time (redshift, then blueshift, then redshift, etc.), it’s a spectroscopic binary. If one star is much fainter than the other, you may not see its lines. The object is then a singleline spectroscopic binary. If both sets of lines are see ...
... If the Doppler shift of a star’s absorption lines changes with time (redshift, then blueshift, then redshift, etc.), it’s a spectroscopic binary. If one star is much fainter than the other, you may not see its lines. The object is then a singleline spectroscopic binary. If both sets of lines are see ...
How far away are the Stars?
... • If distance to an object is known, we can measure its size. Diameter 2 Dis tan ce ...
... • If distance to an object is known, we can measure its size. Diameter 2 Dis tan ce ...
A105 Stars and Galaxies
... diameters through a telescope. Stars are so far away that we see them just as points of light. ...
... diameters through a telescope. Stars are so far away that we see them just as points of light. ...
Measuring Stars
... hilltop miles away, it appears faint – Its apparent brightness depends on its distance – Its intrinsic brightness, the amount of light it emits, is independent of distance. ...
... hilltop miles away, it appears faint – Its apparent brightness depends on its distance – Its intrinsic brightness, the amount of light it emits, is independent of distance. ...
Lecture18
... • Even with the Hipparchus we can only measure distances out to 300 LY, which is only 1% of the size of own galaxy and very small on the scale of the universe ...
... • Even with the Hipparchus we can only measure distances out to 300 LY, which is only 1% of the size of own galaxy and very small on the scale of the universe ...
Astronomy
... 3. If you live on the equator, where would the celestial equator be in your sky? It would run from East to West and directly overhead through your zenith 4. What is the difference between 1st magnitude and 2nd magnitude stars? 1st magnitude are brighter ...
... 3. If you live on the equator, where would the celestial equator be in your sky? It would run from East to West and directly overhead through your zenith 4. What is the difference between 1st magnitude and 2nd magnitude stars? 1st magnitude are brighter ...
MS Word
... luminosity). Familiarize yourself with Figure 1 which is an empty H-R diagram. Along the bottom of the diagram are the common spectral types (we have left off O type stars since there are no O stars anywhere near the Sun). Recall that each letter category is also broken into ten subcatagories. Thus ...
... luminosity). Familiarize yourself with Figure 1 which is an empty H-R diagram. Along the bottom of the diagram are the common spectral types (we have left off O type stars since there are no O stars anywhere near the Sun). Recall that each letter category is also broken into ten subcatagories. Thus ...
answer key
... 2. What is a parsec? Compare it with the astronomical unit. Astronomers measure parallax in arc seconds rather than in degrees. If we ask at what distance a star must lie in order for its observed parallax to be exactly 1", we get an answer of 206,265 A.U., or 3.1 1016 m. Astronomers call this dista ...
... 2. What is a parsec? Compare it with the astronomical unit. Astronomers measure parallax in arc seconds rather than in degrees. If we ask at what distance a star must lie in order for its observed parallax to be exactly 1", we get an answer of 206,265 A.U., or 3.1 1016 m. Astronomers call this dista ...
ph507lecnote07
... If they have the same surface brightness ( L/R2 is constant) and the same mass-to-light ratio (M/L is constant), then L ~ V4. So, provided we can measure the velocity V, certain galaxies can be used as standard candles. (determine V through the 21 cm line of atomic hydrogen in the galaxy). ...
... If they have the same surface brightness ( L/R2 is constant) and the same mass-to-light ratio (M/L is constant), then L ~ V4. So, provided we can measure the velocity V, certain galaxies can be used as standard candles. (determine V through the 21 cm line of atomic hydrogen in the galaxy). ...
Week8Lecture1
... stars in the halo are very old, and there is no gas and dust. The galactic disk is where the youngest stars are, as well as star formation regions – emission nebulae, large clouds of gas and dust. Surrounding the galactic center is the galactic bulge, which contains a mix of older and younger stars. ...
... stars in the halo are very old, and there is no gas and dust. The galactic disk is where the youngest stars are, as well as star formation regions – emission nebulae, large clouds of gas and dust. Surrounding the galactic center is the galactic bulge, which contains a mix of older and younger stars. ...
ASTR 1120 General Astronomy: Stars and Galaxies
... That’s one foot per nanosecond One Year is 3.15x107 seconds long In one year light travels 3.15x107x3x108 = 1016m This is the definition of a light year. Prox Cen is at 4ly. ...
... That’s one foot per nanosecond One Year is 3.15x107 seconds long In one year light travels 3.15x107x3x108 = 1016m This is the definition of a light year. Prox Cen is at 4ly. ...
Constellations, Star Names, and Magnitudes
... were named for their brightest star. Of the constellations defined by the Babylonians, Egyptians, and Greeks, 48 are still used today. ...
... were named for their brightest star. Of the constellations defined by the Babylonians, Egyptians, and Greeks, 48 are still used today. ...
Malmquist bias
The Malmquist bias is an effect in observational astronomy which leads to the preferential detection of intrinsically bright objects. It was first described in 1922 by Swedish astronomer Gunnar Malmquist (1893–1982), who then greatly elaborated upon this work in 1925. In statistics, this bias is referred to as a selection bias and affects the survey results in a brightness limited survey, where stars below a certain apparent brightness are not included. Since observed stars and galaxies appear dimmer when farther away, the brightness that is measured will fall off with distance until their brightness falls below the observational threshold. Objects which are more luminous, or intrinsically brighter, can be observed at a greater distance, creating a false trend of increasing intrinsic brightness, and other related quantities, with distance. This effect has led to many spurious claims in the field of astronomy. Properly correcting for these effects has become an area of great focus.