Distances. Parallax Near objects appear to move more than far objects against a distant horizon....
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Transcript of Distances. Parallax Near objects appear to move more than far objects against a distant horizon....
![Page 1: Distances. Parallax Near objects appear to move more than far objects against a distant horizon. Trigonometric parallax is used to measure distance to.](https://reader030.fdocuments.us/reader030/viewer/2022032523/56649d775503460f94a59b81/html5/thumbnails/1.jpg)
Distances
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Parallax
• Near objects appear to move more than far objects against a distant horizon.
• Trigonometric parallax is used to measure distance to near stars.
Earth’s orbit
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time B distant starsnear stars
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Parsec
• Stellar distances are inversely proportional to the parallax angle.
– Earth’s radius fixed
– Define distance by angle
• The parsec (pc) is the distance that would result in one arc second of parallax.
– 1 pc = 3.086 1016 m
– 1 pc = 2.06 105 AU
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Near Stars
• The Hipparcos satellite measured parallax of 118,000 stars.
– Resolution: 0.001 arc-second and 0.2% luminosity.
• Gaia launches in 2011 to measure 109 stars in the galaxy
Arcturus 11.3 pc (ESA)
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Spectroscopic Parallax
• The Hipparcos data provides very precise distances.
– Use for absolute magnitudes
– Precise HR diagram
• Distant stars can be fit on the main sequence.
– Measure luminosity and apparent magnitude
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Star Clusters
• Spectroscopic parallax assumes stars on the main sequence.
– Better to average stars at the same distance
• Globular clusters are dense with 100,000 stars in a 20-100 pc region with less than 0.3 pc separating the stars.
• Open clusters tend to be smaller and younger.
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Cluster Types
Type I Clusters
– Hot young stars
– Lots of gas and dust
– Abundant in heavy elements
• Active star formation
Type II Clusters
– Old red stars
– No gas and dust
– Few heavy elements
• No star formation, just old stars
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Standard Candle
• Up to 30 pc distance is measured with parallax.
– Less certainty to 300 pc
– Longer distances by spectroscopic parallax
• The best measure of large distances are variable stars.
– Luminosity directly related to the period.
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Vibrational Modes
• Thermal motion in a star relates the speed to potential energy.
• Radial pressure waves move at the speed of sound.
• The period of vibration is inversely proportional to the square root of the density.
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Cepheid Variables
• Cepheid variables are massive relatively cool stars.
– ~ 4 to 15 M
– Color classification F to K
• The period and apparent luminosity determine the distance.
• Density ~ 10-3 kg/m3
• Vibrational period ~ 106 s
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RR Lyrae Variables
• RR Lyrae variables are short period white variables.
– ~ 1 M
– Color classification A
• These are type I stars.
– Found in globular clusters
– Useful for galactic distances
• Density ~ 10 kg/m3
• Vibrational period ~ 4 104 s
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Variables in M3
RR Lyrae stars in one night time lapse
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Instability Strip
• Cepheid and RR Lyrae stars fall in a narrow band on the HR diagram.
– Instability strip
– Not on main sequence
• As stars pass through band they oscillate.
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Band of Stars
• The sun is in a galaxy called the Milky Way.
– Observed as a diffuse band
– Millions of stars in a telescope
• The Milky Way is thicker in some directions.
– Appears as a band across the sky
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Disk
• The band of the Milky Way is the same view a viewer would have sitting inside a disk of stars.
• This disk has type I stars with gas and dust.
top view side view
sun sun
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Halo
• Astronomers measure the distance to globular clusters.
• Type II globular clusters are in a sphere around one point.
• This sphere is the galactic halo.
• The center of the sphere is the center of the galaxy.
sun globular clusters
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Size and Shape
• To view the galaxy from inside, we
– measure the distance to globular clusters
– measure distributions of hydrogen gas in the disk.
• The Milky Way is 50,000 pc across with a central bulge.
• The stars group in arms.
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Galactic Structure
• The galactic nucleus is bright and massive.
• It is obscured by the dust of the galactic disk.
• The Milky Way is probably similar to M83.