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Prepare your scantron:

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Presentation on theme: "Prepare your scantron:"— Presentation transcript:

1 Prepare your scantron:
Use a pencil, not a pen! Fill in your name and fill the bubbles under your name. LAST NAME FIRST, First name second Put your 4-digit code instead of “IDENTIFICATION NUMBER”. --- (The last 4 digits of your OleMiss ID.) Question # 1: answer A Question # 2: answer C Question # 3: answer C Setup: Test 2: Monday Pass/fail makeup: Today 5:00 pm Please take a moment to mute your cell phone!

2 Example: Rotational line broadening:
The details of the spectra tell a lot: • Chemical composition: from color of lines • Rotation: from width of lines • Movement (towards us or away from us): from shift of lines • Strength of magnetic field (if any): from split of lines • Temperature, gravity, wind speed, …: from detailed structure of lines Example: Rotational line broadening: What do spectra tell us?

3 Example: a rotating galaxy
The top of the slit shows blueshift - - stars there are moving towards us The bottom of the slit shows redshift - - stars there are moving away: Example: a rotating galaxy Example: This galaxy rotates!

4 Questions coming …

5 sec 10 9 11 12 15 14 13 8 7 1 2 3 5 4 6 16 26 17 27 28 30 29 24 25 23 19 18 20 21 22 Question 4 How do we know that galaxies rotate? A Their spectral lines are broad. B The spectral lines of different parts of the galaxy show different red- and blueshift. C The shape of a galaxy changes in a few years. Next question coming …

6 sec 10 9 11 13 14 8 12 7 2 1 3 4 6 5 15 17 26 25 27 28 30 29 16 24 19 18 23 20 22 21 Question 5 How will the rotation of a star affect its spectrum? A Spectral lines get blueshifted. B Spectral lines get redshifted. C Spectral lines broaden. D The spectral lines are not affected, but the stars overall color changes.

7 Spectroscopic binaries
Measure: * Blue/red shift of lines * Time period Earth Calculate: * Orbital speed ( shift in % of wavelength = speed in % of speed of light ) * Size of orbit ( time period × speed = 2 r p ) * Mass of stars ( Kepler III: M × T2 = r3 )

8 Questions coming …

9 sec 10 9 11 12 15 14 13 8 7 1 2 3 5 4 6 16 26 17 27 28 30 29 24 25 23 19 18 20 21 22 Question 6 How do we know the mass of (some) stars? A Using measurements of their planets. B Using measurements of the force of their gravity on spaceships. C Using the red/blue shift of spectral lines of double stars. D Using measurements of their brightness and color. Next question coming …

10 sec 8 9 10 12 11 7 6 1 2 3 4 13 30 35 40 45 14 25 16 15 18 17 19 20 5 Question 7 In a star’s spectrum all the hydrogen lines are shifted towards red, and all the metal (sodium, calcium, etc. ) lines are blueshifted. This could be explained by the following situation: A The hydrogen in the star’s atmosphere is hotter than the metals. B The hydrogen in the star’s atmosphere is colder than the metals. C The star is a double, consisting of a regular star A plus a metal-reach star B. Star A is moving away from us, star B is approaching us as they revolve. D The star is a double, consisting of a regular star A plus a metal-reach star B. Star B is moving away from us, star A is approaching us as they revolve.

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