When an object like a star or galaxy is moving relative to us, we can observe...
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When an object like a star or galaxy is moving relative to us, we can observe that the spectral lines are shifted relative to the direction that the object is moving with respect to us. If the object and observer are getting closer, the lines will be shifted a bit towards the blue end of the spectrum (blueshifted); moving apart will shift them towards the red end of the spectrum (redshifted). The interesting thing is that all of the lines will be shifted the same amount and the line pattern will be preserved so we can still identify what atoms or compounds are responsible. As the Earth orbits the Sun, a star is observed to have the dark line spectra below. Label when the earth is moving towards, away from and parallel to the star. Doppler Shift and Direction Not only will the spectral lines be redshifted or blueshifted depending on relative direction, the amount they are shifted will depend on how fast we are moving towards or away from each other. In other words, spectral lines are shifted proportional to the speed (velocity). Astronomers typically use the Hydrogen Alpha line (Ha - no joke, Ha!) to figure this out. We use the difference (A) between what wavelength it's observed to be compared to what it would be if nothing was moving (A = 656.3 nm); then we can calculate the velocity. The relationship looks like this: V=Cx (AAA) Equation 3 Where V is the velocity and C is the speed of light (3 x 108 m/s). Now we can find the how fast something is moving even if it's incredibly far away! Example: The Ha line for the absorption spectra of an object is observed to be = 656.1 nm (shorter \ so blue shifted). How fast is it going? (3 x 108 m/s) (0.2 nm 656.3 nm) = 91.4 x 103 m/s = 91.4 km/s The Ha line for the absorption spectra of an object is observed to be = 656.5 nm. Is it redshifted or blueshifted? (circle the correct one) Calculate: How fast is it going? When an object like a star or galaxy is moving relative to us, we can observe that the spectral lines are shifted relative to the direction that the object is moving with respect to us. If the object and observer are getting closer, the lines will be shifted a bit towards the blue end of the spectrum (blueshifted); moving apart will shift them towards the red end of the spectrum (redshifted). The interesting thing is that all of the lines will be shifted the same amount and the line pattern will be preserved so we can still identify what atoms or compounds are responsible. As the Earth orbits the Sun, a star is observed to have the dark line spectra below. Label when the earth is moving towards, away from and parallel to the star. Doppler Shift and Direction Not only will the spectral lines be redshifted or blueshifted depending on relative direction, the amount they are shifted will depend on how fast we are moving towards or away from each other. In other words, spectral lines are shifted proportional to the speed (velocity). Astronomers typically use the Hydrogen Alpha line (Ha - no joke, Ha!) to figure this out. We use the difference (A) between what wavelength it's observed to be compared to what it would be if nothing was moving (A = 656.3 nm); then we can calculate the velocity. The relationship looks like this: V=Cx (AAA) Equation 3 Where V is the velocity and C is the speed of light (3 x 108 m/s). Now we can find the how fast something is moving even if it's incredibly far away! Example: The Ha line for the absorption spectra of an object is observed to be = 656.1 nm (shorter \ so blue shifted). How fast is it going? (3 x 108 m/s) (0.2 nm 656.3 nm) = 91.4 x 103 m/s = 91.4 km/s The Ha line for the absorption spectra of an object is observed to be = 656.5 nm. Is it redshifted or blueshifted? (circle the correct one) Calculate: How fast is it going?
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