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$### Spectroscopy in Astronomy **2.9) Explain how astronomers might use spectroscopy to determine the composition and temperature of a star.** #### Spectroscopy and Its Application in Astronomy Spectroscopy is a powerful analytical technique used by astronomers to gather information about the materials composing astronomical objects and their physical conditions, such as temperature. By analyzing the light emitted or absorbed by a star, researchers can deduce its properties as follows: 1. **Composition**: - **Emission and Absorption Lines**: When light from a star passes through a prism or a diffraction grating, it splits into its constituent colors, forming a spectrum. Spectra can show dark lines known as absorption lines or bright lines called emission lines at specific wavelengths. These lines correspond to the energies required for electrons to change energy levels in atoms and molecules. - **Chemical Fingerprint**: Each chemical element has a unique set of spectral lines, acting as a fingerprint. By identifying these lines, astronomers can determine the presence of specific elements within the star. 2. **Temperature**: - **Blackbody Radiation**: Stars emit light across a range of wavelengths, forming a continuous spectrum that approximates blackbody radiation. The peak wavelength of this spectrum shifts according to the temperature of the star (Wien's Law). - **Color Index**: The overall color of the star (blue or red) can give information about its temperature. Hotter stars emit more blue light, and cooler stars emit more red light. - **Line Broadening**: The width of spectral lines can also provide temperature information. Higher temperatures cause more thermal motion among atoms, broadening the spectral lines. By analyzing both the continuous spectrum for temperature and the discrete spectral lines for composition, astronomers can gather a comprehensive understanding of a star’s physical characteristics.$

Transcribed Image Text:### Spectroscopy in Astronomy **2.9) Explain how astronomers might use spectroscopy to determine the composition and temperature of a star.** #### Spectroscopy and Its Application in Astronomy Spectroscopy is a powerful analytical technique used by astronomers to gather information about the materials composing astronomical objects and their physical conditions, such as temperature. By analyzing the light emitted or absorbed by a star, researchers can deduce its properties as follows: 1. **Composition**: - **Emission and Absorption Lines**: When light from a star passes through a prism or a diffraction grating, it splits into its constituent colors, forming a spectrum. Spectra can show dark lines known as absorption lines or bright lines called emission lines at specific wavelengths. These lines correspond to the energies required for electrons to change energy levels in atoms and molecules. - **Chemical Fingerprint**: Each chemical element has a unique set of spectral lines, acting as a fingerprint. By identifying these lines, astronomers can determine the presence of specific elements within the star. 2. **Temperature**: - **Blackbody Radiation**: Stars emit light across a range of wavelengths, forming a continuous spectrum that approximates blackbody radiation. The peak wavelength of this spectrum shifts according to the temperature of the star (Wien's Law). - **Color Index**: The overall color of the star (blue or red) can give information about its temperature. Hotter stars emit more blue light, and cooler stars emit more red light. - **Line Broadening**: The width of spectral lines can also provide temperature information. Higher temperatures cause more thermal motion among atoms, broadening the spectral lines. By analyzing both the continuous spectrum for temperature and the discrete spectral lines for composition, astronomers can gather a comprehensive understanding of a star’s physical characteristics.

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