Spectral Classes Worksheet-1.docx

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Apr 3, 2024

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Spectral Class Worksheet These lab activities have evolved over years of use in Clemson University’s Department of Physics and Astronomy general astronomy laboratory. Contributors include Tom Collins, Mark Leising, Neil Miller, Peter Milne, Grant Williams, Donna Mullenax, Jessica Crist, Keith Davis, Amber Porter, Lea Marcotulli, and David Connick. Please direct all questions, complaints, and corrections to David Connick (dconnic@clemson.edu) who is responsible for all errors and omissions. Worksheet Name _Andrew Birchler___________ III Example Stars Table 1. Stars Spectral Class Name Temperature (K) B-V Color Index (number) Absolute Magnitude (total) Distance (ly) O Nair al Saif 31,500 -0.21 -6.50 2300 B Phact 12,700 -0.10 -2.88 261 A Fomalhaut 8,730 0.14 1.61 25.1 F Tabit 6,520 0.47 3.51 26.3 G Kraz 5,050 0.89 -0.93 146 K Wazn 4,390 1.18 0.35 87.2 M Gacrux 3,490 1.52 -2.44 88.6 1) In which properties do you see a trend as you move down the spectral class? What is the trend? B-V color index increases and Temperature decreases Table 2. Spectral Class K or G Stars Luminosity Class Name Temperature (K) Absolute Magnitude (total) Distance (ly) I Rastaban 5,190 -2.75 380 II Kraz 5,050 -0.93 146 III Vindemiatrix 4,800 -0.22 110 IV Mu Herculis 5,560 3.61 27.1 V Rigil Kentaurus 5,790 4.17 4.36
2) Which property of the star determines its Luminosity Class. How is that property changing as you move from class I to class V? Absolute magnitude determines luminosity class. Absolute magnitude increases as you move from class I to class V IV Spectral Class Spectra 3) Calculate the wavelength extremes for the visible spectrum of hydrogen (n 1 = 2): Ask your instructor for help with this calculation. Longest wavelength: ___ 6578.95 ____ Line designation (n 2 )___ 3 ____ Shortest wavelength: ___ 4166.67 ____ Line designation (n 2 )___ 6 ____ V Spectral Class Ordering 4) Using the numerical designations of the absorption spectrum plots which is the simplest plot (least dips and fluctuations)? Plot 1 has the least dips and fluctuations 5) Which absorption spectrum plot is the most complex (most dips and fluctuations)? Plot 7 is the most complex 6) In which of the absorption spectrum plots are the hydrogen lines the strongest? Plot 7 7) Which of the absorption spectrum plots is from the highest temperature source? Plot 1 8) Which of the absorption spectrum plots is from the lowest temperature source? Plot 3 9) Focus on the dips in the absorption spectrum plots due only to Hydrogen. Using the numerical designations list the spectrum from strongest (deepest) hydrogen lines to weakest (shallowest) hydrogen lines. 7, 6, 5, 4, 3, 2, 1 10) Looking at the calcium emission lines, at what wavelengths do the K and H lines appear at in Angstroms? K is at 3940 and H is at 3990 11) In which absorption spectrum plots can you see (both dips about the same size) the K and H calcium dips? Plots 2, 3, 4, and 5 all have roughly the same saze K and H calcium dips.
When the spectra are ordered by the intensity of the hydrogen lines alone, other spectral lines do not seem to be appropriately ordered. In particular there is a discontinuity (abrupt change) in the intensity of the K and H lines of calcium between adjacent spectra. In fact, this hydrogen ordering is not the best way to organize the physical properties of the stars. Now list your spectra in a way so that there is a smooth transition between the appearances and disappearances of lines of all elements. List them with the spectral sequence designations (O, B, A, F, G, K, M). Make sure that these make sense given what you know about the spectral classes. Hint: consider the temperature and expected continuum spectra of these stellar types. O B A F G K M 1 6 7 5 4 2 3 Now using the Letter designation of the spectral classes answer the following questions. 12) Which is the simplest spectrum? O 13) Which is the most complex spectrum? A 14) Which is the spectrum of the coolest source? M 15) Which is the spectrum of the hottest source? O 16) Conclusion - The key stellar property that determines the spectrum, both continuum and absorption line is: _ Temperature _____________________________ 17) Hydrogen is by far the most abundant element in the atmospheres of virtually all "normal" stars. Explain how a star can have very strong lines of other low-abundance elements and only very weak lines of hydrogen. (Hint: Visible hydrogen absorption lines can occur only if the electron starts in the n = 2 orbit.) What basic condition in the star’s atmosphere (other than absence of hydrogen) could make this possible? The stars that have very weak lines of hydrogen are also those that are the highest temperature. These extreme temperatures means that hydrogen doesnt exist in its normal atomic state, the electrons are not starting in the n = 2 orbit. Therefore no absorption lines are created.
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