Absorption pattern for Hydrogen 1.0 F Intensity 0.5 400 420 440 460 480 500 520 540 560 580 600 620 640 660 680 700 Absorption pattern for Helium 1.0 Intensity 0.5 400 420 440 460 480 500 520 540 560 580 600 620 640 660 680 700 Absorption pattern for Lithium L.O Intensity 0.5 400 420 440 460 480 500 520 540 560 580 600 620 640 660 680 700 Absorption pattern for Sodium 1.0 Intensity 0.5 0.0 - 400 420 440 460 480 500 520 540 560 580 600 620 640 660 680 700 Absorption pattern for Mercury 1.0 F Intensity 0.5 400 420 440 460 480 500 520 540 560 580 600 620 640 660 680 700 Wavelength (nm)Absorption pattern for Neon 1.0 WWW Intensity 0.5 0.0 400 420 440 460 480 500 520 540 560 580 600 620 640 660 680 700 Absorption pattern for Nitrogen 1.0 Intensity 0.5 400 420 440 460 480 500 520 540 560 580 600 620 640 660 680 700 Absorption pattern for Carbon 1.0 F Intensity 0.5 400 420 440 460 480 500 520 540 560 580 600 620 640 660 680 700 Absorption pattern for Oxygen 1.0 Intensity 0.5 400 420 440 460 480 500 520 540 560 580 600 620 640 660 680 700 Absorption pattern for Iron 1.0 4 Intensity 0.5 400 420 440 460 480 500 520 540 560 580 600 620 640 660 680 700 Wavelength (nm)Place both your assigned Figure 1 and Figure 2 from StudentSteilar Spectra in this section. Answer the questions below. Many of these questions require you to both draw on your Figures 1 and 2 as well as type out written answers and descriptions. Be clear in your drawings; be detailed in your written answers. Your Figure 1 displays the strengthtintensity of the electromagnetic spectrum at a variety of wavelengths for a random star. The shape of this spectrum {starting on the left. a steep rise to a peak intensity and then a shallower reduction of intensity trailing off to the right} is actually the characteristic shape of a spectrum of any dense object that has a temperature [a star. a planet. you. for example}. We call this a thermal spectrum, or often we call it a Blackbody spectrum. 1. [2 marks] Draw vertical lines in your Figure 1. clearly dividing the DU. 'v'isible. and Infrared portions of your star's spectrum. Clearly label them as well. In what portion of the electromagnetic spectrum is most of your star's light coming from? How have you come to this conclusion? 2. [2 marks] At what exact wavelength is your star producing the most light? Another way of asking this is: at what wavelength is the star's peak intensity\"? Draw and label on your Figure 1 the wavelength of peak intensity [maybe another vertical line to help you read the number?}. Describe what you did. and the answer you got. 3. [2 marks]Astar's temperature is directly related to the wavelength of its peak intensity via 1v'lfien's Law. Consult Example 5.3 from our textbook. Astronomy 2e. for a demonstration of how this simple calculation is done. then calculate the temperature of your star. Show your work. Summarize your answer. [Don't be scared. it's a very easy calculation :} ] 4. [2 marks] How many times hotterrcooler is your star compared to the Sun? [Hint: you can nd the Sun's temperature in our textbook]. Show your work. Explain what you did. 5. [2 marks] What spectral type is your star? [Don't worry. we haven't covered this yet. but it's easy to figure out. Consult Table 1?.2 of our textbook, Astronomy 2a.} Describe your star's spectral type using the information in the table. 6. [2 marks] Use Stellarium [https:ttstellarium-web.orgf} to nd four examples of other stars that are of the same spectral type as your star. Feel free to start your search with the stars given as examples in Table 1?.2. then nd a couple more. In Stellarium. to determine its star is a specic spectral type. click on it and look in the info box for the heading 'spectral type'; only concern yourself with the letter at the beginning. See next page for an example.