SOLARLAB

docx

School

Southwest University *

*We aren’t endorsed by this school

Course

110

Subject

Astronomy

Date

Jun 24, 2024

Type

docx

Pages

Uploaded by olivaselias20

Astronomy Solar Lab EPCC Purpose : Learn about the sun’s solar dynamics. The Solar Basics: Review these chapter links to learn more about our Sun: • Astronomy (Chapter 15) ; Astronomy (Chapter 16) Questions – Concisely answer within three (3) sentences: 1. Sketch the interior of the sun and describe what each layer does. S 2. Describe how the sun’s hydrostatic equilibrium works in the sun. The hydrostatic equilibrium of the Sun represents a finely tuned equilibrium wherein the gravitational force, drawing material inward towards the core, is offset by the outward pressure produced by nuclear fusion reactions within its core. This equilibrium plays a vital role in upholding the Sun's stable form and preventing its collapse due to gravitational forces. Understanding NASA’s SDO mission. NOTE: DO NOT LOOK DIRECTLY AT THE SUN. We will use NASA data to analyze the sun’s surface features and dynamics. Go to the website to access this data: https://sdo.gsfc.nasa.gov/mission/ Plot Analysis (Refer to figure 1 and 2): In the menu bar, go to data, The sun now, and select EVE link. Once you see a graph with data plotted on it, look for a Time and Date section and input a start date 60 days prior to the current date. Input the current date for the end date, and select submit. Once 1

Astronomy Solar Lab EPCC you get a new plot, save it as a PNG file. From this file, identify and highlight a day with the highest irradiance. Figure 2: Enter today's date and the date of 30 days prior (blue arrows), click “submit” (red Figure 1: Select "data', "EVE Data" highlighted in arrow), then save the data plot as a PNG file red, and access the irradiance data. (black arrow) Analyzing Solar Activity: Go back to the main SDO website. Then go to main menu → select data→The Sun Now. Of the array of images for today’s date, select the following and save them as a JPG file: 171 Å, 1600 Å, HMI Colorized Magnetogram, Intensitygram and HMI Dopplergram. Use the following link to learn what each data image describes about our Sun: https://www.nasa.gov/missions/sdo/sun-science-stamps-highlight-a-decade-of-sun watching- from-space/ I n-situ solar image An image will be taken during class/lab of the Sun, which will be used to study the surface dynamics occurring on the Sun. Remember DO NOT LOOK DIRECTLY AT THE SUN . 2

Astronomy Solar Lab EPCC I mage and data submission In the table below, place those images and the plot you gathered from class and the website. Image of Sun (class/lab) • 171 Å (X- Ray) • 1600 Å (UV) • HMI Colorized Magnetogram • Intensitygram • HMI Dopplergram PNG Data Plot Questions – Answer concisely within two (2) sentences. You may use your own sketches to help illustrate your answers : 3

Your preview ends here

Eager to read complete document? Join bartleby learn and gain access to the full version

Access to all documents
Unlimited textbook solutions
24/7 expert homework help

Astronomy Solar Lab EPCC 1. Define irradiance. I rradiance refers to the amount of electromagnetic radiation power per unit area that falls onto a surface, as per radiometry terminology. It's measured in watts per square meter (W/m2) or equivalently in milliwatts per square millimeter. 2. Define the electromagnetic spectrum. The electromagnetic spectrum encompasses all forms of electromagnetic radiation, arranged according to their wavelengths or frequencies. It ranges from short wavelengths, such as gamma rays and X-rays, to long wavelengths, such as radio waves. This spectrum includes visible light, which is the narrow range of electromagnetic radiation that the human eye can detect. 3. What features can you see in some of the images that you cannot see in your own image taken of the sun? Images of the sun taken with special tools can show details like solar flares and coronal loops that regular cameras can't capture. These features are usually hidden because the sun is too bright to see them directly. Telescopes with filters can pick out specific light wavelengths, helping scientists study different parts of the sun's atmosphere and its activities. 4. What feature on the sun may yield the high irradiance you identified? The sun's very hot surface, with temperatures around 5,500 degrees Celsius, is the main reason for the high irradiance we see on Earth. This heat causes the sun to emit a lot of electromagnetic radiation, affecting the irradiance we experience. 5. Are these features (if any) correspond to any features shown in the magnetogram, intensitygram and Dopplergram? Yes, features observed on the sun align with those depicted in magnetograms, intensity grams, and Dopplergrams. Magnetograms, for instance, illustrate sunspots, while intensity grams capture brightness fluctuations such as solar flares, and Dopplergrams indicate shifts indicating solar movements and oscillations. 6. How does viewing the sun in the UV and X-ray radiation help understand what’s going on in the sun? Studying the sun with UV and X-ray radiation helps scientists understand different parts of its activity. UV radiation shows details of the sun's outer layer, like the corona, which helps explain events like solar flares. X-ray observations reveal hotter areas, helping scientists study phenomena related to magnetic fields, such as solar flares and solar wind. Solar Processes: CNO and Proton-Proton chains 4

Astronomy Solar Lab EPCC Proton-Proton https://astronomy.swin.edu.au/cosmos/c/cno+cycle CNO Cycle http://burro.cwru.edu/academics/Astr221/StarPhys/ppchain.html Questions – Answer concisely within 3 sentences. 7. How many hydrogen atoms are needed to make a helium atom? 8. How does Carbon, Nitrogen and Oxygen form in the CNO cycle? Useful links https://spaceplace.nasa.gov/solar-activity/en/ http://www.pas.rochester.edu/~blackman/ast104/spectrum.html https://www.science.org/content/blog-post/finding-right-wavelength 5

SOLARLAB

Related Documents