Solar Features

Solar scientists want to measure the temperature inside the sun by sending in probes. Imagine that temperature increases by 1 million◦C for every 10,000 km below the surface. A probe that can handle a temperature of x million degrees costs x³ million dollars. a. How much would it cost to measure the temperature 10,000 km down? b. How much would it cost to measure the temperature 100,000 km down? c. How much would it cost to measure the temperature 200,000 km down?

57. Solar Power Collectors. This problem leads you through the calculation and discussion of how much solar power can in principle be collected by solar cells on Earth. a. Imagine a giant sphere with a radius of 1 AU surrounding the Sun. What is the surface area of this sphere, in square meters? (Hint: The formula for the surface area of a sphere is 4rr2.) b. Because this imaginary giant sphere surrounds the Sun, the Sun's entire luminosity of 3.8 × 1020 watts must pass through it. Calculate the power passing through each square meter of this imaginary sphere in watts per square meter. Explain why this number represents the maximum power per square meter that a solar collector in Earth orbit can collect. c. List several reasons why the average power per square meter collected by a solar collector on the ground will always be less than what you found in part b. d. Suppose you want to put a solar collector on your roof. If you want to optimize the amount of power you can collect, how…

a. Describe the concept of “sphere of influence” and how it is estimated. b. Calculate the SOI for the Moon relative to the Earth. c. Would a single lone star have a computed sphere of influence, as defined in this class, which could be calculated? If no, why not? If yes, how would you do it?

2. Plasma oscillations in the ionosphere. The plasma density in the lower ionosphere has been measured during satellite reentry to be about a) 10¹8 m-³ at 50 km altitude, b) 10¹7 m-³ at 70 km and c) 10¹4 m²³ at 85 km. Use the formula for the electron plasma frequency to compute its numerical value for each of these three altitudes, AND state (we'll address this quantitatively later, when we get to EM wave propagation in plasmas) why the ionosphere is a relevant consideration for radio communications both on earth and between earth and interplanetary spacecraft.

paste BIUvab x, x here. I'm referring to A.A. Sunspot Core Radiation Granules of Chromosphere Wind from the Sun's Convective Zone and Conduction Zone Explanation of the Name Hydrogen Consider what is missing from this image. English (United States) word count of 6,204,461

What is Tyndall Effect? Explain why is it important for us to learn about it?

If a species evolved in order to see white tissues of the body, which wavelength do they have receptors for? *   A.) Gamma   B.) Infrared   C.) Ultraviolet   D.) X-ray   If a species evolved in order to see bones and metals, which wavelength do they have receptors for? *   A.) Gamma   B.) Infrared   C.) Ultraviolet   D.) X-ray

Q26-A(i). Define solar constant. Explain a process which converts light energy into electricity.

Suppose YOUR body temperature averages 98.6 F. 1. How much radiant energy in Wm^-2 is emitted from YOUR body?  2. What is the total radiant energy in W that is emitted from YOUR body? 3. At what wavelength does YOUR body emit the largest amount of radiant energy?

The sunspot cycle affects   I. the latitude at which sunspots are visible at a given time.   II. the number of sunspots that are visible at a given time.   III. the rotation rate of the sun’s equator at a given time.   IV. the magnetic polarity of the sunspots at a given time.   a. I & II   b. I & IV   c. II & III   d. I, II & III   e. I, II, & IV

H.M 1-What wavelength (in nanometers) is the peak intensity of the light coming from a star whose surface temperature is 11,000 Kelvin? (Note: This is about twice the temperature of our Sun's surface.) 2-Determine the surface temperature of a star whose maximum intensity is at 400nm.

1.  The Sun radiates energy like a black body with temperature 5800 K.  Use the Stefan-Boltzmann Law to calculate the Sun's Luminosity (which is the Sun's Surface Area times the Flux radiated per unit surface area. Use the following parameters: Sun's Radius = R = 6.96 x 1010 cm         Stefan-Boltzmann Const = s = 5.67 x 10-5 ergs/cm2 K4 sSun's Temperature = T = 5800 K           Formula for Luminosity:   L  =  4pR2 sT 4  What is the Sun's Luminosity?   __________  ergs/s

1..what is corona phenomena? 2..what are the effects of corona? 3..what are the ways to raduce corona?

Why don’t we see hydrogen Balmer lines in the spectra of stars with temperatures of 3,200 K?   a. There is no hydrogen in stars this cool.   b. The stars are hot enough that most of the hydrogen is ionized and the atoms cannot absorb energy.   c. These stars are so cool that nearly all of the hydrogen atoms are in the ground state.   d. Stars of this temperature are too cool to produce an absorption spectrum.   e. Stars of this temperature are too hot to produce an absorption spectrum.

What does the Wien Displacement Law (also known as Wien's Law) tell us? a) There is an inverse relation between the temperature of a thermal emitter and the wavelength where the emission peaks. b) There is a proportional relation between the temperature of a thermal emitter and the wavelength where the emission peaks. c) None of the above.

Define Solar Energy? Identify key historical events surrounding solar energy in the form of a timeline, create several ethical questions to be answered, and determine the ethical lens through which they will view Solar energy?

How are neutrinos observed?   a. by using a large tank of cleaning fluid buried deep in beneath Earth’s surface   b. by using spectral observations   c. by using a radio receiver   d. by using a Schmidt-Cassegrain focus   e. by using a magneto-hydrodynamic detector

A bright blue star is moving away from Earth. Which of the choices best completes the following statement describing the spectrum of this star? A(n) spectrum that is relative to an unmoving star. O A. absorption; redshifted O B. emission; redshifted O C. continuous; blueshifted D. continuous; redshifted O E. absorption; blueshifted

62. Pressure of the Photosphere. The gas pressure of the photosphere changes substantially from its upper levels to its lower levels. Near the top of the photosphere, the temperature is about 4500 K and there are about 1.6 x 1016 gas particles per cubic centimeter. In the middle, the temperature is about 5800 K and there are about 1.0 x 10" gas particles per cubic centimeter. At the bottom of the photosphere, the temperature is about 7000 K and there are about 1.5 × 10" gas particles per cubic centimeter. Use the ideal gas law (Mathematical Insight 14.2) to compare the pressures of each of these layers; explain the reason for the trend that you find. How do these gas pressures compare with Earth's atmospheric pressure at sea level?

How can we know that the sun will “die” in about 5 billion years? Choose the correct answer. A. We can see the evolution and death in the spectra B. We can see the entire process as it plays out in a star C. We look at thousands of stars like the sun and can see them in all stages of development

Read each question carefully and choose the letter of the best answer. Use the following choices to answer questions 1-3. a. nebula nucleosynthesis b. supernova nucleosynthesis c. stellar nucleosynthesis d. big bang nucleosynthesis 1. Which process is probable to produce the heaviest element? 2. When are hydrogen and helium formed? 3. When are carbon and oxygen formed? 4. What elements will be produced when carbon undergoes fusion reactions? a. hydrogen and helium b. beryllium and hydrogen C. oxygen and neon d. xenon and gold 5. When does a massive star enter the stage of becoming a supernova? a. when the star has used up all its hydrogen fuel b. when the star has burned all its oxygen C. when the chromium fusion stop 6. Which of the following describes stellar nucleosynthesis? a. It is the formation of light elements such as hydrogen and helium. b. It is the process by which elements are produced in gas clouds. c. It is the formation of elements during a supernova explosion. d. It is…

Imagine there is a large star that produces 2.5 x 1030 Watts of power. If there is a planet orbiting this star from 500 million kms away, what would be the solar constant of that planet?   a. 7,900W/m2   b. 52,000 W/m2   c. 250,000 W/m2   d. 800,000 W/m2​​​​​​​

Based on what you learned about the source of stellar energy and how stars make energy, select all of the correct statements from the following list. 1. Many stars make energy with the proton-proton cycle. 2. The CNO cycle is more efficient than the proton-proton cycle. 3. The sun's energy comes from the CNO cycle.More massive stars make energy with the proton-proton cycle. 4. The leftover mass in both the proton-proton cycle and the CNO cycle is converted to energy. 5. A helium atom is more massive than four hydrogen atoms. 6. The CNO cycle requires a higher temperature than the proton-proton cycle.

1) What is thermal equilibrium? Is the Sun in thermal equilibrium? How do we know this? 2) In order to maintain thermal equilibrium, how much energy must the Sun generate every second?