The Sun has a luminosity of L = 3.846 x 1026 W, and a radius of Rs = 697,000 km. Working with L the inverse-square law for intensities, R² = , and the surface-intensity of the Sun as I R²¹ = TR how much power would a 12.0 m² solar panel collect on Earth as compared to that when used on a PJupiter ? Take the distance from the Sun to PEarth = 7.78 x 10⁹ m, and - in short, what is the ratio Galilean moon of Jupiter Earth as RE = 1.49 x 10⁹ m and from the Sun to a Galiena moon as RJ the power formula is P= I. A where I is the intensity of light at a given distance from the Sun, and A is the area of the solar panel.
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- The energy flux from the sun has a peak value of around 1500 W/m2, and solar cells are around 15% efficient. Estimate the area needed to satisfy US energy needs using solar cells, using the estimates that there are about 350 million people in the US and that we use an average of 90 kW/person. Also assume that there are about 6 hours of "peak" sunlight per day. Answer in square kilometers (do not put units in your answer, however).3Calculate minimum and maximum energies that can be associated with IR?
- B, n, and p denote magnetic field strength, particle number density, and pressure, respectively. γ is theadiabatic index. The integral is taken over the full length of a flux tube with a small cross section.In ideal MHD convection, these quantities are conserved.A) Pinpoint the detailed assumptions of “ideal MHD convection”;B) With the ideal MHD assumption, prove that V, N, and H are conserved.Gamma rays typically have frequencies above 10 exahertz (or 10^19 Hz). What is the corresponding wavelength in units of picometers (pm) of a gamma ray with a 3*10^19 H? (1pm-10^-12m) Accessibility: Good to go Q Search F6 F7 F8 8 F9 F10 F11 F12 PrtSc/dsinė A beam of electrons is shot towards a material X with a crystalline structure. A diffraction pattern is observed corresponding to a distance d=0.15 nm. between two adjacent Bragg planes. The electrons are each sent in with a kinetic energy of 51.900000000000006 eV. Part a) Find the de Broglie wavelength in nanometres of an electron incident on the material X.
- could you explain why we calculate dLrel (The angular momentum) of two mass elements not one? We calculate dLrel and than to find Lrel we integrate L from 0 to l/2. Why do that ? Couldnt we calculate dLrel of one mass element and than calculate L from 0 to l/2?find the temperature of the coolest star whose peak blackbody wavelength can be observed with the human eye (the exact range of visible light varies from publication to publication, so use 380nm to 750 nm).You are on an interstellar mission from the E arth to the 8.7 light-years distant star Sirius. Your spaceship can travel with 70% the spee d of light and has a cylindrical shape with a diameter of 6 m at the front surface and a le ngth of 25 m. You have to cross the interstel lar medium with an approximated density of 1 hydrogen atom/m3. (a) Calculate the time it takes your spaceshi p to reach Sirius. (b) Determine the mass of interstellar gas th at collides with your spaceship during the mi ssion.
- a.Calculate the mass loss rate of the Sun M˙ due to the solar wind flow. Assume averageproperties of the solar wind of number density 6 protons cm−3, and a flow speed of 450 kms−1. Express your answer in units of both kg per year, and solar masses per year. b.Suppose the solar wind flow is perfectly radial. Calculate the expected rate of change ofsolar rotation frequency dω/dt at the present time, based on conservation of angular momentum. Give your answer in units of rad s−1 y−1(i.e., radians per second per year) and alsoin terms of fractional change per year, i.e., 1/ωdω/dt .Use a current solar rotation period of P = 25.38 days to calculate the current angularfrequency of rotation ω. The moment of inertia of a uniform sphere is 2/5 MR2. You canassume that the radius of the Sun is approximately constant, and the change in its momentof inertia due to the solar wind is only due to the mass loss. c.By observing the rotation period of stars similar to the Sun, it is inferred that their…Two stars, both of which behave like ideal blackbodies, radiate the same total energy per second. The cooler one has a surface temperature T and 4.0 times the diameter of the hotter star. What is the temperature of the hotter star in terms of T? (Just write the result)The first unmanned probe called ”Albert Einstein’s cousin” will reach the stellar system of theAlfa Centauri (estimated radius 5x104km) in year 2145. The probe will enter stationary orbit ofradius R=3.0 x108 km. In order to power itself the probe will convert all of the radiation energyreceived from the star by its hemispherical antenna (radius=10m). It is estimated that whenoriented at a right angle with respect to the incoming radiation, the antenna will collect total powerof 3x105W. From this information find the λmax, wavelength for which the Alfa Centauri emitsmost of its energy