i need help to create this program in matlab . both photos include all the infor
ID: 3602894 • Letter: I
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i need help to create this program in matlab . both photos include all the information we got
extra information needed for program on the first line of each m-file name %reeshad sewdass,60499
Can you predict the next solar eclipse? Equations to determine the eclipse path On August 21, 2017, millions of people gathered in a narrow band in the United States to witness a total eclipse of the sun. A solar eclipse cccurs when the moon's orbit coincides with the sun's orbit such that the moon casts a shadow on the earth. Persons within that shadow observe the moon completely eclipsing the sun. At any given time, the following equations can be used to determine the latitude () and longitude (A) of the center of the moon's shadow on the earth's surface. Once these coordinates are calculated for various time values, you can plot the path of the eclipse The path of a solar eclipse can be predicted in advance using the theory of Besselian Elements. The basic equations to predict the path of a solar eclipse are given below. You are required to implement these equations in MATLAB, determine the path of the solar eclipse of July 2, 2019, and plot it on a map NOTE: you are not required to study Besselian theory, only to implement the equations in MATLAB NOTE: In these equations, longitude is measured positively to the west from the prime meridian. Latitude is measured positively to the north from the equator Values Provided Plotting the Path The following table of Besselian elements is pravided by NASA. Once you obtain the coordinates of the eclipse path for various times, you can plot it on a world map by modifying the script below. Polynomial Besselian Elesents for: 2019 7ul 02 19:00 ee.e TOT (te) 12 % set coordinate arrays-modify accordingly Longitude-array·30:10: 200; Latitude_array- -30:5:55 1 e.5B6207', e.", 106401 -n·001187.0.00 OMi9B -0.000094 14.999507 load('topo.mat','topo,'topomapl): % load earth topography whos topo topomapi; Tan fi.8045984 Tan f2 9.0045755 At tiee t1 decinal hours), each Besselian element is-valuated by: % set background parameters contour(0:359, -89.90, topo, [O,0L 'E. 'Linewidth', 21 axis equal -x, y, d, 11, 12, or t-t1 . to decinal hours) and to where: 19,000 TDT setlgca, Color, [oo1]. 'XLim, O 3601. YLim, 1.90 901. 'XTick, 10:30:3601 YTIck. 1-90:15-90]12 rid; SOURCE hold on % wait for more plot commands plot(Longitude-array, Latitude-array, 'y','inev idth', 2); % enter plot command here hold off % no more plot commands to come after this line How to use the table: y rectangular coordinates of the moon with respect to the fundamental p ane measured as a fraction of the e quatorial ra dius Submission Instructions d right declination angle of the point on the celestial sphere towards which the axis of the moon's shadow is directed ephemeris hour angle of the point above Write a MATLAB program to determine the path of the eclipse. Write your program in such a way that when executed, ONLY the final plot is displayed. Ensure that your file is error free before submitting e 0.00669454, ellipticity of the earth due to lts non-spherical shape A reference time is iven which corresponds to t a 0. The values of x,y,d and at this time are given in the line corresponding to n-0. Values at other times can be obtained from the polynomial equation using the coefficients in the table. Angles are given in degrees, and time is Save your main file as "PRGA STUDENTID.m. If you use function files, then save them as "PRGA STUDENTID_F.m" or "PRGA STUDENTID F2.m e-g. if your student ID is 54321, then save the files as "PRGA 54321.m, "PRGA 54321 F.m "PRGA54 321F2.rn", etc. asured in hours. On the first line of each m-file, include your name and ID as a comment, Le. % John Doe, 5432Explanation / Answer
Eclipse maps have long been used to plot the predicted path of the moon’s shadow as it crosses the face of Earth. Friedrich Wilhelm Bessel and William Chauvenet, two prominent 19th century astronomers and mathematicians, developed the math still used to make eclipse maps — long before computers and the precise astronomical data gathered during the Space Age.
Traditionally, eclipse calculations assume that all observers are at sea level and that the moon is a smooth sphere that is perfectly symmetrical around its center of mass. The calculations do not take into account different elevations on Earth and the moon’s cratered, uneven surface.
The true shape of the umbra is more like an irregular polygon with slightly curved edges. Each edge corresponds to a single valley on the lunar limb, the last spot on the limb that lets sunlight through. As these edges pass over mountain ranges, they are scalloped by the peaks and valleys of the landscape. The moon’s umbra will cross the Cascades, Rockies and Appalachians during the 2017 eclipse.
“Solar and lunar eclipses provide an excellent opportunity to talk about the moon, since without the moon there would be no eclipses,” said Noah Petro, deputy project scientist for LRO. “Because we know the shape of the moon better than any other planetary body, thanks to LRO, we can now accurately predict the shape of the shadow as it falls on the face of the Earth. In this way, LRO data sheds new light on our predictions for the upcoming eclipse.”
The total solar eclipse on Monday, Aug. 21, 2017 will cross the continental United States beginning in Oregon and ending in South Carolina. The last time a total solar eclipse spanned the United States was in 1918, when the path of totality entered through the southwest corner of Washington and passed over Denver, Colorado, Jackson, Mississippi, and Orlando, Florida before exiting the country at the Atlantic coast of Florida.
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