Problem on spacecraft
Assuming that ground stations are equally distributed on the Earth, how many ground stations are required to maintain constant contact with a spacecraft at 750 km altitude, and 72 degrees inclination?
Expert
Given:
θ (theta) = 72°, Perpendicular distance of spacecraft=750 km.
We know that, 1° = π/180 radian, Radius of earth=6400 km. So, 72°= (72*π)/180 radian, = 2*π/5Since,θ = Arc/Radius,
Therefore, Arc = θ*Radius, =2*π*750/5, = 300π
Circumference of earth = 2*π*Radius = 2*π*6400
No. of space station = Circumference of earth/2*Arc = (2*π*6400)/(2*300*π) = 21 space station (approx.)
Rydberg formula (Rydberg): The formula that explains all of the characteristics of hydrogen's spectrum, comprising the Balmer, Paschen, Lyman, Brackett, and Pfund sequence. For the transition between an electron in
Null experiment: The experiment which, after being performed, yields no outcome. The null experiments are just as significant as non-null experiments; when current theory predicts an observable result (or predicts there must be no observable result),
Faint, young sun paradox: The theories of stellar evolution point out that as stars mature on the main series, they grow gradually hotter and brighter; computations propose that at as regards the time of the formation of Earth, the Su
Second: s: The basic SI unit of time, stated as the period of time equivalent to the duration of 9 192 631 770 periods of the radiation analogous to the transition between the two hyperfine levels of the ground state of cesium-133 atom.
Metre: meter; m: The basic SI unit of length, stated as the length of the path traveled by light in vacuum throughout a period of 1/299 792 458 s.
What do you understand by the term Ambient Reflection? And also write down its characteristic?
Rydberg constant (Rydberg): The constant that governs the relationship of the spectral line features of an atom via the Rydberg formula. For hydrogen, it is around 1.097 x 107 m-1.
Wien's displacement law constant, b: It is the constant of Wien displacement law. This has the value of 2.897 756 x 10-3 m K.
Chandrasekhar limit (S. Chandrasekhar; 1930): A limit that mandates that no white dwarf (a collapsed, degenerate star) can be much massive than around 1.4 masses solar. Any of the degenerate mass more massive should inevitably collaps
Cosmological constant (Lambda): The constant mentioned to the Einstein field equation, proposed to admit the static cosmological solutions. At the time the present philosophical view was steady-state model of the space, where the Universe has been aro
18,76,764
1952432 Asked
3,689
Active Tutors
1450886
Questions Answered
Start Excelling in your courses, Ask an Expert and get answers for your homework and assignments!!