What is the Semimajor Axis and Greatest Distance of the Comet?

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SUMMARY

The discussion centers on calculating the semimajor axis and greatest distance of a comet observed in 545 A.D. and again in 1937, using Kepler's Third Law. The period of the comet is determined to be 1392 years, leading to a semimajor axis of approximately 2.69e11 meters. The error in the initial calculation was identified as using Earth's mass instead of the Sun's mass, which is crucial for accurate orbital calculations. The discussion also touches on the applicability of Kepler's Laws to both natural celestial bodies and man-made satellites.

PREREQUISITES
  • Understanding of Kepler's Third Law of planetary motion
  • Familiarity with gravitational constant (G = 6.67e-11)
  • Knowledge of the mass of celestial bodies, specifically the Sun (Me = 5.98e24)
  • Basic algebra for solving equations involving orbital mechanics
NEXT STEPS
  • Study the derivation and applications of Kepler's Third Law in detail
  • Learn about the gravitational influence of the Sun on cometary orbits
  • Explore the differences between natural celestial orbits and those of artificial satellites
  • Investigate the methods for calculating orbital parameters using observational data
USEFUL FOR

Astronomy students, astrophysicists, and anyone interested in celestial mechanics and orbital dynamics will benefit from this discussion.

Gold3nlily
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Homework Statement


Suppose that a comet that was seen in 545 A.D. by Chinese astronomers was spotted again in year 1937. Assume the time between observations is the period of the comet and take its eccentricity as 0.11. What are (a) the semimajor axis of the comet's orbit and (b) its greatest distance from the Sun?


Homework Equations


Kepler's Third Law
T2= [(4pi2)/(GM)]* a3
G = 6.67e-11
Me = 5.98e24

The Attempt at a Solution



part a:
T = 1937-545 = 1392 (365d*24h*3600s) = 4.38e10 sec
e = 0.11

T2= [(4pi2)/(GM)]* a3
solve for a
a = [T2*[(GM)/(4pi2)]](1/3)
a = [(4.38e10)2*[(6.67e-11*5.98e24)/(4pi2)]](1/3)
a= 2.69e11 m

Part b:
Ra = a + ea
solve for Ra with e and a... but I can't find the correct a in first part of question

Whats going on, where did I go wrong?
 
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You used the Earth's mass - you should be using the sun's mass.
 
phyzguy said:
You used the Earth's mass - you should be using the sun's mass.

:face palm:

Thanks so much.
 
In what way kepler's law affects the motion of the Earth when it goes round the sun.
wil kepler's law apply to man-made satellites also. If so why?
 
In what way kepler's law affects the motion of the Earth when it goes round the sun.
wil kepler's law apply to man-made satellites also. If so why?

Well, Kepler's Laws describe any light particle orbiting a very heavy body. So Earth's orbit about the sun follows Kepler's Laws, as do the orbits of satellites about Earth. Does that answer your question?
 
well ... thanks for your answer about the relation between kepler's law and satellites but could you be more specific, coz its a 30marks question and i need a kind of detailed explanation...
 
I won't write your essay for you. For general information on Kepler's Laws, see Wikipedia or your textbook. If you have any specific questions after doing some research, I'm all ears.
 
How would you obtain the index error of the sextant of the sun "by using its diameter on the arc and off the arc".
kindly give ans. appropriately, coz i know how to just obtain the index error of the sun by using a sextant.
 

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