How Do You Convert Arcseconds to Meters for Calculating Celestial Masses?

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In summary, the Homework Statement discusses an object close to the Galactic Centre which has certain properties. The mass of the object, the semi-major axis of its orbit, the inclination of the orbit, and the orbital period are all mentioned. Additionally, the eccentricity and pericentre separation of the orbit are also mentioned.
  • #1
tomeatworld
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Homework Statement


By mapping the star S2 close to Galactic Centre, the orbit is found to have a semi-major axis of 0.119 arcsec , an inclination of 46[itex]^{o}[/itex], an orbital period of 15.2 years, an eccentricity of 0.87 and a pericentre separation of 0.0155.
a) Estimate the mass of object at the centre of the Galaxy.
b) Place a limit on the density.

Edit: For a) told to assume distance to galactic centre is 8kpc.

Homework Equations



T[itex]^{2}[/itex] = [itex]\frac{4\pi^{2}}{GM} \alpha^{3}[/itex]

The Attempt at a Solution


The problem I have is using the semimajor axis in the calculation. It's given in arcsec but (I assume) it's needed in m. How do you convert? All attempts I made, using trig, gave me the wrong answer. Do I need to convert? How would I go about it?
 
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  • #2
Perhaps if you know the distance to the Galactic Center over which the specified angles are observed you could convert them to a distance.
 
  • #3
Just added an edit. We are told to assume the distance to galactic centre is 8kpc.

Ok. Very silly of me. Worked it out perfectly. Thanks for the push in the right direction!

I can't however work the second bit out. It's wanted in [itex]M_{SUN}[/itex] [itex]pc^{-3}[/itex] but I just don't know where to start.
 
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  • #4
tomeatworld said:
Just added an edit. We are told to assume the distance to galactic centre is 8kpc.

Ok. Very silly of me. Worked it out perfectly. Thanks for the push in the right direction!

I can't however work the second bit out. It's wanted in [itex]M_{SUN}[/itex] [itex]pc^{-3}[/itex] but I just don't know where to start.

Well, let's see. You've worked out a mass for the central object in part (a), and the orbit of the star would seem to describe certain limits to the area enclosed by that orbit...
 
  • #5
The 8kpc is for the Suns orbit. How can you use that for S2's orbit?
 
  • #6
tomeatworld said:
The 8kpc is for the Suns orbit. How can you use that for S2's orbit?

I thought you'd solved part (a)? What did you use for "a" in your period equation? What would be the pericentre separation?
 
  • #7
So using the pericentre (is that the right point?) you can get the closest approach to the black hole. Then assuming a sphere get the volume etc etc.

I used the semimajor axis in a).
 
  • #8
tomeatworld said:
So using the pericentre (is that the right point?) you can get the closest approach to the black hole. Then assuming a sphere get the volume etc etc.

I used the semimajor axis in a).

Yes, the pericentre separation is the distance of closest approach of the star to the galactic centre. And yes, this pericentre distance will give you a upper bound on the volume of whatever it is that's inside that distance.
 
  • #9
Ok, thanks! Sorts everything out I think!
 

FAQ: How Do You Convert Arcseconds to Meters for Calculating Celestial Masses?

How do you apply Kepler's 3rd Law?

Kepler's 3rd Law states that the square of a planet's orbital period is proportional to the cube of its semi-major axis. To apply this law, you must first determine the orbital period of the planet and the semi-major axis of its orbit. Then, you can use the formula T^2/a^3 = constant to calculate the constant, which is equal to the sum of the masses of the planet and the central body in solar masses. This constant can then be used to find the mass of the central body.

What is the significance of Kepler's 3rd Law?

Kepler's 3rd Law is significant because it provides a mathematical relationship between a planet's orbital period and its distance from the central body. This law allows scientists to accurately calculate the mass of the central body, which is crucial in understanding the dynamics of the solar system and the universe.

How is Kepler's 3rd Law related to Newton's Law of Universal Gravitation?

Kepler's 3rd Law and Newton's Law of Universal Gravitation are closely related. Kepler's law describes the relationship between a planet's orbital period and its distance from the central body, while Newton's law explains the force of gravity between two objects based on their masses and distance. Together, these laws provide a comprehensive understanding of the motion of objects in space.

Can Kepler's 3rd Law be applied to all planetary systems?

Yes, Kepler's 3rd Law can be applied to all planetary systems, as long as the objects in the system are orbiting a single central body and their masses are known. This law has been successfully applied to our own solar system as well as many other planetary systems in the universe.

How did Kepler discover his 3rd Law?

Johannes Kepler discovered his 3rd Law while studying the motion of the planets in our solar system. By analyzing the data collected by his mentor Tycho Brahe, Kepler noticed a pattern between a planet's orbital period and its distance from the sun. After many years of calculations and observations, he was able to formulate this law and provide a key insight into the motion of planets.

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