Using Kepler’s Third Law (r3 = MT2 where M is the mass of the central star) find the orbital radius in astronomical units of this planet. M = 1.5 times the mass of the sun. Remember to convert days to years using 365.25 as the length of a year in days. Key Points to know: - The semimajor axis of the planet in AU is r = 0.0379 AU - The circumference of the orbit is l = 3.562 x 10^10 m - The orbital velocity in m/s is v = 1.874 x 10^5 m/s Questions that need to be answered: - With that orbital velocity, the radius of the orbit in meters, find the centripetal acceleration of our exoplanet:
Using Kepler’s Third Law (r3 = MT2 where M is the mass of the central star) find the orbital radius in astronomical units of this planet. M = 1.5 times the mass of the sun. Remember to convert days to years using 365.25 as the length of a year in days.
Key Points to know:
- The semimajor axis of the planet in AU is r = 0.0379 AU
- The circumference of the orbit is l = 3.562 x 10^10 m
- The orbital velocity in m/s is v = 1.874 x 10^5 m/s
Questions that need to be answered:
- With that orbital velocity, the radius of the orbit in meters, find the centripetal acceleration of our exoplanet:
- Knowing the acceleration that our planet experiences, calculate the force that the host star exerts on the planet:
- Knowing the force on the planet, the orbital radius, and the mass of the parent star, use the equation for gravitational force to find the mass of our planet (m2). (To get m1 in kg multiply the mass of the star in solar masses by 1.98 x 1030).
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