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Chapter 37, Problem 14P
To determine

The appropriate telescope to have better resolved image.

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H5. A star with mass 1.05 M has a luminosity of 4.49 × 1026 W and effective temperature of 5700 K. It dims to 4.42 × 1026 W every 1.39 Earth days due to a transiting exoplanet. The duration of the transit reveals that the exoplanet orbits at a distance of 0.0617 AU. Based on this information, calculate the radius of the planet (expressed in Jupiter radii) and the minimum inclination of its orbit to our line of sight.   Follow up observations of the star in part reveal that a spectral feature with a rest wavelength of 656 nm is redshifted by 1.41×10−3 nm with the same period as the observed transit. Assuming a circular orbit what can be inferred about the planet’s mass (expressed in Jupiter masses)?
Sometime around 2022, astronomers at the European Southern Observatory hope to begin using the E-ELT(European Extremely Large Telescope), which is planned to have a primary mirror 42 m in diameter. Let us assume that the light it focuses has a wavelength of 550 nm. (1 light-year = 9.461×10^15 m) Note:  Jupiter's Diameter dj=1.43×10^8 m 1)What is the most distant Jupiter-sized planet the telescope could resolve, assuming it operates at the diffraction limit? (Express your answer to two significant figures.) 2)What is the most distant Jupiter-sized planet the telescope could resolve, assuming it operates at the diffraction limit? (Express your answer to two significant figures.) 3)The nearest known exoplanets (planets beyond the solar system) are around 20 light-years away. What would have to be the minimum diameter of an optical telescope to resolve a Jupiter-sized planet at that distance using light of wavelength 550 nm? (Express your answer to two significant figures.)
One way that astronomers detect planets outside of our solar system (called exoplanets) is commonly referred to as the radial velocity method. This relies on the __________ ___________ to cause shifts in the spectral lines of stars as the stars perform tiny orbits around the center of mass of the host star and its orbiting planets. Those tiny orbits cause the stars to periodically (and therefore predictably) move closer to and further away from our solar system. Luckily, this method only relies on the motion of the star; its physical distance from us does not impact the resulting shifts.

Chapter 37 Solutions

Bundle: Physics For Scientists And Engineers With Modern Physics, 10th + Webassign Printed Access Card For Serway/jewett's Physics For Scientists And Engineers, 10th, Multi-term

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