UNIVERSE (LOOSELEAF):STARS+GALAXIES
6th Edition
ISBN: 9781319115043
Author: Freedman
Publisher: MAC HIGHER
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Chapter 20, Problem 31Q
To determine
The mass of a white dwarf which has a diameter of
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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)?
Analysis of the spectrum of a solar–mass star shows a periodic back-and-forth shift of its spectral lines with a period of 3 days. A spectral line centred at wavelength λ0 = 500 nm shows a shift ∆λ = ±2.5 × 10−4 nm. Estimate the mass of the unseen orbiting companion by assuming the angle of inclination i = 90◦, and express your answer in Jupiter masses.
1) There is a one earth mass planet orbiting an M5 star of 0.2 Mo and luminosity 1x10-2 Lo-
A) How close does the planet need to be to the star in order to receive the same amount of energy
as the Earth receives from the sun?
B) What is the orbital period of the planet at this distance?
C) What is the magnitude of the radial velocity perturbation of the star?
D) If the system is edge on to us, would we be likely to detect this planet using the radial
velocity method?
Chapter 20 Solutions
UNIVERSE (LOOSELEAF):STARS+GALAXIES
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