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While doing a transit study, you find an exoplanet around a nearby Sun-like star. The time between transits in P = 45 days. During a transit, the time from first to second contact is t₂ - t1 = 20 minutes and the time from first to third contact is t3 - t₁ = 5 hours. The depth of the transit is F = 0.05 (and we don't know the distance to the star so we can only measure the flux variation and not the luminosity variation; if we knew the distance this would then translate in ). 8.1 Draw a lightcurve of the transit labeling t₁, t2 and t3 and indicating the % in flux variation recorded. 8.2 What is the radius of the planet (in meters)? 8.3 What is the semi-major axis of the planet's orbit (in AU)? NOTE: to answer the last items you need to recall what we have seen in Module 2 about orbits. You can assume the planet is orbiting in an elliptical orbit.

While doing a transit study, you find an exoplanet around a nearby Sun-like star. The time between transits in P = 45 days. During a transit, the time from first to second contact is t₂ - t1 = 20 minutes and the time from first to third contact is t3 - t₁ = 5 hours. The depth of the transit is F = 0.05 (and we don't know the distance to the star so we can only measure the flux variation and not the luminosity variation; if we knew the distance this would then translate in ). 8.1 Draw a lightcurve of the transit labeling t₁, t2 and t3 and indicating the % in flux variation recorded. 8.2 What is the radius of the planet (in meters)? 8.3 What is the semi-major axis of the planet's orbit (in AU)? NOTE: to answer the last items you need to recall what we have seen in Module 2 about orbits. You can assume the planet is orbiting in an elliptical orbit.

Applications and Investigations in Earth Science (9th Edition)
Applications and Investigations in Earth Science (9th Edition)
9th Edition
ISBN:9780134746241
Author:Edward J. Tarbuck, Frederick K. Lutgens, Dennis G. Tasa
Publisher:Edward J. Tarbuck, Frederick K. Lutgens, Dennis G. Tasa
Chapter1: The Study Of Minerals
Section: Chapter Questions
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While doing a transit study, you find an exoplanet around a nearby Sun-like star. The time between transits in \( \mathrm{P}=45 \) days. During a transit, the time from first to second contact is \( t_{2}-t_{1}=20 \) minutes and the time from first to third contact is \( t_{3}-t_{1}=5 \) hours. The depth of the transit is \( \frac{\delta F}{F}=0.05 \) (and we don't know the distance to the star so we can only measure the flux variation and not the luminosity variation; if we knew the distance this would then translate in \( \frac{\delta L}{L} \) ).
8.1 Draw a lightcurve of the transit labeling \( t_{1}, t_{2} \) and \( t_{3} \) and indicating the \( \% \) in flux variation recorded.
8.2 What is the radius of the planet (in meters)?
8.3 What is the semi-major axis of the planet's orbit (in \( \mathrm{AU} \) )?

While doing a transit study, you find an exoplanet around a nearby Sun-like star. The time between transits in P = 45 days. During a transit, the time from first to second contact is t₂ - t1 = 20 minutes and the time from first to third contact is t3 - t₁ = 5 hours. The depth of the transit is F = 0.05 (and we don't know the distance to the star so we can only measure the flux variation and not the luminosity variation; if we knew the distance this would then translate in ). 8.1 Draw a lightcurve of the transit labeling t₁, t2 and t3 and indicating the % in flux variation recorded. 8.2 What is the radius of the planet (in meters)? 8.3 What is the semi-major axis of the planet's orbit (in AU)? NOTE: to answer the last items you need to recall what we have seen in Module 2 about orbits. You can assume the planet is orbiting in an elliptical orbit.
Transcribed Image Text:While doing a transit study, you find an exoplanet around a nearby Sun-like star. The time between transits in P = 45 days. During a transit, the time from first to second contact is t₂ - t1 = 20 minutes and the time from first to third contact is t3 - t₁ = 5 hours. The depth of the transit is F = 0.05 (and we don't know the distance to the star so we can only measure the flux variation and not the luminosity variation; if we knew the distance this would then translate in ). 8.1 Draw a lightcurve of the transit labeling t₁, t2 and t3 and indicating the % in flux variation recorded. 8.2 What is the radius of the planet (in meters)? 8.3 What is the semi-major axis of the planet's orbit (in AU)? NOTE: to answer the last items you need to recall what we have seen in Module 2 about orbits. You can assume the planet is orbiting in an elliptical orbit.
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