Lab8ExtrasolarPlanetsReport

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Sam Houston State University *

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1404

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Astronomy

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Oct 30, 2023

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Carissa Buckland PHYS 1404 14 Lab 8 Extrasolar Planets Lab 8: Extrasolar Planets The objective of Lab 8: Extrasolar Planets is to become familiarized with two prominent methods of extrasolar planet detection, the radial velocity method and the transit method, display technological proficiency by using Nebraska Astronomy Applet Project (NAAP) simulation programs for both detection methods, and observe, accurately record, and interpret empirical data collected from the simulation programs. The radial velocity method of extrasolar planetary detection is used to detect planets by measuring changes in the wavelength of a star’s light due to its velocity in response to a planet. Changes in wavelength are either blueshifted, indicating planetary movement towards Earth, or redshifted, indicating planetary movement away from Earth. The transit method of extrasolar planetary detection is when a planet passes directly in front of its parent star, blocking some of the star’s light, and resulting in a measurable decrease in the parent star’s brightness. Of the two methods, the transit method is the easiest, most direct method of detecting extrasolar planets and has resulted in the vast majority of extrasolar planet discoveries to date. Extrasolar Planets begins with launching NAAP’s Exoplanet Radial Velocity Simulator. The simulator displays a number of important data sets, including the radial velocity curve, star properties, planet properties, and system orientation. Within the radial velocity curve data set, the radial velocity in m/s, phase, system period, and noise in m/s can be found. Manual manipulations can be made to noise and number. Planet properties include a manually changeable mass in M jup , semimajor axis in AU, and eccentricity. Star properties include a manually adjustable mass in M sun . System orientation includes manually adjustable degrees of inclination and longitude. Initial observations of the radial velocity curve, amplitude, and orbital period for Preset A are made to give baseline data for the remainder of the lab experiment. Adjusting planet mass (M jup ), observations are made to changes that occur to the radial velocity curve. Returning to Preset A initial settings, adjustments are made to the star mass (M sun ), and changes to the radial velocity curve are noted. Again, after returning to Preset A initial settings, adjustments are made to the semimajor axis (AU), and observation of the resulting changes to the radial velocity curve is noted.

Carissa Buckland PHYS 1404 14 Lab 8 Extrasolar Planets Initial values of Preset A are reset, manipulation of the degree of inclination occurs, and changes to the radial velocity curve are noted. A second preset planet is loaded, Preset B, and data is observed and recorded. The degrees of longitude are manipulated, and the observed changes are recorded. More preset values are loaded, manipulated, observed, and data recorded. The final portion of the radial velocity method section includes manipulating planet mass (M jup ) and radius/semimajor axis (AU), recording the amplitude and period (days), determining the detectability of the planet, and rationalizing the detectability choice based on a too small amplitude or too large period. The second section of Extrasolar Planets starts with the launching of NAAP’s Exoplanet Transit Simulator. The simulator displays data similar to the Exoplanet Radial Velocity Simulator with the exception of a theoretical curve displaying the length of the planet’s eclipse, replacing the radial velocity curve and eclipse depth replacing the length of the orbital period, and the addition of a manually adjustable radius measurement (R jup ) found under planet properties. It should be noted that the orbital period is on the X-axis of the curve, and changes can be observed in that area. Preset A is loaded, and the planet radius (R jup ), semimajor axis (AU), star mass (M sun ), and inclination are all manipulated. Changes in observable data are used to determine how changes in these variables affect eclipse depth and duration. Preset B, an Earth-like planet, is loaded, and noise is adjusted. Changes in reported data are observed and used to answer questions regarding Earth-sized planets. In conclusion, Lab 8: Extrasolar Planets successfully utilizes NAAP’s simulation software to accurately depict how extrasolar planets are detected, observed, and measured. Extrasolar Planets allowed students to complete the lab with a higher degree of understanding for both methods of detection, the radial velocity method and the transit method, and the impacts that changes in variables will have on the ability for extrasolar planets to be observed.

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