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SUMMARY:Determining Stellar Inclinations and True Planet Mass with RVs
DTSTART;VALUE=DATE-TIME:20261028T170500Z
DTEND;VALUE=DATE-TIME:20261028T171500Z
DTSTAMP;VALUE=DATE-TIME:20261025T193347Z
UID:indico-contribution-3666@nyx.physics.mcgill.ca
DESCRIPTION:Speakers: Riley Rosener (Université de Montréal)\nI aim to d
 etermine the inclination of the rotation axis of stars that host exoplanet
 s and to use that information to find the true mass of their exoplanets. T
 o detect exoplanets via the radial velocity method\, one measures the minu
 te redshifts and blueshifts in a star’s spectrum as a star’s planet ca
 uses orbital reflex motion towards and away from the observer. The strengt
 h of the radial velocity signal depends on the planet’s mass and its a p
 riori unknown orbital inclination–the rotational plane tilt relative to 
 the observer. Without knowing the inclination\, the radial velocity techni
 que can only provide a lower limit on the planet mass–a limitation for t
 he past 30 years. If one can find the stellar rotation axis inclination an
 d assumes that the planet’s orbital inclination is perpendicular to the 
 stellar rotation axis\, one can find the planet’s true mass. My research
  investigates a new method of determining the stellar rotation axis from R
 V observations by analyzing and modeling the changes in both stellar radia
 l velocity and surface temperature shifts as a function of time. I use dat
 a from the NIR spectrographs NIRPS and SPIRou and reduce it via the line-b
 y-line technique (LBL) to measure both the stellar RV and temperature vari
 ations (dTemp)\, modeling the outputs with starry and fitting the stellar 
 rotation axis inclination with MCMC sampling\, from which a true planet ma
 ss can be found.\n\nhttps://nyx.physics.mcgill.ca/event/587/contributions/
 3666/
LOCATION:Online 
URL:https://nyx.physics.mcgill.ca/event/587/contributions/3666/
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