Photometric Monte Carlo Simulation of Wolf-Rayet Wind-Eclipsing Binaries
Faculty Mentor Name
Noel Richardson
Format Preference
Poster
Abstract
Wolf-Rayet (WR) stars are highly evolved, massive stars that have shed their hydrogen envelopes, now burning helium in their cores. They are remarkably compact and exhibit fast, dense stellar winds. Much like their less-evolved O star counterparts, WR stars are frequently found in binary systems, typically paired with massive O stars. In these binaries, determining the system' s inclination angle is key to accurately measuring stellar masses. Short-period WR systems present a unique opportunity: when the WR star passes in front of its companion, its hot, ionized wind scatters light from the O star. This scattering effect, which depends on the binary' s inclination, the density of free electrons (directly tied to the star's mass-loss rate), and the separation between the stars, can be modeled to yield independent measurements of both stellar masses and the WR star's mass-loss rate. This year, I am advancing a Markov Chain Monte Carlo fitting technique, using Python-based algorithm emcee, designed to analyze these light curves. By modeling a binary WR system, we can better understand the intricacies of the physics behind their high mass loss rates . Under the guidance of Dr. Richardson last summer, I achieved results that were consistent with previously modeled ground-based light curves. With further code enhancements, the routine will soon be capable of processing high precision measurements from the Transiting Exoplanet Survey Satellite (TESS), capturing subtle brightness variations in these systems. Ultimately, the project aims to provide a robust method for determining both the masses and mass-loss rates of WR stars.
*"Wind-Eclipsing" misspelled in the original title as "Wind-Eclipsinf"
Photometric Monte Carlo Simulation of Wolf-Rayet Wind-Eclipsing Binaries
Wolf-Rayet (WR) stars are highly evolved, massive stars that have shed their hydrogen envelopes, now burning helium in their cores. They are remarkably compact and exhibit fast, dense stellar winds. Much like their less-evolved O star counterparts, WR stars are frequently found in binary systems, typically paired with massive O stars. In these binaries, determining the system' s inclination angle is key to accurately measuring stellar masses. Short-period WR systems present a unique opportunity: when the WR star passes in front of its companion, its hot, ionized wind scatters light from the O star. This scattering effect, which depends on the binary' s inclination, the density of free electrons (directly tied to the star's mass-loss rate), and the separation between the stars, can be modeled to yield independent measurements of both stellar masses and the WR star's mass-loss rate. This year, I am advancing a Markov Chain Monte Carlo fitting technique, using Python-based algorithm emcee, designed to analyze these light curves. By modeling a binary WR system, we can better understand the intricacies of the physics behind their high mass loss rates . Under the guidance of Dr. Richardson last summer, I achieved results that were consistent with previously modeled ground-based light curves. With further code enhancements, the routine will soon be capable of processing high precision measurements from the Transiting Exoplanet Survey Satellite (TESS), capturing subtle brightness variations in these systems. Ultimately, the project aims to provide a robust method for determining both the masses and mass-loss rates of WR stars.
*"Wind-Eclipsing" misspelled in the original title as "Wind-Eclipsinf"