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3D Modeling of Solar-Type Stars to Characterize Stellar JitterDetection of Earth-mass planets requires measurements of radial velocity with extreme precision. To capture the tiny disturbances caused by a planet's motion, it is necessary to understand and characterize the host star’s turbulent dynamics in order to apply proper filtering to the observational data. We take advantage of current computational and technological capabilities to develop 3D realistic models of the stellar subsurface convection and atmospheres and thereby estimate the photospheric jitter. We have identified an initial set of target stars, obtained initial conditions using the MESA code, and obtained initial 3D radiative models of the stellar
surfaces and atmospheres with a spatial resolution of 50km. We present initial 3D radiative hydrodynamic model results of the planet-hosting star HD209458.
Document ID
20210019211
Acquisition Source
Ames Research Center
Document Type
Poster
Authors
Irina N. Kitiashvili
(Bay Area Environmental Research Institute Petaluma, California, United States)
Alan A. Wray
(Ames Research Center Mountain View, California, United States)
Samuel Granovsky
(Universities Space Research Association Columbia, Maryland, United States)
Date Acquired
July 26, 2021
Subject Category
Aeronautics (General)
Meeting Information
Meeting: TESS Science Conference II
Location: Virtual
Country: US
Start Date: August 2, 2021
End Date: August 6, 2021
Sponsors: Massachusetts Institute of Technology
Funding Number(s)
WBS: 936723.02.01.10.87
CONTRACT_GRANT: NNA16BD14C
Distribution Limits
Public
Copyright
Portions of document may include copyright protected material.
Technical Review
NASA Peer Committee
Keywords
SMD
Heliophysics
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