Location
Toomey Hall, Room 199
Presentation Date
April 22, 2023, 8:30am-10:00am
Session
Session 5s
Description
The goal of this project is to determine masses and radii of hot subdwarf B stars in hopes of connecting these fundamental intrinsic properties to the evolutionary history of such stars. Subdwarf B stars burn helium in their core, serving as interesting physical laboratories, and the abundance of public data, including GAIA parallaxes and archival photometry, can be used to determine stellar characteristics. In this study, observed photometry is compared to synthetic photometry, calculated from a similar-stellaratmosphere model spectrum. This match determines the effective stellar temperature and radius. With an estimate of surface gravity, mass can be determined. Such determinations are a direct application of the Spectral Energy Distribution (SED) fitting method.
Meeting Name
32nd Annual Spring Meeting of the NASA-Mo Space Grant Consortium
Document Type
Presentation
Document Version
Final Version
File Type
text
Language(s)
English
Rights
© 2023 The Authors, all rights reserved.
Masses and Radii of Subdwarf B Stars - SED Fitting Method
Toomey Hall, Room 199
The goal of this project is to determine masses and radii of hot subdwarf B stars in hopes of connecting these fundamental intrinsic properties to the evolutionary history of such stars. Subdwarf B stars burn helium in their core, serving as interesting physical laboratories, and the abundance of public data, including GAIA parallaxes and archival photometry, can be used to determine stellar characteristics. In this study, observed photometry is compared to synthetic photometry, calculated from a similar-stellaratmosphere model spectrum. This match determines the effective stellar temperature and radius. With an estimate of surface gravity, mass can be determined. Such determinations are a direct application of the Spectral Energy Distribution (SED) fitting method.
