Stellar Parameters for Pulsating B-star Candidates in the Kepler Field

The field of asteroseismology has enjoyed a large swath of data coming from recent missions (e.g., CoRoT, Kepler, K2). This wealth of new data has allowed the field to expand beyond the previous limitation of a few extremely bright and evolved stars. Asteroseismology relies on accurate surface measu...

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Bibliographic Details
Published in:The Astronomical journal 2019-03, Vol.157 (3), p.129
Main Authors: Hanes, Richard J., Waskie, Steven, Labadie-Bartz, Jonathan M., Wall, Audrey, Boyer, Amber, McSwain, M. Virginia
Format: Article
Language:English
Subjects:
Astronomy
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BOUNDARY CONDITIONS
ENERGY SPECTRA
GRAVITATION
Hot stars
LUMINOSITY
MAIN SEQUENCE STARS
MASS
OSCILLATIONS
Parameters
PHOTOMETRY
Physical properties
Rotation
Rotational spectra
stars: fundamental parameters
stars: massive
stars: oscillations
STELLAR ATMOSPHERES
Stellar evolution
Stellar seismology
SURFACES
VELOCITY
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Summary:The field of asteroseismology has enjoyed a large swath of data coming from recent missions (e.g., CoRoT, Kepler, K2). This wealth of new data has allowed the field to expand beyond the previous limitation of a few extremely bright and evolved stars. Asteroseismology relies on accurate surface measurements for boundary conditions, but the predicted physical parameters in the Kepler Input Catalog (KIC) are unreliable for hot stars. We present stellar parameters of 25 candidate pulsating B-star candidates in the Kepler field. We use blue optical spectra to measure the projected rotational velocity ( ), effective temperature (Teff), and surface gravity ( ) using TLUSTY and Kurucz ATLAS9 model atmospheres. We find a large discrepancy between our spectroscopically derived parameters and those derived from photometry in the KIC and Gaia Data Release 2 (DR2). Using spectral energy distributions, we also measure the radii of these stars and later calculate the luminosities and masses. We find the extinctions (AV) of these stars to be consistent with zero, which is expected for stars of high Galactic latitude.
ISSN:0004-6256
1538-3881
1538-3881
DOI:10.3847/1538-3881/ab064e