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|Title:||Refining our knowledge of the white dwarf mass-radius relation with HST observations of Sirius-type binaries|
|Authors:||Barstow, M. A.|
Bond, H. E.
Burleigh, M. R.
Casewell, S. L.
Holberg, J. B.
|Presented at:||19th European Workshop on White Dwarfs, Proceedings of a conference held at the Université de Montréal, Montréal, Canada|
|Publisher:||Astronomical Society of the Pacific|
|Citation:||ASP Conference Series, 2015, 493, p. 307|
|Abstract:||The presence of a white dwarf in a resolved binary system, such as Sirius, provides an opportunity to combine dynamical information about the masses, from astrometry and spectroscopy, with a gravitational red-shift measurement and spectrophotometry of the white dwarf atmosphere to provide a test of theoretical mass-radius relations of unprecedented accuracy. We demonstrated this with the first Balmer line spectrum of Sirius B to be obtained free of contamination from the primary, with STIS on HST. However, we also found an unexplained discrepancy between the spectroscopic and gravitational red-shift mass determinations. With the recovery of STIS, we have been able to revisit our observations of Sirius B with an improved observation strategy designed to reduce systematic errors on the gravitational red-shift measurement. We provide a preliminary report on the refined precision of the Sirius B mass-radius measurements and the extension of this technique to a larger sample of white dwarfs in resolved binaries. Together these data can provide accurate mass and radius determinations capable of testing the theoretical mass-radius relation and distinguishing between possible structural models.|
|Rights:||Copyright © 2015, Astronomical Society of the Pacific. Deposited with reference to the publisher’s open access archiving policy.|
|Appears in Collections:||Conference Papers & Presentations, Dept. of Physics and Astronomy|
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|1505.03427v1.pdf||Post-review (final submitted author manuscript)||54.33 kB||Adobe PDF||View/Open|
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