Modeling the Spectra of Dense Hydrogen Plasmas: Beyond Occupation Probability
Abstract
Accurately measuring the masses of white dwarf stars is crucial in many astrophysical contexts (e.g., asteroseismology and cosmochronology). These masses are most commonly determined by fitting a model atmosphere to an observed spectrum; this is known as the spectroscopic method. However, for cases in which more than one method may be employed, there are well known discrepancies between masses determined by the spectroscopic method and those determined by astrometric, dynamical, and/or gravitational-redshift methods. In an effort to resolve these discrepancies, we are developing a new model of hydrogen in a dense plasma that is a significant departure from previous models. Experiments at Sandia National Laboratories are currently underway to validate these new
models, and we have begun modifications to incorporate these models into stellar-atmosphere codes.- Publication:
-
20th European White Dwarf Workshop
- Pub Date:
- March 2017
- DOI:
- 10.48550/arXiv.1610.02342
- arXiv:
- arXiv:1610.02342
- Bibcode:
- 2017ASPC..509..143G
- Keywords:
-
- Astrophysics - Solar and Stellar Astrophysics;
- Physics - Atomic Physics
- E-Print:
- 6 pages, 4 figures, to appear in the Proceedings of The 20th European Workshop on White Dwarfs