Hβ and Hγ Absorption-line Profile Inconsistencies in Laboratory Experiments Performed at White Dwarf Photosphere Conditions

Schaeuble, M. -A.; Nagayama, T.; Bailey, J. E.; Gomez, T. A.; Montgomery, M. H.; Winget, D. E.

doi:10.3847/1538-4357/ab479d

Hβ and Hγ Absorption-line Profile Inconsistencies in Laboratory Experiments Performed at White Dwarf Photosphere Conditions

Journal Article · Fri Nov 01 00:00:00 EDT 2019 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/ab479d· OSTI ID:1574124

Schaeuble, M. -A. ^[1]; Nagayama, T. ^[2]; Bailey, J. E. ^[2]; Gomez, T. A. ^[2]; ^[3]; Winget, D. E. ^[3]

Sandia National Lab. (SNL-NM), Albuquerque, NM (United States); The Univ. of Texas at Austin, Austin, TX (United States). Astronomy Dept.; Sandia National Laboratories
Sandia National Lab. (SNL-NM), Albuquerque, NM (United States)
The Univ. of Texas at Austin, Austin, TX (United States). Dept. of Astronomy and McDonald Observatory

The spectroscopic method relies on hydrogen Balmer absorption lines to infer white dwarf (WD) masses. These masses depend on the choice of atmosphere model, hydrogen atomic line shape calculation, and which Balmer series members are included in the spectral fit. In addition to those variables, spectroscopic masses disagree with those derived using other methods. Here we present laboratory experiments aimed at investigating the main component of the spectroscopic method: hydrogen line shape calculations. These experiments use X-rays from Sandia National Laboratories’ Z-machine to create a uniform ~15 cm³ hydrogen plasma and a ~4 eV backlighter that enables recording high-quality absorption spectra. The large plasma, volumetric X-ray heating that fosters plasma uniformity, and the ability to collect absorption spectra at WD photosphere conditions are improvements over past laboratory experiments. Analysis of the experimental absorption spectra reveals that electron density (n_e) values derived from the Hγ line are ~34% ± 7.3% lower than from Hβ. Two potential systematic errors that may contribute to this difference were investigated. A detailed evaluation of self-emission and plasma gradients shows that these phenomena are unlikely to produce any measurable Hβ–Hγ n_e difference. WD masses inferred with the spectroscopic method are proportional to the photosphere density. Hence, the measured Hβ–Hγ n_e difference is qualitatively consistent with the trend that WD masses inferred from their Hβ line are higher than that resulting from the analysis of Hβ and Hγ. In conclusion, this evidence may suggest that current hydrogen line shape calculations are not sufficiently accurate to capture the intricacies of the Balmer series.

View Accepted Manuscript (DOE)

Research Organization:: The Univ. of Texas at Austin, Austin, TX (United States)

Sponsoring Organization:: USDOE National Nuclear Security Administration (NNSA)

Grant/Contract Number:: NA0003843

OSTI ID:: 1574124

Alternate ID(s):: OSTI ID: 1595035

Journal Information:: The Astrophysical Journal (Online), Journal Name: The Astrophysical Journal (Online) Journal Issue: 1 Vol. 885; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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