Laboratory Hydrogen-Beta Emission Spectroscopy for Analysis of Astrophysical White Dwarf Spectra
This work communicates a review on Balmer series hydrogen beta line measurements and applications for analysis of white dwarf stars. Laser-induced plasma investigations explore electron density and temperature ranges comparable to white dwarf star signatures such as Sirius B, the companion to the br...
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| Format: | Article |
| Language: | English |
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MDPI AG
2018-07-01
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| Series: | Atoms |
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| Online Access: | http://www.mdpi.com/2218-2004/6/3/36 |
| _version_ | 1818483742105141248 |
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| author | Christian G. Parigger Kyle A. Drake Christopher M. Helstern Ghaneshwar Gautam |
| author_facet | Christian G. Parigger Kyle A. Drake Christopher M. Helstern Ghaneshwar Gautam |
| author_sort | Christian G. Parigger |
| collection | DOAJ |
| description | This work communicates a review on Balmer series hydrogen beta line measurements and applications for analysis of white dwarf stars. Laser-induced plasma investigations explore electron density and temperature ranges comparable to white dwarf star signatures such as Sirius B, the companion to the brightest star observable from the earth. Spectral line shape characteristics of the hydrogen beta line include width, peak separation, and central dip-shift, thereby providing three indicators for electron density measurements. The hydrogen alpha line shows two primary line-profile parameters for electron density determination, namely, width and shift. Both Boltzmann plot and line-to-continuum ratios yield temperature. The line-shifts recorded with temporally- and spatially-resolved optical emission spectroscopy of hydrogen plasma in laboratory settings can be larger than gravitational redshifts that occur in absorption spectra from radiating white dwarfs. Published astrophysical spectra display significantly diminished Stark or pressure broadening contributions to red-shifted atomic lines. Gravitational redshifts allow one to assess the ratio of mass and radius of these stars, and, subsequently, the mass from cooling models. |
| first_indexed | 2024-12-10T15:45:58Z |
| format | Article |
| id | doaj.art-a54a46e9cc4549d6bb02104c1d8362ef |
| institution | Directory Open Access Journal |
| issn | 2218-2004 |
| language | English |
| last_indexed | 2024-12-10T15:45:58Z |
| publishDate | 2018-07-01 |
| publisher | MDPI AG |
| record_format | Article |
| series | Atoms |
| spelling | doaj.art-a54a46e9cc4549d6bb02104c1d8362ef2022-12-22T01:42:57ZengMDPI AGAtoms2218-20042018-07-01633610.3390/atoms6030036atoms6030036Laboratory Hydrogen-Beta Emission Spectroscopy for Analysis of Astrophysical White Dwarf SpectraChristian G. Parigger0Kyle A. Drake1Christopher M. Helstern2Ghaneshwar Gautam3Physics and Astronomy Department, University of Tennessee Space Institute, University of Tennessee, Center for Laser Applications, 411 B.H. Goethert Parkway, Tullahoma, TN 37388-9700, USAPhysics and Astronomy Department, University of Tennessee Space Institute, University of Tennessee, Center for Laser Applications, 411 B.H. Goethert Parkway, Tullahoma, TN 37388-9700, USAPhysics and Astronomy Department, University of Tennessee Space Institute, University of Tennessee, Center for Laser Applications, 411 B.H. Goethert Parkway, Tullahoma, TN 37388-9700, USAPhysics Department, Fort Peck Community College, 605 Indian Avenue, Poplar, MT 59255, USAThis work communicates a review on Balmer series hydrogen beta line measurements and applications for analysis of white dwarf stars. Laser-induced plasma investigations explore electron density and temperature ranges comparable to white dwarf star signatures such as Sirius B, the companion to the brightest star observable from the earth. Spectral line shape characteristics of the hydrogen beta line include width, peak separation, and central dip-shift, thereby providing three indicators for electron density measurements. The hydrogen alpha line shows two primary line-profile parameters for electron density determination, namely, width and shift. Both Boltzmann plot and line-to-continuum ratios yield temperature. The line-shifts recorded with temporally- and spatially-resolved optical emission spectroscopy of hydrogen plasma in laboratory settings can be larger than gravitational redshifts that occur in absorption spectra from radiating white dwarfs. Published astrophysical spectra display significantly diminished Stark or pressure broadening contributions to red-shifted atomic lines. Gravitational redshifts allow one to assess the ratio of mass and radius of these stars, and, subsequently, the mass from cooling models.http://www.mdpi.com/2218-2004/6/3/36white dwarfsburning in starsplasma diagnosticsatomic spectraplasma spectroscopylaser spectroscopylaser-induced breakdown spectroscopy |
| spellingShingle | Christian G. Parigger Kyle A. Drake Christopher M. Helstern Ghaneshwar Gautam Laboratory Hydrogen-Beta Emission Spectroscopy for Analysis of Astrophysical White Dwarf Spectra Atoms white dwarfs burning in stars plasma diagnostics atomic spectra plasma spectroscopy laser spectroscopy laser-induced breakdown spectroscopy |
| title | Laboratory Hydrogen-Beta Emission Spectroscopy for Analysis of Astrophysical White Dwarf Spectra |
| title_full | Laboratory Hydrogen-Beta Emission Spectroscopy for Analysis of Astrophysical White Dwarf Spectra |
| title_fullStr | Laboratory Hydrogen-Beta Emission Spectroscopy for Analysis of Astrophysical White Dwarf Spectra |
| title_full_unstemmed | Laboratory Hydrogen-Beta Emission Spectroscopy for Analysis of Astrophysical White Dwarf Spectra |
| title_short | Laboratory Hydrogen-Beta Emission Spectroscopy for Analysis of Astrophysical White Dwarf Spectra |
| title_sort | laboratory hydrogen beta emission spectroscopy for analysis of astrophysical white dwarf spectra |
| topic | white dwarfs burning in stars plasma diagnostics atomic spectra plasma spectroscopy laser spectroscopy laser-induced breakdown spectroscopy |
| url | http://www.mdpi.com/2218-2004/6/3/36 |
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