dc.contributor.author |
Moharana, Satyajeet |
|
dc.contributor.author |
Hema, B. P |
|
dc.contributor.author |
Pandey, Gajendra |
|
dc.date.accessioned |
2024-11-21T04:34:50Z |
|
dc.date.available |
2024-11-21T04:34:50Z |
|
dc.date.issued |
2024-10-20 |
|
dc.identifier.citation |
The Astrophysical Journal, Vol. 974, No. 2, 312 |
en_US |
dc.identifier.issn |
1538-4357 |
|
dc.identifier.uri |
http://hdl.handle.net/2248/8583 |
|
dc.description |
Open Access |
en_US |
dc.description |
Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. |
|
dc.description.abstract |
Determining the He/H ratio in cool stars presents a fundamental astrophysical challenge. While this ratio is
established for hot O and B stars, its extrapolation to cool stars remains uncertain due to the absence of helium lines in their observed spectra. We address this knowledge gap by focusing on the Sun as a representative cool star. We conduct spectroscopic analyses of the observed solar photospheric lines by utilizing a combination of MgH molecular lines and neutral Mg atomic lines including yet another combination of CH and C2 molecular lines with neutral C atomic lines. Our spectroscopic analyses were further exploited by adopting solar model atmospheres constructed for distinct He/H ratios to determine the solar photospheric helium abundance. The helium abundance is determined by enforcing the fact that for an adopted model atmosphere with an appropriate He/H ratio, the derived Mg abundance from the neutral Mg atomic lines and that from the MgH molecular lines must be the same. The same holds for the C abundance derived from neutral C atomic lines and that from CH lines of the CH molecular band and C2 lines from the C2 Swan band. The estimated He/H ratio for the Sun is discussed based on the one-dimensional local thermodynamic equilibrium model atmosphere. The helium abundance (He/H = - + 0.091 0.014 0.019) obtained for the Sun serves as a critical reference point to characterize the He/H ratio of cool stars across the range in their effective temperature. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
American Astronomical Society |
en_US |
dc.relation.uri |
https://doi.org/10.3847/1538-4357/ad6ccf |
|
dc.rights |
© 2024. The Author(s) |
|
dc.subject |
Chemical abundances |
en_US |
dc.subject |
Solar photosphere |
en_US |
dc.subject |
Stellar spectral lines |
en_US |
dc.subject |
Stellar atmospheres |
en_US |
dc.subject |
Molecular data |
en_US |
dc.subject |
Atomic data |
en_US |
dc.title |
Helium Abundance of the Sun: A Spectroscopic Analysis |
en_US |
dc.type |
Article |
en_US |