A Solar Spectrum Synthesis Method Based on Monochrome LED

2020 ◽  
Vol 57 (9) ◽  
pp. 093004
Author(s):  
王宏民 Wang Hongmin ◽  
唐帆 Tang Fan ◽  
薛萍 Xue Ping
Keyword(s):  
Synthesis Method ◽  
Solar Spectrum ◽  
Spectrum Synthesis

Impact of the convective mixing-length parameter α on stellar metallicity

2020 ◽  
Vol 635 ◽  
pp. A176 ◽  
Author(s):  
N. Song ◽  
S. Alexeeva ◽  
T. Sitnova ◽  
L. Wang ◽  
F. Grupp ◽  
...  
Keyword(s):  
Open Cluster ◽  
Synthesis Method ◽  
Stellar Atmospheres ◽  
High Signal ◽  
Mixing Length ◽  
Dwarf Stars ◽  
Giant Stars ◽  
Spectrum Synthesis ◽  
Mixing Length Theory ◽  
The Impact

Context. Mixing-length theory is used to treat stellar convection. As a simulation in one-dimensional stellar atmospheres models, the mixing-length parameter α is calibrated from the Sun and then applied to other stars. However, there is no strong evidence to suggest that α should be the same for stars of different evolutionary stages. Aims. We evaluate the impact of the α value on the metallicity of different types of stars and investigate the correlation between the metallicity discrepancy (Δ[Fe∕H]) and stellar parameters (Teff, log g). Methods. We selected ten well-studied field stars and one open cluster of nine members for which high-resolution and high signal-to-noise spectra are available. The model atmospheres were calculated with the code MAFAGS-OS. We derived iron abundances from Fe I and Fe II lines both under local thermodynamic equilibrium and non-LTE conditions using a spectrum synthesis method. After deriving [Fe/H] for each line, we calculated Δ[Fe∕H] with two different α values, fixed solar-calibrated α, and α obtained for each star individually. Finally, we investigated the correlation between Δ[Fe∕H] caused by revised α with stellar parameters. Results. For FGK dwarf stars, the Δ[Fe∕H] caused by the α correction is less than 0.02 dex, while for turn-off and giant stars, the Δ[Fe∕H] values are no more than 0.03 dex, which are lower than typical uncertainties in metallicity. For main-sequence stars, Δ[Fe∕H] versus Teff and Δ[Fe∕H] versus log g are well fit by linear relations.

Solar Spectrum Synthesis Based on LED Peak

2018 ◽  
Vol 39 (4) ◽  
pp. 555-561
Author(s):  
王凌云 WANG Ling-yun ◽  
王立辉 WANG Li-hui ◽  
苏拾 SU Shi ◽  
张健 ZHANG Jian ◽  
张国玉 ZHANG Guo-yu
Keyword(s):  
Solar Spectrum ◽  
Spectrum Synthesis

scholarly journals Synthetic Infrared Spectra

1994 ◽  
Vol 154 ◽  
pp. 523-531 ◽  
Author(s):  
Robert L. Kurucz
Keyword(s):  
Infrared Spectrum ◽  
Molecular Spectroscopy ◽  
Solar Spectrum ◽  
The Sun ◽  
Signal To Noise ◽  
Molecular Line ◽  
Central Intensity ◽  
Spectrum Synthesis ◽  
Considerable Work ◽  
Atomic And Molecular Spectroscopy

The Sun is the star we can observe with the highest spectral resolution and signal-to-noise. From studying the infrared spectrum we can learn about the Sun, about stars in general, and about atomic and molecular spectroscopy. We discuss the computer programs for spectrum synthesis, the infrared flux and central intensity atlases of the solar spectrum, and the atomic and molecular line data. Considerable work is still required to improve the observations and to improve the line data.

Application of spectrum synthesis method to depth profile analysis

1990 ◽  
Vol 50 (1) ◽  
pp. 53-60 ◽  
Author(s):  
Isao Kojima ◽  
Natsuo Fukumoto ◽  
Masayasu Kurahashi ◽  
Tetsuya Kameyama
Keyword(s):  
Depth Profile ◽  
Profile Analysis ◽  
Synthesis Method ◽  
Depth Profile Analysis ◽  
Spectrum Synthesis

Spectrum synthesis of sharp-line B, A and F stars

2005 ◽  
Vol 17 ◽  
pp. 345-348 ◽  
Author(s):  
J. Silaj ◽  
A. Townshend ◽  
F. Kupka ◽  
J. Landstreet ◽  
A. Sigut
Keyword(s):  
Sharp Line ◽  
Spectrum Synthesis ◽  
F Stars
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