Study investigates chemical composition of metal-poor star HD 1936

Utilizing the Ankara College Kreiken Observatory (AUKR) in Turkey, astronomers have carried out high-resolution spectroscopic observations of a metal-poor star often known as HD 1936. Outcomes of the observations marketing campaign, published February 15 on the preprint server arXiv, shed extra mild on the chemical composition of this star.

Metallic-poor stars are uncommon objects as only some thousand stars with iron abundances [Fe/H] beneath -2.0 have been found thus far. Increasing the nonetheless quick checklist of metal-poor stars and learning these objects intimately is of excessive significance for astronomers, as such stars have the potential to enhance our information of chemical evolution of the universe.

HD 1936 (often known as HIP 1873) is a really vibrant metal-poor star of spectral kind G5, positioned some 1,000 mild years away, within the galactic halo. The star, assumed to be about 10 billion years outdated, is estimated to be at the very least 10 occasions bigger than the sun, whereas its mass is most certainly between 0.9 and three.0 solar lots. Some research have steered that the star has a substellar companion with a mass of round 18.35 Jupiter lots.

Though earlier observations decided the atmospheric parameters of HD 1936, an in depth chemical research of this star has not been carried out but. That’s the reason a group of Turkish astronomers led by Şeyma Çalışkan of the Ankara College, determined to research HD 1936 with the Whoppshel Spectrograph mounted on the AUKR’s 0.8-m Berahitdin Albayrak telescope.

“We current chemical abundances of the very vibrant metal-poor star HD 1936 primarily based on high-resolution and excessive SNR [signal-to-noise ratio] spectra from AUKR,” the researchers wrote.

The group managed to acquire the abundances of 29 atomic species for HD 1936. The metallicity of the star was decided to be at a stage of -1.74, which is usually in settlement with earlier estimates.

The observations discovered that HD 1936 will not be carbon-enhanced and showcases mild in addition to odd-Z aspect abundance ratios principally appropriate with these of metal-poor discipline stars. The sodium to iron abundance ratio seems to be sub-solar, whereas the aluminum to iron abundance ratio turned out to be super-solar.

In response to the paper, the preliminary lithium abundance for HD 1936 was measured to be roughly 1.01 dex. That is in line with what’s often noticed in decrease pink big department stars.

The decided abundance ratios of europium and barium steered little or no s-process contamination for the investigated star. This allowed the astronomers to categorise HD 1936 as a reasonably r-process-enhanced metal-poor star.

The obtained outcomes additionally recommend that HD 1936 could also be a second-generation star shaped in a multi-enriched setting. The measured abundance ratio of magnesium to carbon factors to the enrichment on account of multiple supernova.

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