Unique chemical composition of the very metal-poor star LAMOST J1645+4357

TL;DR

This paper analyzes the unique chemical composition of the very metal-poor star LAMOST J1645+4357, revealing peculiar abundance ratios and comparing them with supernova models to understand its origins.

Contribution

It provides the first detailed abundance analysis of LAMOST J1645+4357 and discusses its unusual chemical pattern in the context of supernova nucleosynthesis models.

Findings

Nitrogen and C+N are significantly enhanced.

Alpha-elements are over-abundant; Ti, Sc, Co, Zn are deficient.

Cr and Mn are enhanced; Sr and Ba are deficient.

Abstract

We report on the chemical composition of the very metal-poor ([Fe/H]=-2.9) star LAMOST J1645+4357 that is identified to be a red giant having peculiar abundance ratios by Li et al. (2022). The standard abundance analysis is carried out for this object and the well studied metal-poor star HD~122563 that has similar atmospheric parameters. LAMOST J1645+4357 has a remarkable abundance set, highlighted by these features: (1) Nitrogen is significantly enhanced ([N/Fe]=+1.4) and the total abundance of C and N is also very high ([(C+N)/Fe]=+0.9); (2) alpha-elements are over-abundant with respect to iron as generally found in very metal-poor stars; (3) Ti, Sc, Co and Zn are significantly deficient; (4) Cr and Mn are enhanced compared to most of very metal-poor stars; (5) Sr and Ba are deficient and the Sr/Ba ratio ([Sr/Ba]=-1.0) is significantly lower than the value expected for the r-process. The overall abundance pattern of this object from C to Zn is well reproduced by a faint supernova model assuming spherical explosion, except for the excess of Cr and Mn which requires enhancement of incomplete Si burning or small contributions of a type Ia supernova or a pair-instability supernova. There remains, however, a question why the abundance pattern of this star is so unique among very metal-poor stars.