The N/O ratio in early B-type main sequence stars as an indicator of their evolution

TL;DR

This study demonstrates that the N/O ratio in early B-type main sequence stars is a reliable indicator of stellar evolution, less affected by ionization issues, and remains relatively constant across various stellar parameters.

Contribution

It establishes N/O as a more dependable evolutionary indicator for early B-type stars compared to N/C and C/O ratios, considering ionization effects.

Findings

N/O ratio is insensitive to overionization effects.

Most early B-stars have [N/O] ≈ 0, indicating little variation during the main sequence.

High initial rotation velocities correlate with higher [N/O] values.

Abstract

It is shown that, in the case of early B-type main-sequence stars, of the three ratios N/C, C/O, and N/O which are regarded as indicators of stellar evolution, the ratio N/O is more reliable since it seems to be insensitive to overionization of the NII and OII ions. On the other hand, the N/C and C/O ratios, which include carbon, may contain systematic errors for stars with Teff > 18500 K because of neglected overionization of CII ions. The ratio N/O is studied in the atmospheres of 46 early main-sequence B stars. These values of N/O are examined as functions of the effective temperature, age, rotation speed, and mass of the stars. Most early B-stars in the main sequence are found to have [N / O] = 0 , which indicates that N/O varies little during the main sequence stage, and this result is independent of the basic parameters listed above. There are two explanations for the large number of stars with [N / O] = 0 : it is predicted theoretically that for an initial rotation velocity V0 < 100 km/s, N/O varies little toward the end of the main sequence stage ([N/O] < 0.2) and observations show that most early main-sequence B-stars do actually have low initial rotation velocities V0. The few early main-sequence B-stars with higher [N/O] = 0.4-0.8 correspond to models with rotation velocities V0 = 200-300 km/s. This conclusion is consistent with earlier data for stars with the same masses in a later stage of evolution: the AFG-supergiant and bright giant stage.