V410 Puppis: A useful laboratory for early stellar evolution

TL;DR

This paper combines various observational data to derive detailed parameters of the multiple star system V410 Puppis, revealing its young age, stellar variability, and possible accretion features, thus establishing it as a valuable laboratory for studying early stellar evolution.

Contribution

The study provides the first comprehensive set of absolute parameters for V410 Puppis and identifies new stellar variability and accretion features, enhancing its role as a model for early stellar evolution.

Findings

Derived stellar masses, radii, and temperatures for V410 Pup Aab.

Discovered low-amplitude SPB variability in the system.

Indications of accretion structures and emission cores in the components.

Abstract

New spectrometric (HERCULES) and ground-based multi-colour photometric data on the multiple star V410 Puppis are combined with satellite photometry (HIPPARCOS and TESS), as well as historic astrometric observations. Absolute parameters for V410 Pup Aab are derived: $M_{Aa}$ = $3.15 \pm 0.10$, $M_{Ab}$ = $1.83 \pm 0.08$ (M$_{\odot}$); $R_{Aa}$ = $2.12 \pm 0.10$, $R_{Ab}$ = $1.52 \pm 0.08$ (R$_\odot$); $a$ = $6.57 \pm 0.04$ R$_\odot$; $T_{Aa}$ = $12500 \pm 1000$, $T_{Ab}$ = $9070 \pm 800$ (K), and photometric distance $350 \pm 10$ (pc). We report the discovery of a low-amplitude SPB variation in the light curve and also indications of an accretion structure around V410 Pup B as well as emission cores in V410 Pup C. We argue that V410 Pup is probably a young formation connected with the Vela 2 OB Association. The combined evidence allows an age in the range 7-25 Myr from comparisons with standard stellar evolution modelling.