Detection and characterisation of two VLM binaries: LP 1033-31 and LP 877-72

TL;DR

This study used high-resolution near-infrared adaptive optics imaging to discover and characterize two new binary systems of M-dwarf stars, providing detailed properties and orbital estimates for each system.

Contribution

First high-resolution imaging characterization of two VLM binaries, including discovery of a new binary companion and detailed stellar and orbital parameters.

Findings

LP 1033-31 AB has a separation of 6.7 AU with similar-mass components.

LP 877-72 AB has a separation of 45.8 AU with primary twice as massive as secondary.

Both systems are dynamically stable with binding energies >10^43 erg.

Abstract

Using the high-resolution near-infrared adaptive optics imaging from the NaCo instrument at the Very Large Telescope, we report the discovery of a new binary companion to the M-dwarf LP 1033-31 and also confirm the binarity of LP 877-72. We have characterised both the stellar systems and estimated the properties of their individual components. We have found that LP 1033-31 AB with the spectral type of M4.5+M4.5 has a projected separation of 6.7$\pm$1.3 AU. Whereas with the spectral type of M1+M4, the projected separation of LP 877-72 AB is estimated to be 45.8$\pm$0.3 AU. The binary companions of LP 1033-31 AB are found to have similar masses, radii, effective temperatures, and log $g$ with the estimated values of 0.20$\pm$0.04 $\rm{M}_{\odot}$, 0.22$\pm$0.03 $\rm{R}_{\odot}$, 3200 K, 5.06$\pm$0.04. However, the primary of LP 877-72 AB is found to be twice as massive as the secondary with the derived mass of 0.520$\pm$0.006 $\rm{M}_{\odot}$. The radius and log $g$ for the primary of LP 877-72 AB are found to be 1.8 and 0.95 times that of the secondary component with the estimated values of 0.492$\pm$0.011 $\rm{R}_{\odot}$ and 4.768$\pm$0.005, respectively. With an effective temperature of 3750$\pm$15 K, the primary of LP 877-72 AB is also estimated to be $\sim$400 K hotter than the secondary component. We have also estimated the orbital period of LP 1033-31 and LP 877-72 to be $\sim$28 and $\sim$349 yr, respectively. The binding energies for both systems are found to be $\gt$10$^{43}$ erg, which signifies both systems are stable.