Local effects in astrometric binary orbits: perspective transformation and light-travel time

TL;DR

This paper investigates how local perspective and light-travel time effects influence the accuracy of astrometric binary orbit measurements, proposing methods to improve orbital element determination with upcoming high-precision data.

Contribution

It introduces a comprehensive approach to incorporate local perspective and light-travel time effects into astrometric binary orbit analysis, enhancing the accuracy of derived orbital parameters.

Findings

Including LP and LTT effects improves orbital parameter accuracy.

Ignoring LP can underestimate component masses by 14%.

Degenerate LP solutions are reliable for larger measurement errors.

Abstract

In order to get astrometric parameters achieving the precision permitted by the the forthcoming generation of astrometri cmeasurements, it will be necessary to take into account effects that were neglected until the present time. Two effects concerning the orbital elements of binary stars are considered hereafter: the former is the local perspective (LP) effect, which is due to the variation of the distance and of the orientation of the orbital plane during the observation time span. The latter effect is the light--travel time (LTT), which is also related to the orientation of the orbital plane. Taking these effects into account would allow to find the ascending nodes of the orbits, and lead to orbital elements more accurate than when they are ignored. It is derived from simulations that, at a distance of 5 pc, and assuming velocities typical of Pop.I stars, the position of the right ascending node could be derived for a few simulated unresolved binaries when the astrometric measurements have errors around 1 microas. For the resolved brown dwarf binary 2MASS J07464256 +2000321, it appears that ignoring the LP effect would result in underestimating the masses of the components by 14 per cent of the errors as soon as the astrometric errors are around 20 microas for each measurement. However, a `degenerate LP solution', taking into account the variation of the semi-major axis when the distance is varying, should provide reliable masses when the measurement errors are larger than 1 or 2 microas. A few binaries in the Gaia program could deserve a degenerate LP solution, whereas a the complete LP+LTT solution could be justified for resolved binaries observed with SIM.