Influence of misalignments on performance of externally occulted solar coronagraphs. Application to PROBA-3/ASPIICS

TL;DR

This paper analyzes how satellite misalignments affect the performance of the PROBA-3/ASPIICS solar coronagraph, providing a numerical model and guidelines to optimize internal occulter size and alignment strategies for better observations.

Contribution

It extends a numerical diffraction model to non-symmetrical cases and offers a practical 'recipe' for designing and aligning the coronagraph to mitigate diffracted light.

Findings

The internal occulter with R=1.1RSun effectively compensates misalignments.

Apodizing the IO edge further suppresses diffracted light.

Tilt misalignment of the telescope is the most critical factor.

Abstract

ASPIICS is a novel externally occulted coronagraph that will be launched onboard the PROBA-3 mission of ESA. The external occulter (EO) will be placed on one satellite ~150 m ahead of the second satellite with an optical instrument. During part of each orbit, the satellites will fly in a precise formation, constituting a giant externally occulted coronagraph. Large distance between the EO and the primary objective will allow observations of the white-light solar corona starting already from ~1.1RSun. We analyze influence of shifts of the satellites and misalignments of optical elements on diffracted light. Based on the quantitative influence of misalignments on diffracted light, we will provide a "recipe" for choosing the size of the internal occulter (IO) to achieve a trade-off between the minimal height of observations and sustainability to possible misalignments. We implement a numerical model of the diffracted light and its propagation through the optical system, and compute intensities of diffracted light throughout the instrument. Our numerical model extends axi-symmetrical model of Rougeot et al. 2017 to non-symmetrical cases. The computations fully confirm main properties of the diffracted light obtained from semi-analytical consideration. Results: relative influences of various misalignments are significantly different. We show that: the IO with R=1.1RSun is large enough to compensate possible misalignments in ASPIICS, apodizing the edge of the IO leads to additional suppression of the diffracted light. Conclusions: the most important misalignment is the tilt of the telescope WRT the line connecting the center of the EO and the entrance aperture. Special care should be taken to co-align the EO and the coronagraph, i.e. co-aligning the diffraction fringe from the EO and the IO. We suggest that the best orientation strategy is to point the coronagraph to the center of the EO.