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Defect and Contact Passivation for Perovskite Solar Cells

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Defect and Contact Passivation for Perovskite Solar Cells

by Erkan Aydin, Michaele De Bastiani, Stefaan De Wolf
Review Year: 2019 DOI: https://doi.org/10.1002/adma.201900428

Bibliography

Aydin, E., De Bastiani, M., De Wolf, S., Defect and Contact Passivation for Perovskite Solar Cells. Advanced Materials 2019, 1900428.

Extra Information

A comprehensive review on the passivation routes for perovskite solar cells toward the Shockley–Queisser limit.

Abstract

​Metal‐halide perovskites are rapidly emerging as an important class of photovoltaic absorbers that may enable high‐performance solar cells at affordable cost. Thanks to the appealing optoelectronic properties of these materials, tremendous progress has been reported in the last few years in terms of power conversion efficiencies (PCE) of perovskite solar cells (PSCs), now with record values in excess of 24%. Nevertheless, the crystalline lattice of perovskites often includes defects, such as interstitials, vacancies, and impurities; at the grain boundaries and surfaces, dangling bonds can also be present, which all contribute to nonradiative recombination of photo‐carriers. On device level, such recombination undesirably inflates the open‐circuit voltage deficit, acting thus as a significant roadblock toward the theoretical efficiency limit of 30%. Herein, the focus is on the origin of the various voltage‐limiting mechanisms in PSCs, and possible mitigation strategies are discussed. Contact passivation schemes and the effect of such methods on the reduction of hysteresis are described. Furthermore, several strategies that demonstrate how passivating contacts can increase the stability of PSCs are elucidated. Finally, the remaining key challenges in contact design are prioritized and an outlook on how passivating contacts will contribute to further the progress toward market readiness of high‐efficiency PSCs is presented.

Keywords

contacts hysteresis passivation Perovskite recombination solar cell stability
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