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Gamma-rays and neutrons are the only sources of information on energetic ionspresent during solar flares and on properties of these ions when they interactin the solar atmosphere. The production of {\gamma}-rays and neutrons resultsfrom convolution of the nuclear cross-sections with the ion distributionfunctions in the atmosphere. The observed {\gamma}-ray and neutron fluxes thusprovide useful diagnostics for the properties of energetic ions, yieldingstrong constraints on acceleration mechanisms as well as properties of theinteraction sites. The problem of ion transport between the accelerating andinteraction sites must also be addressed to infer as much information aspossible on the properties of the primary ion accelerator. In the last coupleof decades, both theoretical and observational developments have led tosubstantial progress in understanding the origin of solar {\gamma}-rays andneutrons. This chapter reviews recent developments in the study of solar{\gamma}-rays and of solar neutrons at the time of the RHESSI era. Theunprecedented quality of the RHESSI data reveals {\gamma}-ray line shapes forthe first time and provides {\gamma}-ray images. Our previous understanding ofthe properties of energetic ions based on measurements from the former solarcycles is also summarized. The new results-obtained owing both to the gain inspectral resolution (both with RHESSI and with the non solar-dedicatedINTEGRAL/SPI instrument) and to the pioneering imaging technique in the{\gamma}-ray domain-are presented in the context of this previous knowledge.Still open questions are emphasized in the last section of the chapter andfuture perspectives on this field are briefly discussed.

Properties of Energetic Ions in the Solar Atmosphere from {\gamma} -Ray and Neutron Observations