Near-Ultraviolet and Visible Spectroscopy of HAYABUSA Spacecraft Re-Entry

Abstract

HAYABUSA is the first spacecraft ever to land on and lift off from any celestial body other than the moon. The mission, which returned asteroid samples to the Earth while overcoming various technical hurdles, ended on 2010 June 13, with the planned atmospheric re-entry. In order to safely deliver the sample return capsule, the HAYABUSA spacecraft ended its 7-year journey in a brilliant ``artificial fireball'' over the Australian desert. Spectroscopic observation was carried out in the near-ultraviolet and visible wavelengths between 3000 Å and 7500 Å at 3–20 Å resolution. Approximately 100 atomic lines such as Fe i, Mg i, Na i, Al i, Cr I, Mn i, Ni i, Ti i, Li i, Zn i, O i, and N i were identified from the spacecraft. Exotic atoms such as Cu i, Mo i, Xe i and Hg i were also detected. A strong Li i line (6708 Å) at a height of $\sim\ $55 km originated from the onboard Li-Ion batteries. The FeO molecule bands at a height of $\sim\ $63 km were probably formed in the wake of the spacecraft. The effective excitation temperature as determined from the atomic lines varied from 4500 K to 6000 K. The observed number density of Fe i was about 10 times more abundant than Mg i after the spacecraft explosion. N$_{2}^{+}$ ($1^-$) bands from a shock layer and CN violet bands from the sample return capsule's ablating heat shield were dominant molecular bands in the near-ultraviolet region of 3000–4000 Å. OH($A$–$X$) band was likely to exist around 3092 Å. A strong shock layer from the HAYABUSA spacecraft was rapidly formed at heights between 93 km and 83 km, which was confirmed by detection of N$_{2}^{+}$ ($1^-$) bands with a vibration temperature of $\sim\ $13000 K. Gray-body temperature of the capsule at a height of $\sim\ $42 km was estimated to be $\sim\ $2437 K which is matched to a theoretical prediction. The final message of the HAYABUSA spacecraft and its sample return capsule are discussed through our spectroscopy.