我們的行星系統，由星際間密集的分子雲(Dense molecular cloud)彼此重力相互的吸引後所形成。而星際間的密集分子雲主要是由氣體及微小晶粒(Sub-micrometer sized grain)所組成。在太空溫度如此低溫的狀態環境下氣體會附著於星際塵埃粒子的表面，形成星際冰晶。主要包含H2O、CO、CO2、CH3OH、CH4、OCN-及NH2COOH…等。這些冰晶在經過太陽風(Solar wind)的轟擊後，其演化的機制，是我們主要探討的地方。 本實驗室將模擬外太空環境，在低溫(24K)、超高真空(6 × 10-10 Torr)下，以15keV H3+離子轟擊含NH或OH鍵與水H2O相互混合之冰晶，藉由傅式紅外光譜儀(FTIR)掃瞄冰晶結冰與轟擊時的紅外光譜圖。 最後在進而分析在CO(2138 cm-1)、CO2(2341 cm-1)以及OCN-(2165 cm-1)三個位置上在含NH與OH鍵之化合物與水H2O相互混合不同比例下的生成影響。 Our planetary system is composed of the collapse of dense molecular cloud, and it is attracted each other by gravity. The collapse of dense molecular cloud are composed of gases and sub-micrometer sized grains. The main composition of the interstellar solid material include H2O、 CO、CO2、CH3OH、CH4、OCN-、and NH2COOH etc,. These interstellar ice after the energetic particle bombarded that are being come from the solar wind and how evolves its interstellar ice is the main place where we probe into. In our experiment is to utilize cryogenic technique(24 K) and ultra high vacuum(6×10-10) to simulate the environment of outer space, it use H3+ ion to bombard the ice that include NH or OH bond chemical compound and H2O mixed, and the energy as 15keV. It used FTIR to scan the frozen and infrared spectrum of the ice crystal. Finally, analyze the quantity of the CO(2138cm-1)、CO2(2341cm-1) and OCN-(2165cm-1) bond that produced, and analyze the influence of mixing and proportion of H2O with NH and OH bond.
