Experimental study on the chirped structure of the white-light continuum generation by femtosecond laser spectroscopy

The chirped structure of the white-light continuum generation (WLCG) pulse produced by focusing 800nm laser pulse with a pulse duration of 150fs (FWHM: full-width-at-half-maximum) onto a 2.4 mm thick sapphire plate was investigated by the optical Kerr gate technique with normal hexane as the optical Kerr gate medium. The observed WLCG was positively chirped, the measured anti-Stokes spectrum of WLCG ranges from 449 to 580nm with a temporal span of 2.56ps. When using metal reflecting mirrors to eliminate the group velocity dispersion (GVD) effect, we found that a span of 1.3ps still remained, indicating that the chirped pulse cannot be accounted for simply by GVD of the pulse propagation in the dispersive media. Our results suggest that the light-induced refractive index change due to the third-order nonlinear optical effect leads to an additional positive group velocity dispersion, which contributes to an important portion of the observed temporal broadening of the chirped WLCG. In addition to using reflective optical elements instead of dispersive optical elements, an effective way of reducing the chirp is to minimize the optical path length of the WLCG medium.     

星际氧气分子的气相-尘埃模型研究

本文采用气相-尘埃模型Nautilus研究了星际氧气的演化过程,使用了两种典型初始丰度值下的恒温模型和变化物理条件下的加热模型进行模拟计算. 结果表明,在冷致密云的条件下,CO、O₂和H₂O达到峰值的时间依赖于氢核密度的多少,其随氢核密度的增大而减小. 在加热模型中,在温度升高后的10⁵年后,氧气的丰度值与观测结果符合较好. 在温度大于30 K后,氧气的稳态丰度值将不再随氢核密度而变化,且大于此温度可以阻止氧气大量的沉降到尘埃表面. 此外,无论在恒温模型还是在加热模型中,低氢核密度更有利于O₂的生成.     

光深对大质量恒星形成团块化学性质研究的影响

本文使用文献中的N₂H⁺(1-0)、H¹³CO⁺(1-0)、HCN(1-0)和HN¹³C(1-0)谱线数据研究大质量恒星形成团块的化学性质和演化,发现H¹³CO⁺和HN¹³C的丰度受H₂柱密度的影响. 由于从A阶段到B阶段这两个丰度的中值增加了近10倍,H¹³CO⁺和HN¹³C适合追踪大质量恒星形成团块的演化. 从A到B阶段四种分子丰度增长速度从高到低依次为H¹³CO⁺、HCN、HN¹³C、N₂H⁺. 结果表明进行光学薄分子谱线的高分辨率观测对于研究大质量恒星形成团块的化学演化是必要的.