Sion Edward M, Godon Patrick, Bisol Alexandra
Astrophysics & Planetary Science, Villanova University, 800 Lancaster Avenue, Villanova, PA 19085, USA.
Astron J. 2015 Jul;150(No 1). doi: 10.1088/0004-6256/150/1/36. Epub 2015 Jul 7.
We present the results of a synthetic spectral analysis of the far ultraviolet archival IUE, HST and FUSE observations of the fast old nova V603 Aql, obtained some 90 years after its 1918 nova outburst. Our analysis utilizes the new Hubble FGS parallax distance for this nearly face-on old nova, a high white dwarf mass and a low reddening. Our analysis includes non-truncated optically thick accretion disks since V603 Aql is neither a polar nor an intermediate polar. Our synthetic spectral modeling of the FUSE and HST spectra analyzed separately indicate a mass transfer rate [Formula: see text] for the FUSE and HST spectra respectively, assuming a WD mass of 1.2. The mass accretion rate also depends on the assumed WD mass, and increases by a factor of two for a WD mass of 0.8. Combining the FUSE and HST spectra together lead to the same results. Potential implications are discussed.
我们展示了对快速老新星V603天鹰座在1918年新星爆发约90年后获取的远紫外存档国际紫外探测器（IUE）、哈勃太空望远镜（HST）和远紫外光谱探测器（FUSE）观测数据进行的合成光谱分析结果。我们的分析利用了这颗几乎正面朝向我们的老新星的哈勃精细制导传感器（FGS）新视差距离、高白矮星质量和低红化程度。由于V603天鹰座既不是极型新星也不是中间极型新星，我们的分析包括非截断的光学厚吸积盘。我们分别对FUSE和HST光谱进行的合成光谱建模表明，假设白矮星质量为1.2时，FUSE和HST光谱的质量转移率分别为[公式：见原文]。质量吸积率也取决于假设的白矮星质量，对于白矮星质量为0.8时，吸积率会增加两倍。将FUSE和HST光谱结合在一起得到相同的结果。我们还讨论了潜在的影响。
