当前位置: X-MOL 学术Astron. J. › 论文详情
Our official English website, www.x-mol.net, welcomes your feedback! (Note: you will need to create a separate account there.)
Far Ultraviolet Spectroscopy of Old Novae. II. RR Pic, V533 Her, and DI Lac
The Astronomical Journal ( IF 5.3 ) Pub Date : 2017-02-14 , DOI: 10.3847/1538-3881/153/3/109
Edward M Sion 1 , Patrick Godon 1 , Liam Jones 1
Affiliation  

The old novae V533 Her (Nova Her 1963), DI Lac (Nova Lac 1910), and RR Pic (Nova Pic 1891) are in (or near) their quiescent stage, following their nova explosions, and continue to accrete at a high rate in the aftermath of their explosions. They exhibit continua that are steeply rising into the FUV, as well as absorption lines and emission lines of uncertain origin. All three have Far Ultraviolet Spectroscopic Explorer (FUSE) spectra that offer not only higher spectral resolution but also wavelength coverage extending down to the Lyman Limit. For DI Lac, we have matched these FUSE spectra with existing archival International Ultraviolet Explorer spectral coverage to broaden the FUV wavelength coverage. We adopted the newly determined interstellar reddening corrections of Selvelli & Gilmozzi. The dereddened FUV spectra have been modeled with our grids of optically thick accretion disks and hot, NLTE white dwarf (WD) photospheres. The results of our modeling analysis indicate that the hot components in RR Pic and V533 Her are likely to be accretion disks with mass accretion rates of 10-8M⊙ yr-1 and 10-9M⊙ yr-1 respectively. However, the disk cannot produce the observed absorption lines. For the WD to be the source of the absorption lines in these two systems, it must be very hot, with a radius several times its expected size (because the WD in these systems is massive, it has a smaller radius). For DI Lac, we find the best fit to be a disk with Ṁ = 10-10M⊙ yr-1 with a 30,000 K WD.

中文翻译:

旧新星的远紫外光谱。二、RR Pic、V533 Her 和 DI Lac

老新星 V533 Her (Nova Her 1963)、DI Lac (Nova Lac 1910) 和 RR Pic (Nova Pic 1891) 处于(或接近)静止阶段,在它们的新星爆发之后,并继续高速增生在他们的爆炸之后。它们表现出急剧上升到 FUV 的连续谱,以及来源不明的吸收线和发射线。三者都具有远紫外光谱探索器 (FUSE) 光谱,不仅提供更高的光谱分辨率,而且波长覆盖范围延伸至莱曼极限。对于 DI Lac,我们将这些 FUSE 光谱与现有存档的 International Ultraviolet Explorer 光谱覆盖范围相匹配,以扩大 FUV 波长覆盖范围。我们采用了 Selvelli & Gilmozzi 新确定的星际变红修正。去除的 FUV 光谱是用我们的光学厚吸积盘和热的 NLTE 白矮星 (WD) 光球的网格建模的。建模分析结果表明,RR Pic和V533 Her中的热成分很可能是质量吸积速率分别为10-8M⊙ yr-1和10-9M⊙ yr-1的吸积盘。然而,圆盘不能产生观察到的吸收线。为了使WD成为这两个系统中吸收线的来源,它必须非常热,半径是其预期大小的几倍(因为这些系统中的WD很大,因此半径较小)。对于 DI Lac,我们发现最适合的是 Ṁ = 10-10M⊙ yr-1 且 30,000 K WD 的圆盘。建模分析结果表明,RR Pic和V533 Her中的热成分很可能是质量吸积速率分别为10-8M⊙ yr-1和10-9M⊙ yr-1的吸积盘。然而,圆盘不能产生观察到的吸收线。为了使WD成为这两个系统中吸收线的来源,它必须非常热,半径是其预期大小的几倍(因为这些系统中的WD很大,因此半径较小)。对于 DI Lac,我们发现最适合的是 Ṁ = 10-10M⊙ yr-1 且 30,000 K WD 的圆盘。建模分析结果表明,RR Pic和V533 Her中的热成分很可能是质量吸积速率分别为10-8M⊙ yr-1和10-9M⊙ yr-1的吸积盘。然而,圆盘不能产生观察到的吸收线。为了使WD成为这两个系统中吸收线的来源,它必须非常热,半径是其预期大小的几倍(因为这些系统中的WD很大,因此半径较小)。对于 DI Lac,我们发现最适合的是 Ṁ = 10-10M⊙ yr-1 且 30,000 K WD 的圆盘。半径是其预期大小的几倍(因为这些系统中的 WD 很大,所以半径较小)。对于 DI Lac,我们发现最适合的是 Ṁ = 10-10M⊙ yr-1 且 30,000 K WD 的圆盘。半径是其预期大小的几倍(因为这些系统中的 WD 很大,所以半径较小)。对于 DI Lac,我们发现最适合的是 Ṁ = 10-10M⊙ yr-1 且 30,000 K WD 的圆盘。
更新日期:2017-02-14
down
wechat
bug