AI 中文总结
本研究利用tlusty合成光谱等数据，分析9颗新星的宁静态瞬时吸积率，发现多数系统吸积率高于光度积分结果，提出外盘加热机制以解释部分系统的光谱特征。
AI 中文摘要
基于存档光谱，我们利用tlusty生成的合成吸积盘光谱、盖亚（Gaia）视差推导的距离以及更新后的色余值，计算了新星在宁静态下的瞬时质量转移率。我们对9颗新星的研究基于紫外光谱和多条光学光谱，得出的质量吸积率高于通过紫外和光学光度简单积分得到的结果。HR Del在爆发20年后，其质量转移率为4×10⁻⁷M☉/年，很可能正在燃烧吸积的富氢物质；原本被认为是低质量转移系统的V842 Cen，其质量吸积率与HR Del相当，对于这两颗新星，增强的质量转移必须由反馈回路自我维持。RR Pic的质量吸积率约为3×10⁻⁸M☉/年，其光谱更符合外区被加热至12000K的吸积盘模型，这与来自外盘的氢和氦发射线，以及盘前缘的大发射区域相符；这种受热的吸积盘也能很好地拟合CP Lac和DI Lac的光谱，DI Lac的质量吸积率约为4.5×10⁻⁹M☉/年和9×10⁻⁹M☉/年。V1974 Cyg和V533 Her的质量吸积率约为3×10⁻⁹M☉/年，具有相当平坦的光谱；处于低吸积状态的V446 Her和BK Lyn拥有最低的质量吸积率，分别约为10⁻⁹M☉/年和约10⁻¹⁰M☉/年。质量吸积率约为10⁻⁷M☉/年的较高质量转移率系统符合标准吸积盘模型，其余系统则更适合外盘被加热至约12000K的模型。我们推测，来自受热白矮星（WD）、内盘的辐射，结合潮汐相互作用、亮斑以及盘边缘溢出的物质，可提升外盘的温度。
英文摘要
Based on archival spectra, we derive the quiescent instantaneous mass transfer rates in novae using synthetic disk spectra generated with tlusty, Gaia parallax-derived distances, and updated color excess values. Our results for nine novae, based on ultraviolet spectra and on a number of optical spectra, yield mass accretion rates that are higher than those derived from simple integration of the UV and optical luminosity. HR Del, 20 years after its eruption, has a mass transfer rate of $4\times 10^{-7}M_\odot$/yr, and is likely burning the accreting H-rich material. V842 Cen, thought to be a low mass transfer system, has a comparable mass accretion rate. For both novae, the enhanced mass transfer must be self-sustained by a feedback loop. RR Pic, with $\dot{M}\approx 3\times 10^{-8}M_\odot$/yr, is better fitted with an accretion disk where the outer region is heated up to 12,000 K, in agreement with H and He emission lines coming from the outer disk and a large emission region on the leading side of the disk. Such a heated disk also gives a good fit to the spectra of CP Lac, and DI Lac with $\dot{M}\sim4.5$ and $9\times 10^{-9}M_\odot$/yr. V1974 Cyg and V533 Her, with an accretion rate of $\sim 3\times 10^{-9}M_\odot$/yr, have a rather flat spectrum. V446 Her and BK Lyn, caught in a state of low accretion, have the lowest mass accretion rates with $\dot{M} \sim 10^{-9}$ and $\sim 10^{-10}M_\odot$/yr respectively. The higher mass transfer rate systems, with $\dot{M}\approx \sim 10^{-7}M_\odot$/yr, agree with the standard disk model; the remaining systems are better fitted when the outer disk is heated to $\sim 12,000$~K. We suggest that irradiation from the heated WD, inner disk, together with tidal interaction, the bright spot, and material overflowing the disk edge, can increase the temperature of the outer disk.
Comments20 pages, 25 figures
