经典 nova V Persei 日食模型：吸积盘边缘的作用
摘要
本文提出了 V Persei 这颗日食经典 nova 的多色 (BVRI) 光曲线，并测量了系统中 12 组新的日食时刻。结合文献中以前的日食时刻，这些时刻给出该系统日食中时刻的修订公式为 HJD = 2,447,442.8260(1) + 0.107123474(3) E。日食轮廓被分析为一种参数拟合模型，假设存在四种光源：白矮星主星、主序次星、带皮的吸积盘以及质量传递流与盘边缘交汇处的明亮斑点。计算了一组覆盖广泛合理参数值范围的模型解矩阵。随后探索该矩阵以确定拟合参数的最优值及其相关误差。对于将吸积盘视为无皮结构的模型，最优拟合要求该盘具有平坦的温度轮廓。尽管采用截断内盘 (R_in >> R_wd) 的模型会导致温度轮廓更陡峭，但仅在具有显著盘皮的模型中才发现稳态模型的温度轮廓特征为 T(r) ∝ r^{-3/4}。将观测到的日食中部亮度和颜色与最佳拟合模型的光学特性进行比较，表明 V Persei 位于约 1 kpc 的距离处。
引用
@article{arxiv.astro-ph/0603010,
title = {Modeling Eclipses in the Classical Nova V Persei: The Role of the Accretion Disk Rim},
author = {A. W. Shafter and K. A. Misselt},
journal= {arXiv preprint arXiv:astro-ph/0603010},
year = {2008}
}
备注
Accepted for publication in The Astrophysical Journal. Thirty-nine pages, including 9 figures. V2 - updated to include additional references and related discussion to previous work overlooked in the original version, and to correct a typo in the ephemeris given in the abstract. V3 - Minor typos corrected. The paper is scheduled for the 20 June 2006 issue of the ApJ. V4 - An error in equation (9) has been corrected. The results presented in the paper were not affected, as all computations were made using the correct formulation of this equation