A UNIVERSAL DECLINE LAW OF CLASSICAL NOVAE. IV. V838 HER (1991): A VERY MASSIVE WHITE DWARF

被引：24

作者：

Kato, Mariko ^{[1
]}

Hachisu, Izumi ^{[2
]}

Cassatella, Angelo ^{[3
,4
,5
]}

机构：

[1] Keio Univ, Dept Astron, Yokohama, Kanagawa 2238521, Japan

[2] Univ Tokyo, Coll Arts & Sci, Dept Earth Sci & Astron, Meguro Ku, Tokyo 1538902, Japan

[3] Ist Fis Spazio Interplanetario, INAF, I-00133 Rome, Italy

[4] Univ Complutense Madrid, Fac Fis, Dept Astrofis, E-28040 Madrid, Spain

[5] Univ Roma Tre, Dipartimento Fis E Amaldi, I-00146 Rome, Italy

来源：

ASTROPHYSICAL JOURNAL | 2009年 / 704卷 / 02期

基金：

日本学术振兴会;

关键词：

novae; cataclysmic variables; stars: individual (V838 Herculis); stars: mass loss; ultraviolet: stars; white dwarfs; OPTICALLY THICK WINDS; RAY LIGHT-CURVE; INFRARED OBSERVATIONS; RECURRENT NOVAE; LINE-PROFILES; IA SUPERNOVAE; CYGNI; 1978; SEI METHOD; EVOLUTION; MODEL;

D O I：

10.1088/0004-637X/704/2/1676

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a unified model of optical and ultraviolet (UV) light curves for one of the fastest classical novae, V838 Herculis (Nova Herculis 1991), and estimate its white dwarf (WD) mass. Based on an optically thick wind theory of nova outbursts, we model the optical light curves with free-free emission and the UV 1455 angstrom light curves with blackbody emission. Our models of 1.35 +/- 0.02 M(circle dot) WD simultaneously reproduce the optical and UV 1455 angstrom observations. The mass lost by the wind is Delta M(wind) similar to 2 x 10(-6) M(circle dot). We provide new determinations of the reddening, E(B - V) = 0.53 +/- 0.05, and of the distance, 2.7 +/- 0.5 kpc.

引用

页码：1676 / 1688

页数：13

共 65 条

[1]

ALCOCK G, 1991, 5222 IAU

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