ON THE MASS OF NOVA DQ HERCULIS (1934)

被引：63

作者：

HORNE, K

WELSH, WF

WADE, RA

机构：

[1] PENN STATE UNIV,DEPT ASTRON & ASTROPHYS,DAVEY LAB 525,UNIV PK,PA 16802

[2] CALTECH,PALOMAR OBSERV,PASADENA,CA 91125

[3] UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85724

[4] OHIO STATE UNIV,DEPT ASTRON,COLUMBUS,OH 43210

来源：

ASTROPHYSICAL JOURNAL | 1993年 / 410卷 / 01期

关键词：

BINARIES; SPECTROSCOPIC; NOVAE; CATACLYSMIC VARIABLES; STARS; INDIVIDUAL (NOVA DQ HERCULIS);

D O I：

10.1086/172752

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Published estimates of the white dwarf mass in the moderately slow nova DQ Her range from 0.35 to 1.2 M.. We report new estimates of the stellar masses, M1 = 0.60 +/- 0.07 M. and M2 = 0.40 +/- 0.05 M., and other system parameters as given in Table 2. These estimates are based on time-resolved 1.6 angstrom resolution CCD spectroscopy of Na I lambdalambda8183, 8195 absorption from the secondary star of DQ Her. We measure a radial velocity curve with K(obs) = 232 +/- 5 km s-1 and rotational broadening V(rot) sin i = 115 +/- 18 km s-1. We correct K(obs) to K2 = 227 +/- 10 km s-1 to take account of irradiation effects. The new estimate of M1 is an important parameter for thermonuclear runaway models of the nova eruption that occurred in 1934.

引用

页码：357 / 364

页数：8

共 30 条

[1] ECLIPSE TIMINGS OF DQ-HERCULIS [J].