NOVA LIGHT CURVES FROM THE SOLAR MASS EJECTION IMAGER (SMEI). II. THE EXTENDED CATALOG

被引:15
|
作者
Hounsell, R. [1 ,2 ]
Darnley, M. J. [3 ]
Bode, M. F. [3 ]
Harman, D. J. [3 ]
Surina, F. [3 ,4 ]
Starrfield, S. [5 ]
Holdsworth, D. L. [6 ,7 ]
Bewsher, D. [7 ]
Hick, P. P. [8 ]
Jackson, B. V. [9 ]
Buffington, A. [9 ]
Clover, J. M. [9 ]
Shafter, A. W. [10 ]
机构
[1] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
[2] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA
[3] Liverpool John Moores Univ, Astrophys Res Inst, IC2 Liverpool Sci Pk, Liverpool L3 5RF, Merseyside, England
[4] Chiangrai Rajabhat Univ, Dept Sci & Technol, 80 Moo 9, Chiangrai 57100, Thailand
[5] Arizona State Univ, Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA
[6] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England
[7] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England
[8] CAIDA UCSD SDSC, 9500 Gilman Dr,Mail Stop 0505, La Jolla, CA 92093 USA
[9] Univ Calif San Diego, Ctr Astrophys & Space Sci, 9500 Gilman Dr 0424, La Jolla, CA 92093 USA
[10] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA
来源
ASTROPHYSICAL JOURNAL | 2016年 / 820卷 / 02期
基金
美国国家科学基金会;
关键词
novae; cataclysmic variables; space vehicles: instruments; techniques: photometric; REMARKABLE RECURRENT NOVA; 2010; ERUPTION; V2491; CYGNI; EVOLUTION; VULPECULAE; OUTBURSTS; SEARCH; RAY;
D O I
10.3847/0004-637X/820/2/104
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We present the results from observing nine Galactic novae in eruption with the Solar Mass Ejection Imager (SMEI) between 2004 and 2009. While many of these novae reached peak magnitudes that were either at or approaching the detection limits of SMEI, we were still able to produce light curves that in many cases contained more data at and around the initial rise, peak, and decline than those found in other variable star catalogs. For each nova, we obtained a peak time, maximum magnitude, and for several an estimate of the decline time (t(2)). Interestingly, although of lower quality than those found in Hounsell et al., two of the light curves may indicate the presence of a pre-maximum halt. In addition, the high cadence of the SMEI instrument has allowed the detection of low-amplitude variations in at least one of the nova light curves.
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页数:27
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