A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date

作者：Finzell Thomas; Chomiuk Laura; Metzger Brian D; Walter Frederick M; Linford Justin D; Mukai Koji; Nelson Thomas; Weston Jennifer H S; Zheng Yong; Sokoloski Jennifer L; Mioduszewski Amy; Rupen Michael P; Dong Subo; Starrfield Sumner; Cheung C C; Woodward Charles E; Taylor Gregory B; Bohlsen Terry; Buil Christian; Prieto Jose; Wagner R Mark; Ben**y Thomas; Bond I A; Sumi T; Bennett D P; Abe F; Koshimoto N; Suzuki D; Tristram P J

来源：Astrophysical Journal, 2018, 852(2): 108.

DOI：10.3847/1538-4357/aaa12a

• gamma rays: stars
• novae, cataclysmic variables
• radio continuum: stars
• stars: individual (V1324 Sco)

It has recently been discovered that some, if not all, classical novae emit GeV gamma-rays during outburst, but the mechanisms involved in the production ofgamma-rays are still not well understood. We present here a comprehensive multiwavelength data set-from radio to X-rays-for the most gamma-ray-luminous classical nova to date, V1324 Sco. Using this data set, we show that V1324 Sco is a canonical dusty Fe II-type nova, with a maximum ejecta velocity of 2600 km s(-1) and an ejecta mass of a few x 10(-5) M-circle dot. There is also evidence for complex shock interactions, including a double-peaked radio light curve which shows high brightness temperatures at early times. To explore why V1324. Sco was so gamma-ray luminous, we present a model of the nova ejecta featuring strong internal shocks and find that higher gamma-ray luminosities result from higher ejecta velocities and/or mass-loss rates. Comparison of V1324. Sco with other gamma-ray-detected novae does not show clear signatures of either, and we conclude that a larger sample of similarly well-observed novae is needed to understand the origin and variation of gamma-rays in novae.

• 出版日期2018-1-10