TY - JOUR
T1 - A Detailed Observational Analysis of V1324 Sco, the Most Gamma-Ray-luminous Classical Nova to Date
AU - Finzell, Thomas
AU - Chomiuk, Laura
AU - Metzger, Brian D.
AU - Walter, Frederick M.
AU - Linford, Justin D.
AU - Mukai, Koji
AU - Nelson, Thomas
AU - Weston, Jennifer H.S.
AU - Zheng, Yong
AU - Sokoloski, Jennifer L.
AU - Mioduszewski, Amy
AU - Rupen, Michael P.
AU - Dong, Subo
AU - Starrfield, Sumner
AU - Cheung, C. C.
AU - Woodward, Charles E.
AU - Taylor, Gregory B.
AU - Bohlsen, Terry
AU - Buil, Christian
AU - Prieto, Jose
AU - Wagner, R. Mark
AU - Bensby, Thomas
AU - Bond, I. A.
AU - Sumi, T.
AU - Bennett, D. P.
AU - Abe, F.
AU - Koshimoto, N.
AU - Suzuki, D.
AU - Tristram, P. J.
AU - Christie, Grant W.
AU - Natusch, Tim
AU - McCormick, Jennie
AU - Yee, Jennifer
AU - Gould, Andy
PY - 2018/1/10
Y1 - 2018/1/10
N2 - 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 × 10-5 M⊙. 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.
AB - 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 × 10-5 M⊙. 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.
KW - gamma rays: stars
KW - novae, cataclysmic variables
KW - radio continuum: stars
KW - stars: individual (V1324 Sco)
UR - https://doi.org/10.3847/1538-4357/abb6f1
U2 - 10.3847/1538-4357/aaa12a
DO - 10.3847/1538-4357/aaa12a
M3 - Article
AN - SCOPUS:85040659904
VL - 852
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 108
ER -