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Paper: X-ray Observations of Shocked Nova Ejecta
Volume: 490, Stella Novae: Past and Future Decades
Page: 327
Authors: Mukai, K.; Nelson, T.; Chomiuk, L.; Mioduszewski, A.; Rupen, M. P.; Sokoloski, J. L.; Weston, J. H. S.; Bode, M. F.; Eyres, S. P. S.; O'Brien, T. J.
Abstract: We present X-ray observations of novae, obtained in conjunction with radio observations. The 1–10 keV X-rays are optically thin thermal emission from the ejecta shock-heated to >10 million degrees, while the radio emission is often dominated by Bremsstrahlung emission from ∼10,000 K gas, perhaps with additional contributions from shocks. The very presence of hard X-ray emission requires faster ejecta to catch up with a slower material ejected earlier. The X-ray temperatures allow us to estimate the velocity differential between the two systems. Non-ionization-equilibrium signatures, when present, allow us to constrain the density of the shocked plasma. The absorbing columns, usually observed to decrease as the ejecta expand, constrain the amount of the slower, earlier ejecta that still remain unshocked. Specifically, we will present our analysis of the Swift and Suzaku observations of T Pyx and Nova Mon 2012 and discuss implications.
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