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      Shocks and Ejecta Mass: Radio Observations of Nova V1723 Aql

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          Abstract

          The radio light curves of novae rise and fall over the course of months to years, allowing for detailed observations of the evolution of the nova shell. However, the main parameter determined by radio models of nova explosions - the mass of the ejecta - often seems to exceed theoretical expectations by an order of magnitude. With the recent technological improvements on the Karl G. Jansky Very Large Array (VLA), new observations can test the assumptions upon which ejecta mass estimates are based. Early observations of the classical nova V1723 Aql showed an unexpectedly rapid rise in radio flux density and a distinct bump in the radio light curve on the rise to radio maximum, which is inconsistent with the simple model of spherical ejecta expelled in a single discrete event. This initial bump appears to indicate the presence of shocked material in the outer region of the ejected shell, with the emission from the shocks fading over time. We explore possible origins for this emission and its relation to the mass loss history of the nova. The evolution of the radio spectrum also reveals the density profile, the mass of the ejected shell, and other properties of the ejecta. These observations comprise one of the most complete, longterm set of multi-wavelength radio observations for any classical nova to date.

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          Author and article information

          Journal
          2013-06-10
          2013-07-17
          Article
          1306.2265
          09033e97-7087-491d-a565-7dca556b4d76

          http://arxiv.org/licenses/nonexclusive-distrib/1.0/

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          6 pages, 3 figures, to appear in the proceedings of conference "Stella Novae: Future and Past Decades," P. A. Woudt & V. A. R. M. Ribeiro (eds), ASP Conference Series
          astro-ph.SR astro-ph.HE

          High energy astrophysical phenomena, Solar & Stellar astrophysics

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