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Shara MM, Martin CD, Seibert M, et al. An ancient nova shell around the dwarf nova Z Camelopardalis. Nature. 2007;446(7132):159-62doi: 10.1038/nature05576.
Shara, M. M., Martin, C. D., Seibert, M., Rich, R. M., Salim, S., Reitzel, D., Schiminovich, D., Deliyannis, C. P., Sarrazine, A. R., Kulkarni, S. R., Ofek, E. O., Brosch, N., Lépine, S., Zurek, D., De Marco, O., & Jacoby, G. (2007). An ancient nova shell around the dwarf nova Z Camelopardalis. Nature, 446(7132), 159-62. https://doi.org/10.1038/nature05576
Shara, Michael M, et al. "An ancient nova shell around the dwarf nova Z Camelopardalis." Nature vol. 446,7132 (2007): 159-62. doi: https://doi.org/10.1038/nature05576
Shara MM, Martin CD, Seibert M, Rich RM, Salim S, Reitzel D, Schiminovich D, Deliyannis CP, Sarrazine AR, Kulkarni SR, Ofek EO, Brosch N, Lépine S, Zurek D, De Marco O, Jacoby G. An ancient nova shell around the dwarf nova Z Camelopardalis. Nature. 2007 Mar 08;446(7132):159-62. doi: 10.1038/nature05576. PMID: 17344847.
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Nature. 2007 Mar 08;446(7132):159-62. doi: 10.1038/nature05576.

An ancient nova shell around the dwarf nova Z Camelopardalis.

Nature

Michael M Shara, Christopher D Martin, Mark Seibert, R Michael Rich, Samir Salim, David Reitzel, David Schiminovich, Constantine P Deliyannis, Angela R Sarrazine, Shri R Kulkarni, Eran O Ofek, Noah Brosch, Sebastien Lépine, David Zurek, Orsola De Marco, George Jacoby

Affiliations

  1. Department of Astrophysics, American Museum of Natural History, 79th Street and Central Park West, New York, New York 10024-5192, USA. [email protected]

PMID: 17344847 DOI: 10.1038/nature05576

Abstract

Cataclysmic variables (classical novae and dwarf novae) are binary star systems in which a red dwarf transfers hydrogen-rich matter, by way of an accretion disk, to its white dwarf companion. In dwarf novae, an instability is believed to episodically dump much of the accretion disk onto the white dwarf. The liberation of gravitational potential energy then brightens these systems by up to 100-fold every few weeks or months. Thermonuclear-powered eruptions thousands of times more luminous occur in classical novae, accompanied by significant mass ejection and formation of clearly visible shells from the ejected material. Theory predicts that the white dwarfs in all dwarf novae must eventually accrete enough mass to undergo classical nova eruptions. Here we report a shell, an order of magnitude more extended than those detected around many classical novae, surrounding the prototypical dwarf nova Z Camelopardalis. The derived shell mass matches that of classical novae, and is inconsistent with the mass expected from a dwarf nova wind or a planetary nebula. The shell observationally links the prototypical dwarf nova Z Camelopardalis with an ancient nova eruption and the classical nova process.

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