Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 456, Issue 1, Pages 633-640Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv2689
Keywords
binaries: eclipsing; stars: dwarf novae; stars: individual: CSS111003: 054558+022106; novae, cataclysmic variables; planetary nebulae: general
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Funding
- South African NRF
- University of Cape Town
- SALT [2012-1-RSA-009, 2014-2-SCI-060]
- VLT at the Paranal Observatory [088.D-0750(A)]
- STFC [ST/M001350/1, ST/M002012/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/M001350/1] Funding Source: researchfish
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We report on the discovery of an eclipsing dwarf nova (DN) inside the peculiar, bilobed nebula Te 11. Modelling of high-speed photometry of the eclipse finds the accreting white dwarf to have a mass 1.18 M-circle dot and temperature 13 kK. The donor spectral type of M2.5 results in a distance of 330 pc, colocated with Barnard's loop at the edge of the Orion-Eridanus superbubble. The perplexing morphology and observed bow shock of the slowly expanding nebula may be explained by strong interactions with the dense interstellar medium in this region. We match the DN to the historic nova of 483 CE in Orion and postulate that the nebula is the remnant of this eruption. This connection supports the millennia time-scale of the post-nova transition from high to low mass-transfer rates. Te 11 constitutes an important benchmark system for CV and nova studies as the only eclipsing binary out of just three DNe with nova shells.
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