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Date: 2015
Language: eng
Resource Type: journal article
Identifier: http://hdl.handle.net/1959.14/362826
Description: There is no conclusive explanation of why ∼80 per cent of planetary nebulae (PNe) are non-spherical. In the Binary Hypothesis, a binary interaction is a preferred channel to form a non-spherical PN. A ... More
Reviewed: Reviewed
Date: 2013
Language: eng
Resource Type: journal article
Identifier: http://hdl.handle.net/1959.14/271264
Description: We still do not know what causes aspherical planetary nebula (PN) morphologies. A plausible hypothesis is that they are due to the presence of a close stellar or substellar companion. So far, only ~40 ... More
Full Text: Full Text
Reviewed: Reviewed
Date: 2012
Language: eng
Resource Type: conference paper
Identifier: http://hdl.handle.net/1959.14/216128
Description: 4 page(s)
Full Text: Full Text
Date: 2011
Language: eng
Resource Type: journal article
Identifier: http://hdl.handle.net/1959.14/165789
Description: The α formalism is a common way to parametrize the common envelope interaction between a giant star and a more compact companion. The α parameter describes the fraction of orbital energy released by t ... More
Reviewed: Reviewed
Date: 2010
Language: eng
Resource Type: conference paper abstract
Identifier: http://hdl.handle.net/1959.14/1218088
Description: 1 page(s)
Date: 2006
Language: eng
Resource Type: conference paper
Identifier: http://hdl.handle.net/1959.14/1142531
Description: We present a population synthesis calculation to derive the total number of planetary nebulae (PNe) in the Galaxy from single stars and binaries. By combining the most up-to-date literature results re ... More
Reviewed: Reviewed
Date: 2005
Language: eng
Resource Type: conference paper
Identifier: http://hdl.handle.net/1959.14/1164879
Description: 4 page(s)
Reviewed: Reviewed
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