A Possible Hidden Population of Spherical Planetary Nebulae
Autor: | Eyal Subag, Noam Soker |
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Jazyk: | angličtina |
Rok vydání: | 2005 |
Předmět: |
Physics
Toy model Quantitative Biology::Neurons and Cognition Astrophysics (astro-ph) Binary number FOS: Physical sciences Astronomy and Astrophysics Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Planetary nebula Computer Science::Computers and Society Luminosity Space and Planetary Science Planet Hidden populations Visible band Astrophysics::Solar and Stellar Astrophysics Halo Astrophysics::Galaxy Astrophysics |
Popis: | We argue that relative to non-spherical planetary nebulae (PNs), spherical PNs are about an order of magnitude less likely to be detected, at distances of several kiloparsecs. Noting the structure similarity of halos around non-spherical PNs to that of observed spherical PNs, we assume that most unobserved spherical PNs are also similar in structure to the spherical halos around non-spherical PNs. The fraction of non-spherical PNs with detected spherical halos around them, taken from a recent study, leads us to the claim of a large (relative to that of non-spherical PNs) hidden population of spherical PNs in the visible band. Building a toy model for the luminosity evolution of PNs, we show that the claimed detection fraction of spherical PNs based on halos around non-spherical PNs, is compatible with observational sensitivities. We use this result to update earlier studies on the different PN shaping routes in the binary model. We estimate that ~30% of all PNs are spherical, namely, their progenitors did not interact with any binary companion. This fraction is to be compared with the ~3% fraction of observed spherical PNs among all observed PNs. From all PNs, ~15% owe their moderate elliptical shape to the interaction of their progenitors with planets, while \~55% of all PNs owe their elliptical or bipolar shapes to the interaction of their progenitors with stellar companions. AJ, in press |
Databáze: | OpenAIRE |
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