The ionised and molecular mass of post-common-envelope planetary nebulae. The missing mass problem

AbstractMost planetary nebulae (PNe) show beautiful, axisymmetric morphologies despite their progenitor stars being essentially spherical. Angular momentum provided by a close binary companion is widely invoked as the main agent that would help eject an axisymmetric nebula, after a brief phase of engulfment of the secondary within the envelope of the Asymptotic Giant Branch (AGB) star, known as a common envelope (CE). The evolution on the AGB would thus be interrupted abruptly, its (still quite) massive envelope fully ejected to form the PN, which should be more massive than a PN coming from the same star were it single. We test this hypothesis by deriving the ionised+molecular masses of a pilot sample of post-CE PNe and comparing them to a regular PNe sample. We find the mass of post-CE PNe to be actually lower, on average, than their regular counterparts, raising some doubts on our understanding of these intriguing objects.

Download Full-text

DARK GEOMETRY

International Journal of Modern Physics D ◽

10.1142/s0218271804006322 ◽

2004 ◽

Vol 13 (10) ◽

pp. 2275-2279 ◽

Cited By ~ 31

Author(s):

J. A. R. CEMBRANOS ◽

A. DOBADO ◽

A. L. MAROTO

Keyword(s):

Dark Matter ◽

Extra Dimensions ◽

Degrees Of Freedom ◽

Planck Scale ◽

Point Of View ◽

Missing Mass ◽

Brane Worlds ◽

Mass Problem ◽

Extra Space ◽

The Universe

Extra-dimensional theories contain additional degrees of freedom related to the geometry of the extra space which can be interpreted as new particles. Such theories allow to reformulate most of the fundamental problems of physics from a completely different point of view. In this essay, we concentrate on the brane fluctuations which are present in brane-worlds, and how such oscillations of the own space–time geometry along curved extra dimensions can help to resolve the Universe missing mass problem. The energy scales involved in these models are low compared to the Planck scale, and this means that some of the brane fluctuations distinctive signals could be detected in future colliders and in direct or indirect dark matter searches.

Download Full-text

Tired light and the “missing mass” problem

Acta Physica Academiae Scientiarum Hungaricae ◽

10.1007/bf03158184 ◽

1971 ◽

Vol 30 (3) ◽

pp. 323-329 ◽

Cited By ~ 11

Author(s):

W. Yourgrau ◽

J. F. Woodward

Keyword(s):

Missing Mass ◽

Mass Problem

Download Full-text

Groups of Galaxies and the Missing Mass Problem

Internal Kinematics and Dynamics of Galaxies ◽

10.1007/978-94-009-7075-5_23 ◽

1983 ◽

pp. 95-96

Author(s):

P. N. Appleton ◽

R. D. Davies

Keyword(s):

Missing Mass ◽

Groups Of Galaxies ◽

Mass Problem

Download Full-text

Some Regularities in the Missing Mass Problem

Dark Matter in the Universe ◽

10.1007/978-94-009-4772-6_31 ◽

1987 ◽

pp. 136-136

Author(s):

S. Casertano ◽

J. N. Bahcall

Keyword(s):

Missing Mass ◽

Mass Problem

Download Full-text

Contributions and Prospects for Spectral Classification of Stars with Objective Prism Techniques

International Astronomical Union Colloquium ◽

10.1017/s0252921100104099 ◽

1979 ◽

Vol 47 ◽

pp. 127-136

Author(s):

E. K. Kharadze

Keyword(s):

Galactic Structure ◽

Spectral Classification ◽

Missing Mass ◽

Mass Problem ◽

Important Stage ◽

Objective Prism ◽

Low Dispersion

The following topics will be discussed: a) A few historical comments; b) MK classification - the most important stage of classification work; c) Recently revealed peculiarity features and the problem of further differentiation of the classification scale; d) Classification work in the USSR; e) The role of classification results with respect to galactic structure studies; f) Low dispersion spectra and faint M-type stars and the missing mass problem; g) Extraterrestrial spectral observations: new promising means for research.

Download Full-text

Planetary Nebulae Embryo after a Common Envelope Event

Galaxies ◽

10.3390/galaxies6030075 ◽

2018 ◽

Vol 6 (3) ◽

pp. 75 ◽

Cited By ~ 2

Author(s):

Natalia Ivanova ◽

Jose Nandez

Keyword(s):

Binary Stars ◽

Planetary Nebulae ◽

Close Binary ◽

Common Envelope ◽

Characteristic Speed ◽

Close Binary Stars

In the centers of some planetary nebulae are found close binary stars. The formation of those planetary nebulae was likely through a common envelope event, which transformed an initially-wide progenitor binary into the currently observed close binary, while stripping the outer layers away. A common envelope event proceeds through several qualitatively different stages, each of which ejects matter at its own characteristic speed, and with a different degree of symmetry. Here, we present how typical post-common envelope ejecta looks kinematically a few years after the start of a common envelope event. We also show some asymmetric features we have detected in our simulations (jet-like structures, lobes, and hemispheres).

Download Full-text