scholarly journals Estimating the outcomes of common envelope evolution in triple stellar systems

2020 ◽  
Vol 498 (2) ◽  
pp. 2957-2967
Author(s):  
T A F Comerford ◽  
R G Izzard
Keyword(s):  
Planetary Nebula ◽  
Dynamical Instability ◽  
Stellar Systems ◽  
Dynamical Friction ◽  
Numerical Techniques ◽  
Dynamical Interaction ◽  
New Model ◽  
Common Envelope ◽  
Binary Separation ◽  
Early Stages

ABSTRACT We present a new model describing the evolution of triple stars that undergo common envelope evolution, using a combination of analytical and numerical techniques. The early stages of evolution are driven by dynamical friction with the envelope, which causes the outer triple orbit to shrink faster than the inner binary. In most cases, this leads to a chaotic dynamical interaction between the three stars, culminating in the ejection of one of the stars from the triple. This ejection and resulting recoil on the remnant binary are sufficient to eject all three stars from the envelope, which expands and dissipates after the stars have escaped. These results have implications for the properties of post-common envelope triples: they may only exist in cases where the envelope was ejected before the onset of dynamical instability, the likelihood of which depends on the initial binary separation and the envelope structure. In cases where the triple becomes dynamically unstable, the triple does not survive and the envelope dissipates without forming a planetary nebula.

scholarly journals When nature tries to trick us

2018 ◽  
Vol 619 ◽  
pp. A84 ◽  
Author(s):  
Henri M. J. Boffin ◽  
David Jones ◽  
Roger Wesson ◽  
Yuri Beletsky ◽  
Brent Miszalski ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Binary Star ◽  
Central Star ◽  
Equal Mass ◽  
Type I ◽  
Eclipsing Binary ◽  
Common Envelope ◽  
Bright Object ◽  
F Stars ◽  
Central Stars

Bipolar planetary nebulae (PNe) are thought to result from binary star interactions and, indeed, tens of binary central stars of PNe have been found, in particular using photometric time-series that allow for the detection of post-common envelope systems. Using photometry at the NTT in La Silla we have studied the bright object close to the centre of PN M 3-2 and found it to be an eclipsing binary with an orbital period of 1.88 days. However, the components of the binary appear to be two A or F stars, of almost equal mass, and are therefore too cold to be the source of ionisation of the nebula. Using deep images of the central star obtained in good seeing conditions, we confirm a previous result that the central star is more likely much fainter, located 2″ away from the bright star. The eclipsing binary is thus a chance alignment on top of the planetary nebula. We also studied the nebular abundance and confirm it to be a Type I PN.

scholarly journals The post-common-envelope, binary central star of the planetary nebula Hen 2-11

2014 ◽  
Vol 562 ◽  
pp. A89 ◽  
Author(s):  
D. Jones ◽  
H. M. J. Boffin ◽  
B. Miszalski ◽  
R. Wesson ◽  
R. L. M. Corradi ◽  
...  
Keyword(s):  
Planetary Nebula ◽  
Central Star ◽  
Common Envelope

scholarly journals Common envelope to explosion delay time of Type Ia supernovae

2019 ◽  
Vol 490 (2) ◽  
pp. 2430-2435 ◽  
Author(s):  
Noam Soker
Keyword(s):  
Delay Time ◽  
Planetary Nebula ◽  
Time Distribution ◽  
Circumstellar Matter ◽  
Type Ia Supernovae ◽  
Common Envelope ◽  
Type Ia ◽  
Explosion Delay ◽  
Ia Supernovae ◽  
Short Times

ABSTRACT I study the rate of Type Ia supernovae (SNe Ia) within about a million years after the assumed common envelope evolution (CEE) that forms the progenitors of these SNe Ia, and find that the population of SNe Ia with short CEE to explosion delay (CEED) time is ≈few × 0.1 of all SNe Ia. I also claim for an expression for the rate of these SNe Ia that occur at short times after the CEE ($t_{\rm CEED} \lesssim 10^6 {~\rm yr}$), which is different from that of the delay time distribution (DTD) billions of years after star formation. This tentatively hints that the physical processes that determine the short CEED time distribution (CEEDTD) are different (at least to some extent) from those that determine the DTD at billions of years. To reach these conclusions I examine SNe Ia that interact with a circumstellar matter (CSM) within months after explosion, so-called SNe Ia-CSM, and the rate of SNe Ia that on a time-scale of tens to hundreds of years interact with a CSM that might have been a planetary nebula, so-called SNe Ia inside a planetary nebula (SNIPs). I assume that the CSM in these populations results from a CEE, and hence this study is relevant mainly to the core-degenerate (CD) scenario, the double-degenerate (DD) scenario, the double-detonation (DDet) scenario with white dwarf companions, and to the CEE-wind channel of the single-degenerate (SD) scenario.

scholarly journals Powering and Shaping Planetary Nebulae: The Physics of Common Envelopes

2015 ◽  
Vol 11 (A29B) ◽  
Author(s):  
Jason Nordhaus ◽  
David S. Spiegel
Keyword(s):  
Planetary Nebula ◽  
Planetary Nebulae ◽  
Asymptotic Giant Branch ◽  
Close Binary ◽  
Observational Constraints ◽  
Asymptotic Giant Branch Stars ◽  
Common Envelope ◽  
Accretion Rates ◽  
Binary Channels ◽  
Giant Branch Stars

AbstractThe diversity of collimated outflows in post-asymptotic-giant-branch stars and their planetary nebula progeny are often explained by a combination of close binary interactions and accretion. The viability of such scenarios can be tested by comparing kinematic outflow data to determine minimum accretion rates necessary to power observed outflows. While many binary channels have been ruled out with this technique, common envelope interactions can accommodate the current observational constraints, are potentially common, lead to a diverse array of planetary-nebula shapes, and naturally produce period gaps for companions to white dwarfs.

scholarly journals A Physicist’s View of Stellar Dynamics: Dynamical Instability of Stellar Systems

2005 ◽  
Vol 13 ◽  
pp. 354-357 ◽  
Author(s):  
V.G. Gurzadyan
Keyword(s):  
Linear Systems ◽  
Integrable Systems ◽  
Current Knowledge ◽  
Stellar Dynamics ◽  
Dynamical Instability ◽  
Stellar Systems ◽  
Non Linear ◽  
Non Linear Systems ◽  
Gravitating Systems

AbstractI argue that the widely adopted framework of stellar dynamics survived since 1940s, is not fitting the current knowledge on non-linear systems. Borrowed from plasma physics when several fundamental features of perturbed non-linear systems were unknown, that framework ignores the difference in the role of perturbations in two different classes of systems, in plasma with Debye screening and gravitating systems with no screening. Now, when the revolutionary role of chaotic effects is revealed even in planetary dynamics i.e. for nearly integrable systems, one would expect that for stellar systems, i.e. non-integrable systems, their role have to be far more crucial. Indeed, ergodic theory tools already enabled to prove that spherical stellar systems are exponentially instable due to N-body interactions, while the two-body encounters, contrary to existing belief, are not the dominating mechanism of their relaxation. Chaotic effects distinguish morphological and other properties of galaxies. Using the Ricci curvature criterion, one can also show that a central massive object (nucleus) makes the N-body gravitating system more instable (chaotic), while systems with double nuclei are even more instable than those with a single one.

scholarly journals The EREBOS project: Investigating the effect of substellar and low-mass stellar companions on late stellar evolution

2019 ◽  
Vol 630 ◽  
pp. A80 ◽  
Author(s):  
V. Schaffenroth ◽  
B. N. Barlow ◽  
S. Geier ◽  
M. Vučković ◽  
D. Kilkenny ◽  
...  
Keyword(s):  
Stellar Evolution ◽  
Planetary Nebula ◽  
Eclipsing Binaries ◽  
Atmospheric Parameter ◽  
Reflection Effect ◽  
Common Envelope ◽  
Period Distribution ◽  
Hot Subdwarfs ◽  
Substellar Companions ◽  
Central Stars

Eclipsing post-common-envelope binaries are highly important for resolving the poorly understood, very short-lived common-envelope phase of stellar evolution. Most hot subdwarfs (sdO/Bs) are the bare helium-burning cores of red giants that have lost almost all of their hydrogen envelope. This mass loss is often triggered by common-envelope interactions with close stellar or even substellar companions. Cool companions to hot subdwarf stars such as late-type stars and brown dwarfs are detectable from characteristic light-curve variations – reflection effects and often eclipses. In the recently published catalog of eclipsing binaries in the Galactic Bulge and in the Asteroid Terrestrial-impact Last Alert System (ATLAS) survey, we discovered 125 new eclipsing systems showing a reflection effect seen by visual inspection of the light curves and using a machine-learning algorithm, in addition to the 36 systems previously discovered by the Optical Gravitational Lesing Experiment (OGLE) team. The Eclipsing Reflection Effect Binaries from Optical Surveys (EREBOS) project aims at analyzing all newly discovered eclipsing binaries of the HW Vir type (hot subdwarf + close, cool companion) based on a spectroscopic and photometric follow up to derive the mass distribution of the companions, constrain the fraction of substellar companions, and determine the minimum mass needed to strip off the red-giant envelope. To constrain the nature of the primary we derived the absolute magnitude and the reduced proper motion of all our targets with the help of the parallaxes and proper motions measured by the Gaia mission and compared those to the Gaia white-dwarf candidate catalog. It was possible to derive the nature of a subset of our targets, for which observed spectra are available, by measuring the atmospheric parameter of the primary, confirming that less than 10% of our systems are not sdO/Bs with cool companions but are white dwarfs or central stars of planetary nebula. This large sample of eclipsing hot subdwarfs with cool companions allowed us to derive a significant period distribution for hot subdwarfs with cool companions for the first time showing that the period distribution is much broader than previously thought and is ideally suited to finding the lowest-mass companions to hot subdwarf stars. The comparison with related binary populations shows that the period distribution of HW Vir systems is very similar to WD+dM systems and central stars of planetary nebula with cool companions. In the future, several new photometric surveys will be carried out, which will further increase the sample of this project, providing the potential to test many aspects of common-envelope theory and binary evolution.

scholarly journals The Real-Time Evolution of V4334 Sgr

Galaxies ◽  
2018 ◽  
Vol 6 (3) ◽  
pp. 79 ◽  
Author(s):  
Peter van Hoof ◽  
Stefan Kimeswenger ◽  
Griet Van de Steene ◽  
Adam Avison ◽  
Albert Zijlstra ◽  
...  
Keyword(s):  
Real Time ◽  
Time Evolution ◽  
Planetary Nebula ◽  
Spectral Features ◽  
The Real ◽  
Thermal Pulse ◽  
Early Stages ◽  
Observational Record

V4334 Sgr (Sakurai’s object) is an enigmatic evolved star that underwent a very late thermal pulse a few years before its discovery in 1996. It ejected a new hydrogen-deficient nebula in the process. The source has been observed continuously since, at many wavelengths ranging from the optical to the radio regime. In this paper we evaluate these data and discuss the evolution of this object. We reach the conclusion that we have seen no evidence for photoionization of the nebula yet and that the spectral features we see are caused either by shocks or by dust. These shocks are an integral part of the hydrodynamic shaping that is now producing a new bipolar nebula inside the old planetary nebula (PN), implying that we have a detailed observational record of the very early stages of the shaping of a bipolar nebula.

scholarly journals ALMA imaging of the nascent planetary nebula IRAS 15103–5754

2018 ◽  
Vol 480 (4) ◽  
pp. 4991-5009 ◽  
Author(s):  
José F Gómez ◽  
Gilles Niccolini ◽  
Olga Suárez ◽  
Luis F Miranda ◽  
J Ricardo Rizzo ◽  
...  
Keyword(s):  
Mass Loss ◽  
High Velocity ◽  
Planetary Nebula ◽  
Symmetry Axis ◽  
Stellar System ◽  
Line Emission ◽  
Ionized Gas ◽  
Molecular Line ◽  
Common Envelope ◽  
Loss Event

ABSTRACT We present continuum and molecular-line (CO, C18O, HCO+) observations carried out with the Atacama Large Millimeter/submillimeter Array toward the ‘water fountain’ star IRAS 15103–5754, an object that could be the youngest planetary nebula (PN) known. We detect two continuum sources, separated by 0.39 ± 0.03 arcsec. The emission from the brighter source seems to arise mainly from ionized gas, thus confirming the PN nature of the object. The molecular-line emission is dominated by a circumstellar torus with a diameter of ≃0.6 arcsec (2000 au) and expanding at ≃23 km s−1. We see at least two gas outflows. The highest-velocity outflow (deprojected velocities up to 250 km s−1), traced by the CO lines, shows a biconical morphology, whose axis is misaligned ≃14° with respect to the symmetry axis of the torus, and with a different central velocity (by ≃8 km s−1). An additional high-density outflow (traced by HCO+) is oriented nearly perpendicular to the torus. We speculate that IRAS 15103–5754 was a triple stellar system that went through a common envelope phase, and one of the components was ejected in this process. A subsequent low-collimation wind from the remaining binary stripped out gas from the torus, creating the conical outflow. The high velocity of the outflow suggests that the momentum transfer from the wind is extremely efficient, or that we are witnessing a very energetic mass-loss event.

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