Forming equatorial rings around dying stars

Akashi, Muhammad; Sabach, Efrat; Yogev, Ohad; Soker, Noam

doi:10.1093/mnras/stv1666

Cited by 26 publications

(28 citation statements)

References 49 publications

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“…The presence of a companion significantly influences the evolution of massive stars (Podsiadlowski & Price 1992;Langer et al 2008;Eldridge 2011), and the widespread importance of stellar mass transfer in binary systems has only been realized recently. In the case of MWC 137, circumstellar material may accumulate in the Roche lobe of a putative (smaller) companion to form a disk-like structure, from which a jet could be launched (Harmanec et al 1996;Ak et al 2007;Akashi et al 2015). In such disks, one does not expect any dust, which is consistent with the lack of dust emission found for MWC 137.…”

Section: Mwc 137 E(b-v)supporting

confidence: 57%

VLT/MUSE discovers a jet from the evolved B[e] star MWC 137

Mehner

Wit

Groh

et al. 2015

A&A

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Aims. Not all stars exhibiting the optical spectral characteristics of B [e] stars are in the same evolutionary stage. The Galactic B[e] star MWC 137 is a prime example of an object with uncertain classification, where previous work has suggested either a pre-or a postmain sequence classification. Our goal is to settle this debate and provide a reliable evolutionary classification. Methods. Integral field spectrograph observations with the Very Large Telescope Multi Unit Spectroscopic Explorer (VLT MUSE) of the cluster SH 2-266 are used to analyze the nature of MWC 137. Results. A collimated outflow is discovered that is geometrically centered on MWC 137. The central position of MWC 137 in the cluster SH 2-266 within the larger nebula suggests strongly that it is a member of this cluster and that it is the origin of both the nebula and the newly discovered jet. Comparison of the color-magnitude diagram of the brightest cluster stars with stellar evolutionary models results in a distance of about 5.2 ± 1.4 kpc. We estimate that the cluster is at least 3 Myr old. The jet emanates from MWC 137 at a position angle of 18-20• . The jet extends over 66 (1.7 pc) projected on the plane of the sky, shows several knots, and has electron densities of about 10 3 cm −1 and projected velocities of up to ±450 km s −1 . From the Balmer emission line decrement of the diffuse intracluster nebulosity, we determine E(B-V) = 1.4 mag for the inner 1 cluster region. The spectral energy distribution of the brightest cluster stars yields a slightly lower extinction of E(B-V) ∼ 1.2 mag for the inner region and E(B-V) ∼ 0.4-0.8 mag for the outer region. The extinction toward MWC 137 is estimated to be E(B-V) ∼ 1.8 mag (A V ∼ 5.6 mag). Conclusions. Our analysis of the optical and near-infrared color-magnitude and color-color diagrams suggests a post-main sequence stage for MWC 137. The existence of a jet in this object implies the presence of an accretion disk. Several possibilities for MWC 137's nature and the origin of its jet are discussed: e.g., the presence of a companion and a merger event.

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Section: Mwc 137 E(b-v)supporting

confidence: 57%

VLT/MUSE discovers a jet from the evolved B[e] star MWC 137

Mehner

Wit

Groh

et al. 2015

A&A

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“…The swept-up shell in the equatorial plane fractures into clumps due to hydrodynamical instabilities. Formation of such a clumpy ring can be obtained in different settings, such as a propagation of a jet into a spherical shell (Akashi et al 2015). An animated version of this figure is available in the online material.…”

Section: Discussionmentioning

confidence: 99%

Pre-explosion Spiral Mass Loss of a Binary Star Merger

Pejcha

Metzger

Tyles

et al. 2017

ApJ

108

158

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Binary stars commonly pass through phases of direct interaction which result in the rapid loss of mass, energy, and angular momentum. Though crucial to understanding the fates of these systems, including their potential as gravitational wave sources, this short-lived phase is poorly understood and has thus far been unambiguously observed in only a single event, V1309 Sco. Here we show that the complex and previously-unexplained photometric behavior of V1309 Sco prior to its main outburst results naturally from the runaway loss of mass and angular momentum from the outer Lagrange point, which lasts for thousands of orbits prior to the final dynamical coalescence, much longer than predicted by contemporary models. This process enshrouds the binary in a "death spiral" outflow, which affects the amplitude and phase modulation of its light curve, and contributes to driving the system together. The total amount of mass lost during this gradual phase (∼ 0.05 M ⊙ ) rivals the mass lost during the subsequent dynamical interaction phase, which has been the main focus of "common envelope" modeling so far. Analogous features in related transients suggest that this behavior is ubiquitous.

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“…This paper is another one in our series of papers aiming at exploring the role of jets in shaping some nebulae around evolved stars (Akashi & Soker 2008a,b;Akashi et al 2015). The new ingredient we have added is a fast spherical wind blown after the shaping by jets.…”

Section: Discussion and Summarymentioning

confidence: 99%

“…These bubbles can lead to other morphological features such as a dense equatorial outflow (Soker & Rappaport 2000;Akashi & Soker 2008b;Akashi et al 2015). The rich variety of outflow types, such as slow winds and fast winds that can be blown, before, during, and after the jets-launching episodes, and the rich variety of interacting binary (Soker 1998;De Marco 2015) and triple (Soker 2016) stellar systems ensure the rich variety of descendant nebular morphologies, practically making almost every bipolar nebula 'unique' (Soker 2002b).…”

Section: Introductionmentioning

confidence: 99%

Bipolar rings from jet-inflated bubbles around evolved binary stars

Akashi¹,

Soker²

2016

Mon. Not. R. Astron. Soc.

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We show that a fast wind that expands into a bipolar nebula composed of two opposite jetinflated bubbles can form a pair of bipolar rings around giant stars. Our model assumes three mass loss episodes: a spherical slow and dense shell, two opposite jets, and a spherical fast wind. We use the FLASH hydrodynamical code in three-dimensions to simulate the flow, and obtain the structure of the nebula. We assume that the jets are launched from an accretion disk around a stellar companion to the giant star. The accretion disk is assumed to be formed when the primary giant star and the secondary star suffer a strong interaction accompanied by a rapid mass transfer process from the primary to the secondary star, mainly a main sequence star. Later in the evolution the primary star is assumed to shrink and blow a fast tenuous wind that interacts with the dense gas on the surface of the bipolar structure. We assume that the dense mass loss episode before the jets are launched is spherically symmetric. Our results might be applicable to some planetary nebulae, and further emphasize the large variety of morphological features that can be formed by jets. But we could not reproduce some of the properties of the outer rings of SN 1987A. It seems that some objects, like SN 1987A, require a pre-jets mass loss episode with a mass concentration at mid-latitudes.

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Forming equatorial rings around dying stars

Cited by 26 publications

References 49 publications

VLT/MUSE discovers a jet from the evolved B[e] star MWC 137

VLT/MUSE discovers a jet from the evolved B[e] star MWC 137

Pre-explosion Spiral Mass Loss of a Binary Star Merger

Bipolar rings from jet-inflated bubbles around evolved binary stars

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