Bipolar rings from jet-inflated bubbles around evolved binary stars

Akashi, Muhammad; Soker, Noam

doi:10.1093/mnras/stw1683

Cited by 13 publications

(11 citation statements)

References 53 publications

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“…Such a result could be used as a basis for developing a diagnostic to constrain the nature of the binary prior to the onset of the common envelope phase. We note, however, that bipolar lobes can also be produced, in principle, by the action of jet inflated bubbles emanating from the accretion disk surrounding the companion star (Akashi & Soker 2016). Support for the latter interpretation could be provided if indications of a jet exist (e.g., pointsymmetric structures).…”

Section: Discussionmentioning

confidence: 79%

Common Envelope Shaping of Planetary Nebulae

Garcı́a-Segura

Ricker

Taam

2018

ApJ

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The morphology of planetary nebulae emerging from the common envelope phase of binary star evolution is investigated. Using initial conditions based on the numerical results of hydrodynamical simulations of the common envelope phase it is found that the shapes and sizes of the resulting nebula are very sensitive to the effective temperature of the remnant core, the mass-loss rate at the onset of the common envelope phase, and the mass ratio of the binary system. These parameters are related to the efficiency of the mass ejection after the spiral-in phase, the stellar evolutionary phase (i.e., RG, AGB or TP-AGB), and the degree of departure from spherical symmetry in the stellar wind mass loss process itself respectively. It is found that the shapes are mostly bipolar in the early phase of evolution, but can quickly transition to elliptical and barrel-type shapes. Solutions for nested lobes are found where the outer lobes are usually bipolar and the inner lobes are elliptical, bipolar or barrel-type, a result due to the flow of the photo-evaporated gas from the equatorial region. It is found that the lobes can be produced without the need for two distinct mass ejection events. In all the computations, the bulk of the mass is concentrated in the orbital or equatorial plane, in the form of a large toroid, which can be either neutral (early phases) or photoionized (late phases), depending of the evolutionary state of the system.

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Section: Discussionmentioning

confidence: 79%

Common Envelope Shaping of Planetary Nebulae

Garcı́a-Segura

Ricker

Taam

2018

ApJ

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“…The energetic jets in the LAHE simulation, E 2j = 0.2E SN , and their long activity time lead to an interaction that forms a deep along the symmetry axis, one at each side, in the outer boundary of each of the two dense shells. This is a feature we have obtained before when simulating jets in planetary nebulae (Akashi & Soker 2016). To further present the complicated flow structure, in Fig.…”

Section: Other Casesmentioning

confidence: 58%

Simulating the inflation of bubbles by late jets in core collapse supernova ejecta

Akashi,

Soker

2020

Preprint

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We conducted three-dimensional hydrodynamical simulations to study the interaction of two late opposite jets with the ejecta of a core collapse supernova (CCSN), and study the bipolar structure that results from this interaction as the jets inflate hot-low-density bubbles. The newly born central object, a neutron star (NS; or a black hole), launches these jets at about 50 to 100 days after explosion. The bubbles cross the photosphere in the polar directions at much earlier times than the regions at the same radii near the equatorial plane. The hot bubbles releases more radiation and the photosphere recedes more rapidly in the tenuous bubble. Our results strengthen earlier claims that were based on toy models that such an interaction might lead to a late peak in the light curve, and that an equatorial observer might see a rapid drop in the light curve. Our results have implications to much earlier jets that explode the star, either jets that the newly born NS launches in a CCSN, or jets that a NS companion that merges with the core of a massive star launches in a common envelope jets supernova (CEJSN) event. Our results add indirect support to the CEJSN scenario for fast blue optical transients, e.g.,

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“…From the peak or peaks of the lightcuve, the decline in the optical bands with time is similar over almost four magnitudes. This could not be a coincidence, and 10 0 10 1 10 2 10 3 Ordinate: eruption energy. Blue empty circles: total (radiated + kinetic) energy.…”

Section: Common Properties Of Ilotsmentioning

confidence: 99%

Simulations and Modeling of Intermediate Luminosity Optical Transients and Supernova Impostors

Kashi¹

2018

Preprint

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More luminous than classical novae, but less luminous than Supernovae, lies the exotic stellar eruptions known as Intermediate luminosity optical transients (ILOTs). They are divided into a number of sub-groups depending on the erupting progenitor and the properties of the eruption. A large part of the ILOTs is positioned on the slanted Optical Transient Stripe (OTS) in the Energy-Time Diagram (ETD) that shows their total energy vs. duration of their eruption. We describe the different kinds of ILOTs that populate the OTS and other parts of the ETD. The high energy part of the OTS hosts the supernova impostors -giant eruption (GE) of very massive stars. We show results of 3D hydrodynamical simulations of GEs that expose the mechanism behind these GEs, and present new models for recent ILOTs. We discuss the connection between different kinds of ILOTs, and suggest that they have a common energy source -gravitational energy released by mass transfer. We emphasize similarities between Planetary Nebulae (PN) and ILOTs, and suggest that some PNe were formed in an ILOT event. Therefore, simulations used for GEs can be adapted for PNe, and used for learning about the influence of the ILOT events on the the central star of the planetary nebula.

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Bipolar rings from jet-inflated bubbles around evolved binary stars

Cited by 13 publications

References 53 publications

Common Envelope Shaping of Planetary Nebulae

Common Envelope Shaping of Planetary Nebulae

Simulating the inflation of bubbles by late jets in core collapse supernova ejecta

Simulations and Modeling of Intermediate Luminosity Optical Transients and Supernova Impostors

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