On the Origin of Morphological Structures of Planetary Nebulae

Kwok, Sun

doi:10.3390/galaxies6030066

Cited by 7 publications

(7 citation statements)

References 39 publications

(41 reference statements)

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“…This process has been observed in PPNe, with examples ranging from the discovery of the butterfly-shaped PPN IRAS 17106-3046 that shows a disk and a bipolar outflow [28], and Hen 2-90 with bipolar morphology and indication of a disk-jet operation [29], to recent detailed observations of the PPN IRAS 16342-3814 that allowed constraints to be out on the mass accretion rate and the accretion channel [30]. Many more examples can be found in reference [31]. Numerical simulations have shown that jets from a companion can interact with the wind of the AGB to form a bipolar PN [32], or a multi-polar PN [33], and more modern simulations have even demonstrated the formation of a 'messy' PN lacking any type of symmetry, also known as a highly irregular PN, and other simulations have emphasized the large variety of morphological features that can be formed by jets [34,35].…”

Section: Ges In Very Massive Starsmentioning

confidence: 90%

Simulations and Modeling of Intermediate Luminosity Optical Transients and Supernova Impostors

Kashi

2018

Galaxies

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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 eruptions (GE) of very massive stars. We show the results of the 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 (PNe) 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 to learn about the influence of the ILOT events on the central star of the planetary nebula.

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Section: Ges In Very Massive Starsmentioning

confidence: 90%

Simulations and Modeling of Intermediate Luminosity Optical Transients and Supernova Impostors

Kashi

2018

Galaxies

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show abstract

“…This process is observed in PPNe, with examples range from the discovery of the butterfly-shaped PPN IRAS 17106-3046 that shows a disk and a bipolar outflow [25], and Hen 2-90 with bipolar morphology and indication of a disk-jet operation [36], to recent detailed observations of the PPN IRAS 16342-3814 that allow putting constraints on the mass accretion rate and the accretion channel [37]. Many more examples can be found in [24]. Numerical simulations showed that jets from a companion can interact with the wind of the AGB to form a bipolar PN [14], or a multi-polar PN [8], and more modern simulations even demonstrated the formation of a 'messy' PN lacking any type of symmetry, a.k.a.…”

Section: Ges In Very Massive Starsmentioning

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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“…Given that PNe reveal a vast diversity in terms of size, shapes, kinematics etc. [16] while the time delay between the WD formation and the final SN Ia explosion can be from almost zero up to several Gyr [17], the parameter space involved in our modeling is immense. Here, as a first attempt, we consider the case of a bipolar PN as this morphology is one the most common PN morphologies.…”

Section: Hydrodynamic Modeling Of the Csm Shaped By Planetary Nebulaementioning

confidence: 99%

The Interaction of Type Ia Supernovae with Planetary Nebulae: The Case of Kepler’s Supernova Remnant

2020

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One of the key methods for determining the unknown nature of Type Ia supernovae (SNe Ia) is the search for traces of interaction between the SN ejecta and the circumstellar structures at the resulting supernova remnants (SNRs Ia). So far, the observables that we receive from well-studied SNRs Ia cannot be explained self-consistently by any model presented in the literature. In this study, we suggest that the circumstellar medium (CSM) being observed to surround several SNRs Ia was mainly shaped by planetary nebulae (PNe) that originated from one or both progenitor stars. Performing two-dimensional hydrodynamic simulations, we show that the ambient medium shaped by PNe can account for several properties of the CSM that have been found to surround SNe Ia and their remnants. Finally, we model Kepler’s SNR considering that the SN explosion occurred inside a bipolar PN. Our simulations show good agreement with the observed morphological and kinematic properties of Kepler’s SNR. In particular, our model reproduces the current expansion parameter of Kepler’s SNR, the partial interaction of the remnant with a dense CSM at its northern region and finally the existence of two opposite protrusions (‘ears’) at the equatorial plane of the SNR.

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On the Origin of Morphological Structures of Planetary Nebulae

Cited by 7 publications

References 39 publications

Simulations and Modeling of Intermediate Luminosity Optical Transients and Supernova Impostors

Simulations and Modeling of Intermediate Luminosity Optical Transients and Supernova Impostors

Simulations and Modeling of Intermediate Luminosity Optical Transients and Supernova Impostors

The Interaction of Type Ia Supernovae with Planetary Nebulae: The Case of Kepler’s Supernova Remnant

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