Common envelope jets supernova (CEJSN) impostors resulting from a neutron star companion

Gilkis, Avishai; Soker, Noam; Kashi, Amit

doi:10.1093/mnras/sty3008

Cited by 62 publications

(61 citation statements)

References 107 publications

(156 reference statements)

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“…Such cases take place when the NS manages to eject the entire envelope before it spirals-in into the core, or when it enters the envelope on an eccentric orbit and exits the envelope. This energetic outburst leads to an intermediate luminous optical transient (ILOT) that is termed a CEJSN impostor (Gilkis et al 2019). Later the core explodes and leaves behind another NS, or BH, either bound or not to the first NS.…”

Section: The Key Role Of the Accretion Ratementioning

confidence: 99%

Diversity of common envelope jets supernovae and the fast transient AT2018cow

Soker

Grichener

Gilkis

2019

Monthly Notices of the Royal Astronomical Society

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145

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We propose a common-envelope jets supernova (CEJSN) scenario for the fast-rising blue optical transient AT2018cow. In a CEJSN a neutron star (NS) spirals-in inside the extended envelope of a massive giant star and enters the core. The NS accretes mass from the core through an accretion disc and launches jets. These jets explode the core and the envelope. In the specific polar CEJSN scenario that we propose here the jets clear the polar regions of the giant star before the NS enters the core. The jets that the NS launches after it enters the core expand almost freely along the polar directions that contain a small amount of mass. This, we suggest, explains the fast rise to maximum and the fast ejecta observed at early times of the enigmatic transient AT2018cow. The slower later time ejecta is the more massive equatorial outflow. We roughly estimate the accretion phase onto the NS during the explosion phase to last for a time of ≈ 10 3 s, during which the average mass accretion rate is ≈ 10 −4 M s −1 . We outline the possible diversity of CEJSNe by listing five other scenarios in addition to the polar CEJSN scenario.

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Section: The Key Role Of the Accretion Ratementioning

confidence: 99%

Diversity of common envelope jets supernovae and the fast transient AT2018cow

Soker

Grichener

Gilkis

2019

Monthly Notices of the Royal Astronomical Society

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145

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“…Each periastron passage also makes the binary less eccentric. Gilkis, Soker, & Kashi (2019) discuss the passage of a NS through the envelope of a giant star, likely on an eccentric orbit, and conclude that the system might be able to eject the envelope or lead to a merger between the NS and the core, which they call a CE jets SN (Soker & Gilkis 2018, see also Schrøder et al 2020. The former results in a less luminous transient, comparable in energetic to luminous red novae (Kashi & Soker 2016).…”

Section: Modelling Of Mass Transfer In Eccentric Binariesmentioning

confidence: 99%

Common envelope episodes that lead to double neutron star formation

Vigna-Gómez

MacLeod

Neijssel

et al. 2020

Publ. Astron. Soc. Aust.

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Close double neutron stars (DNSs) have been observed as Galactic radio pulsars, while their mergers have been detected as gamma-ray bursts and gravitational wave sources. They are believed to have experienced at least one common envelope episode (CEE) during their evolution prior to DNS formation. In the last decades, there have been numerous efforts to understand the details of the common envelope (CE) phase, but its computational modelling remains challenging. We present and discuss the properties of the donor and the binary at the onset of the Roche lobe overflow (RLOF) leading to these CEEs as predicted by rapid binary population synthesis models. These properties can be used as initial conditions for detailed simulations of the CE phase. There are three distinctive populations, classified by the evolutionary stage of the donor at the moment of the onset of the RLOF: giant donors with fully convective envelopes, cool donors with partially convective envelopes, and hot donors with radiative envelopes. We also estimate that, for standard assumptions, tides would not circularise a large fraction of these systems by the onset of RLOF. This makes the study and understanding of eccentric mass-transferring systems relevant for DNS populations.

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“…In the common envelope jet supernova (CEJSN) scenario the source of explosion energy is the accretion of gas from a red supergiant (RSG) star onto a neutron star (NS) or a black hole (BH), hereafter NS/BH, that spirals-in inside the RSG, first inside the envelope and then inside the RSG core (e.g., Papish et al 2015;Soker & Gilkis 2018;Gilkis et al 2019;Grichener & Soker 2019a;López-Cámara et al 2019Soker 2021). The accretion process proceeds via an accretion disk that launches energetic jets that explode the star.…”

Section: Introductionmentioning

confidence: 99%

A common envelope jets supernova (CEJSN) impostor scenario for fast blue optical transients

Soker

2022

Preprint

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I propose a new scenario, the polar common envelope jets supernova (CEJSN) impostor scenario, to account for AT2018cow-like fast blue optical transients (FBOTs). The polar CEJSN impostor scenario evolves through four main phases. (1) A red supergiant (RSG) star expands to tidally interact with a neutron star (NS) companion (or a black hole). The interaction increases the RSG mass loss rate to form a circumstellar matter (CSM) halo to r 0.1 pc. (2) Shortly before the onset of a common envelope evolution (CEE) and about a year before explosion the NS accretes mass from the RSG envelope and launches jets that inflate two opposite lobes in the CSM within ≈ 100 AU. (3) The NS-RSG system enters a CEE phase during which the system ejects most of the envelope mass in a dense equatorial outflow. (4) At the termination of the CEE the leftover envelope forms a circumbinary disk around the NS-core system. The NS accretes mass from the circumbinary disk and launches energetic jets that when collide with the fronts of the CSM lobes power an FBOT event. The low mass of the jets-lobes interaction zones and their large distance, of about 100 AU, from the center account for the fast transient. In the future the core collapses to form a second NS. In the far future the two NS might merge. I suggest that FBOTs and similar fast transients are CEJSN impostors which compose a large fraction of the progenitors of NS-NS merger binaries.

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Common envelope jets supernova (CEJSN) impostors resulting from a neutron star companion

Cited by 62 publications

References 107 publications

Diversity of common envelope jets supernovae and the fast transient AT2018cow

Diversity of common envelope jets supernovae and the fast transient AT2018cow

Common envelope episodes that lead to double neutron star formation

A common envelope jets supernova (CEJSN) impostor scenario for fast blue optical transients

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