Supernova 1987A's Keyhole:A Long-lived Jet-pair in the Final Explosion Phase of Core-collapse Supernovae

I further study the manner by which a pair of opposite jets shape the“keyhole”morphological structure of the core-collapse supernova(CCSN)SN 1997A,now the CCSN remnant(CCSNR)1987A.By doing so,I strengthen the claim that the jittering-jet explosion mechanism accounts for most,likely all,CCSNe.The“keyhole”structure comprises a northern low-intensity zone closed with a bright rim on its front and an elongated low-intensity nozzle in the south.This rim-nozzle asymmetry is observed in some cooling flow clusters and planetary nebulae that are observed to be shaped by jets.I build a toy model that uses the planar jittering jets pattern,where consecutive pairs of jets tend to jitter in a common plane,implying that the accreted gas onto the newly born neutron star at the late explosion phase flows perpendicular to that plane.This allows for a long-lived jet-launching episode.This long-lasting jet-launching episode launches more mass into the jets that can inflate larger pairs of ears or bubbles,forming the main jets'axis of the CCSNR that is not necessarily related to a possible pre-collapse core rotation.I discuss the relation of the main jets'axis to the neutron star's natal kick velocity.

The Neutron Star to Black Hole Mass Gap in the Frame of the Jittering Jets Explosion Mechanism(JJEM)

I build a toy model in the frame of the jittering jets explosion mechanism(JJEM)of core collapse supernovae that incorporates both the stochastically varying angular momentum component of the material that the newly born neutron star(NS)accretes and the constant angular momentum component,and show that the JJEM can account for the≃2.5–5M⊙mass gap between NSs and black holes(BHs).The random component of the angular momentum results from pre-collapse core convection fluctuations that are amplified by post-collapse instabilities.The fixed angular momentum component results from pre-collapse core rotation.For slowly rotating pre-collapse cores the stochastic angular momentum fluctuations form intermittent accretion disks(or belts)around the NS with varying angular momentum axes in all directions.The intermittent accretion disk/belt launches jets in all directions that expel the core material in all directions early on,hence leaving an NS remnant.Rapidly rotating pre-collapse cores form an accretion disk with angular momentum axis that is about the same as the pre-collapse core rotation.The NS launches jets along this axis and hence the jets avoid the equatorial plane region.Inflowing core material continues to feed the central object from the equatorial plane increasing the NS mass to form a BH.The narrow transition from slow to rapid pre-collapse core rotation,i.e.,from an efficient to inefficient jet feedback mechanism,accounts for the sparsely populated mass gap.

On the Nature of Jets from a Main Sequence Companion at the Onset of Common Envelope Evolution

I consider a flow structure by which main sequence companions that enter a common envelope evolution(CEE)with giant stars might launch jets even when the accreted gas has a sub-Keplerian specific angular momentum.I first show that after a main sequence star enters the envelope of a giant star the specific angular momentum of the accreted gas is sub-Keplerian but still sufficiently large for the accreted gas to avoid two conical-like openings along the two opposite polar directions.I suggest that the high-pressure zone that the accreted gas builds around the main sequence equatorial plane accelerates outflows along these polar openings.Most of the inflowing gas is deflected to the polar outflows,i.e.,two oppositely directed jets.The actual mass that the main sequence star accretes is only a small fraction,≈0.1,of the inflowing gas.However,the gravitational energy that this gas releases powers the inflow-outflow streaming of gas and adds energy to the common envelope ejection.This flow structure might take place during a grazing envelope evolution if it occurs,during the early CEE and possibly in some post-CEE cases.This study increases the parameter space for main sequence stars to launch jets.Such jets might shape some morphological features in planetary nebulae,add energy to mass removal in CEE and power some intermediate luminosity optical transients.

The Depletion of the Red Supergiant Envelope Radiative Zone During Common Envelope Evolution

We conduct one-dimensional stellar evolution simulations of red supergiant(RSG)stars that mimic common envelope evolution(CEE)and find that the inner boundary of the envelope convective zone moves into the initial envelope radiative zone.The envelope convection practically disappears only when the RSG radius decreases by about an order of magnitude or more.The implication is that one cannot split the CEE into one stage during which the companion spirals-in inside the envelope convective zone and removes it,and a second slower phase when the companion orbits the initial envelope radiative zone and a stable mass transfer takes place.At best,this might take place when the orbital separation is about several solar radii.However,by that time other processes become important.We conclude that as of yet,the commonly used alpha-formalism that is based on energy considerations is the best phenomenological formalism.

Point-symmetry in SNR G1.9+0.3:A Supernova that Destroyed its Planetary Nebula Progenitor

I analyze a new X-ray image of the youngest supernova remnant(SNR)in the Galaxy,which is the type Ia SNR G1.9+0.3,and reveal a very clear point-symmetrical structure.Since explosion models of type Ia supernovae(SNe Ia)do not form such morphologies,the point-symmetrical morphology must come from the circumstellar material(CSM)into which the ejecta expands.The large-scale point-symmetry that I identify and the known substantial deceleration of the ejecta of SNR G1.9+0.3 suggest a relatively massive CSM of■1M⊙.I argue that the most likely explanation is the explosion of this SN Ia into a planetary nebula.The scenario that predicts a large fraction of SN Ia inside PNe(SNIPs)is the core degenerate scenario.Other SN Ia scenarios might lead to only a very small fraction of SNIPs or none at all.

Operation of the jet feedback mechanism (JFM) in intermediate luminosity optical transients (ILOTs)

We follow the premise that most intermediate luminosity optical transients （ILOTs） are powered by rapid mass accretion onto a main sequence star, and study the effects of jets launched by an accretion disk. The disk is formed due to large specific angular momentum of the accreted mass. The two opposite jets might expel some of the mass from the reservoir of gas that feeds the disk, and therefore reduce and shorten the mass accretion process. We argue that by this process ILOTs limit their luminosity and might even shut themselves off in this negative jet feedback mechanism （JFM）. The group of ILOTs is a new member of a large family of astrophysical objects whose activity is regulated by the operation of the JFM.

The Role of Jets in Exploding Supernovae and in Shaping their Remnants

I review studies of core collapse supernovae(CCSNe) and similar transient events that attribute major roles to jets in powering most CCSNe and in shaping their ejecta. I start with reviewing the jittering jets explosion mechanism that I take to power most CCSN explosions. Neutrino heating does play a role in boosting the jets. I compare the morphologies of some CCSN remnants to planetary nebulae to conclude that jets and instabilities are behind the shaping of their ejecta. I then discuss CCSNe that are descendants of rapidly rotating collapsing cores that result in fixed-axis jets(with small jittering) that shape bipolar ejecta. A large fraction of the bipolar CCSNe are superluminous supernovae(SLSNe). I conclude that modeling of SLSN light curves and bumps in the light curves must include jets, even when considering energetic magnetars and/or ejecta interaction with the circumstellar matter(CSM). I connect the properties of bipolar CCSNe to common envelope jets supernovae(CEJSNe) where an old neutron star or a black hole spirals-in inside the envelope and then inside the core of a red supergiant. I discuss how jets can shape the pre-explosion CSM, as in Supernova 1987A, and can power pre-explosion outbursts(precursors)in binary system progenitors of CCSNe and CEJSNe. Binary interaction also facilitates the launching of postexplosion jets.

Imprints of the Jittering Jets Explosion Mechanism in the Morphology of the Supernova Remnant SNR 0540-69.3

I identify a point-symmetric structure in recently published VLT/MUSE velocity maps of different elements in a plane along the line of sight at the center of the supernova remnant SNR 0540-69.3,and argue that jittering jets that exploded this core collapse supernova shaped this point-symmetric structure.The four pairs of two opposite clumps that compose this point symmetric structure suggest that two to four pairs of jittering jets shaped the inner ejecta in this plane.In addition,intensity images of several spectral lines reveal a faint strip(the main jet-axis)that is part of this plane of jittering jets and its similarity to morphological features in a few other SNRs and in some planetary nebulae further suggests shaping by jets.My interpretation implies that in addition to instabilities,jets also mix elements in the ejecta of core collapse supernovae.Based on the point-symmetric structure and under the assumption that jittering jets exploded this supernova,I estimate the component of the neutron star natal kick velocity on the plane of the sky to be■235 km s^(-1),and at an angle of■47°to the direction of the main jet-axis.I analyze this natal kick direction together with 12 other SNRs in the frame of the jittering jets explosion mechanism.

Common Envelope to Explosion Delay time Distribution(CEEDTD)of Type Ia Supernovae

I use recent observations of circumstellar matter(CSM)around type Ia supernovae(SNe Ia)to estimate the fraction of SNe Ia that explode into a planetary nebula(PN)and to suggest a new delay time distribution from the common envelope evolution(CEE)to the SN Ia explosion for SNe Ia that occur shortly after the CEE.Under the assumption that the CSM results from a CEE,I crudely estimate that about 50%of all SNe Ia are SNe Ia inside PNe(SNIPs),and that the explosions of most SNIPs occur within a CEE to explosion delay(CEED)time of less than about ten thousand years.I also estimate that the explosion rate of SNIPs,i.e.,the CEED time distribution,is roughly constant within this timescale of ten thousand years.The short CEED time suggests that a fraction of SNIPs come from the core-degenerate(CD)scenario where the merger of the core with the white dwarf takes place at the end of the CEE.I present my view that the majority of SNIPs come from the CD scenario.I list some further observations that might support or reject my claims,and describe the challenge to theoretical studies to find a process to explain a merger to explosion delay(MED)time of up to ten thousand years or so.A long MED will apply also to the double degenerate scenario.

Amplifying magnetic fields of a newly born neutron star by stochastic angular momentum accretion in core collapse supernovae

I present a novel mechanism to boost magnetic field amplification of newly born neutron stars in core collapse supernovae.In this mechanism,that operates in the jittering jets explosion mechanism and comes on top of the regular magnetic field amplification by turbulence,the accretion of stochastic angular momentum in core collapse supernovae forms a neutron star with strong initial magnetic fields but with a slow rotation.The varying angular momentum of the accreted gas,which is unique to the jittering jets explosion mechanism,exerts a varying azimuthal shear on the magnetic fields of the accreted mass near the surface of the neutron star.This,I argue,can form an amplifying effect which I term the stochastic omega(Sω) effect.In the common αω dynamo the rotation has constant direction and value,and hence supplies a constant azimuthal shear,while the convection has a stochastic behavior.In the Sω dynamo the stochastic angular momentum is different from turbulence in that it operates on a large scale,and it is different from a regular rotational shear in being stochastic.The basic assumption is that because of the varying direction of the angular momentum axis from one accretion episode to the next,the rotational flow of an accretion episode stretches the magnetic fields that were amplified in the previous episode.I estimate the amplification factor of the Sω dynamo alone to be ≈ 10.I speculate that the Sω effect accounts for a recent finding that many neutron stars are born with strong magnetic fields.

The circumstellar matter of type II intermediate luminosity optical transients(ILOTs)

I find that a≃0.1−1M⊙outflowing equatorial dusty disk(torus)that the binary system progenitor of an intermediate luminosity optical transient(ILOT)ejects several years to several months before and during the outburst can reduce the total emission to an equatorial observer by two orders of magnitude and shifts the emission to wavelengths of mainlyλ≳10μm.This is termed a type II ILOT(ILOT II).To reach this conclusion,I use calculations of type II active galactic nuclei and apply them to the equatorial ejecta(disk/torus)of ILOTs II.This reduction in emission can last for tens of years after outburst.Most of the radiation escapes along the polar directions.The attenuation of the emission for wavelengths ofλ<5μm can be more than three orders of magnitude,and the emission atλ\lessim2μm is negligible.Jets that the binary system launches during the outburst can collide with polar CSM and emit radiation above the equatorial plane and dust in the polar outflow can reflect emission from the central source.Therefore,during the event itself the equatorial observer might detect an ILOT.I strengthen the previously suggested ILOT II scenario to the event N6946-BH1,where a red giant star disappeared in the visible.

Rescuing the intracluster medium of NGC 5813

We use recent X-ray observations of the intracluster medium （ICM） of the galaxy group NGC 5813 to confront theoretical studies of ICM thermal evolution with the newly derived ICM prop- erties. We argue that the ICM of the cooling flow in the galaxy group NGC 5813 is more likely to be heated by mixing of post-shock gas from jets residing in hot bubbles with the ICM, than by shocks or turbulent- heating. Shocks thermalize only a small fraction of their energy in the inner regions of the cooling flow; in order to adequately heat the inner part of the ICM, they would overheat the outer regions by a large factor, leading to its ejection from the group. Heating by mixing, which was found to be much more efficient than turbulent-heating and shocks-heating, hence, rescues the outer ICM of NGC 5813 from its predestined fate according to cooling flow feedback scenarios that are based on heating by shocks.

A Pre-explosion Effervescent Zone for the Circumstellar Material in SN 2023ixf

I present the effervescent zone model to account for the compact dense circumstellar material(CSM)around the progenitor of the core collapse supernova(CCSN)SN 2023ixf.The effervescent zone is composed of bound dense clumps that are lifted by stellar pulsation and envelope convection to distances of≈tens×au,and then fall back.The dense clumps provide most of the compact CSM mass and exist alongside the regular(escaping)wind.I crudely estimate that for a compact CSM within R_(CSM)≈30 au that contains M_(CSM)≈0.01 M_(⊙),the density of each clump is k_(b)≳3000 times the density of the regular wind at the same radius and that the total volume filling factor of the clumps is several percent.The clumps might cover only a small fraction of the CCSN photosphere in the first days post-explosion,accounting for the lack of strong narrow absorption lines.The long-lived effervescent zone is compatible with no evidence for outbursts in the years prior to the SN 2023ixf explosion and the large-amplitude pulsations of its progenitor,and it is an alternative to the CSM scenario of several-years-long high mass loss rate wind.

Predicting Gravitational Waves from Jittering-jets-driven Core Collapse Supernovae

I estimate the frequencies of gravitational waves from jittering jets that explode core collapse supernovae(CCSNe)to crudely be 5–30 Hz,and with strains that might allow detection of Galactic CCSNe.The jittering jets explosion mechanism(JJEM)asserts that most CCSNe are exploded by jittering jets that the newly born neutron star(NS)launches within a few seconds.According to the JJEM,instabilities in the accreted gas lead to the formation of intermittent accretion disks that launch the jittering jets.Earlier studies that did not include jets calculated the gravitational frequencies that instabilities around the NS emit to have a peak in the crude frequency range of 100–2000Hz.Based on a recent study,I take the source of the gravitational waves of jittering jets to be the turbulent bubbles(cocoons)that the jets inflate as they interact with the outer layers of the core of the star at thousands of kilometers from the NS.The lower frequencies and larger strains than those of gravitational waves from instabilities in CCSNe allow future,and maybe present,detectors to identify the gravitational wave signals of jittering jets.Detection of gravitational waves from local CCSNe might distinguish between the neutrino-driven explosion mechanism and the JJEM.

Classifying Core Collapse Supernova Remnants by Their Morphology as Shaped by the Last Exploding Jets

Under the assumption that jets explode all core collapse supernovae(CCSNe),I classify 14 CCSN remnants(CCSNRs)into five groups according to their morphology as shaped by jets,and attribute the classes to the specific angular momentum of the pre-collapse core.Point-symmetry(one CCSNR):According to the jittering jets explosion mechanism(JJEM)when the pre-collapse core rotates very slowly,the newly born neutron star(NS)launches tens of jet-pairs in all directions.The last several jet-pairs might leave an imprint of several pairs of“ears,”i.e.,a point-symmetric morphology.One pair of ears(eight CCSNRs):More rapidly rotating cores might force the last pair of jets to be long-lived and shape one pair of jet-inflated ears that dominates the morphology.S-shaped(one CCSNR):The accretion disk might precess,leading to an S-shaped morphology.Barrel-shaped(three CCSNRs):Even more rapidly rotating pre-collapse cores might result in a final energetic pair of jets that clear the region along the axis of the pre-collapse core rotation and form a barrel-shaped morphology.Elongated(one CCSNR):A very rapidly rotating pre-collapse core forces all jets to be along the same axis such that the jets are inefficient in expelling mass from the equatorial plane and the long-lasting accretion process turns the NS into a black hole.The two new results of this study are the classification of CCSNRs into five classes based on jet-shaped morphological features,and the attribution of the morphological classes mainly to the pre-collapse core rotation in the frame of the JJEM.

Launching jets from accretion belts

We propose that sub-Keplerian accretion belts around stars might launch jets. The sub-Keplerian inflow does not form a rotationally supported accretion disk, but it rather reaches the accreting object from a wide solid angle. The basic ingredients of the flow are a turbulent region where the accretion belt interacts with the accreting object via a shear layer, and two avoidance regions on the poles where the accretion rate is very low. A dynamo that is developed in the shear layer amplifies magnetic fields to high values. It is likely that the amplified magnetic fields form polar outflows from the avoidance regions. Our speculative belt-launched jets model has implications on a rich variety of astrophysical objects, from the removal of common envelopes to the explosion of core collapse supernovae by jittering jets.

Using Intermediate-Luminosity Optical Transients(ILOTs) to reveal extended extra-solar Kuiper belt objects

We suggest that in the rare case of an Intermediate-Luminosity Optical Transient（ILOT） event,evaporation of extra-solar Kuiper belt objects（Extra KBOs） at distances of dth to a few years, enough d≈500ust mig-10 000 AU from the ILOT can be detected. If the ILOT lasts for 1 monht be ejected from the Extra KBOs for the infrared（IR） emission to be detected. Because of the large distance of the Extra KBOs,tens of years will pass before the ILOT wind disperses the dust. We suggest that after an ILOT outburst,there is a period of months to several years during which IR excess emission might hint at the existence of a Kuiper belt analog（Extra K-Belt）.

Reviving the stalled shock by jittering jets in core collapse supernovae: jets from the standing accretion shock instability

I present a scenario by which an accretion flow with alternating angular momentum on to a newly born neutron star in a core collapse supernova(CCSN) efficiently amplifies magnetic fields and by that launches jets.The accretion flow of a collapsing core on to the newly born neutron star suffers spiral standing accretion shock instability(SASI).This instability leads to a stochastically variable angular momentum of the accreted gas,which in turn forms an accretion flow with alternating directions of the angular momentum,and hence alternating shear,at any given time.I study the shear in this alternating-shear sub-Keplerian inflow in published simulations,and present a new comparison with Keplerian accretion disks.From that comparison I argue that it might be as efficient as Keplerian accretion disks in amplifying magnetic fields by a dynamo.I suggest that although the average specific angular momentum of the accretion flow is small,namely,sub-Keplerian,this alternating-shear accretion flow can launch jets with varying directions,namely,jittering jets.Neutrino heating is an important ingredient in further energizing the jets.The jittering jets locally revive the stalled accretion shock in the momentarily polar directions,and by that they explode the star.I repeat again my call for a paradigm shift from a neutrino-driven explosion of CCSNe to a jet-driven explosion mechanism that is aided by neutrino heating.

Boosting Jittering Jets by Neutrino Heating in Core Collapse Supernovae

I estimate the energy that neutrino heating adds to the outflow that jets induce in the collapsing core material in core collapse supernovae(CCSNe), and find that this energy crudely doubles the energy that the jets deposit into the outer core. I consider the jittering jets explosion mechanism where there are several stochastic jet-launching episodes, each lasting for about 0.01–0.1 s. The collapsing core material passes through the stalled shock at about100 km and then slowly flows onto the proto-neutron star(NS). I assume that the proto-NS launches jittering jets,and that the jets break out from the stalled shock. I examine the boosting process by which the high-pressure gas inside the stalled shock, the gain region material, expands alongside the jets and does work on the material that the jets shock, the cocoon. This work is crudely equal to the energy that the original jets carry. I argue that the coupling between instabilities, stochastic rotation, magnetic fields, and jittering jets leads to most CCSN explosions. In other cases, the pre-collapse core is rapidly rotating and therefore ordered rotation replaces stochastic rotation and fixed jets replace jittering jets.

Pre-explosion Helium Shell Flash in Type Ia Supernovae

I study the possibility that within the frame of the core degenerate(CD)scenario for type Ia supernovae(SNe Ia)the merger process of the core of the asymptotic giant branch(AGB)star and the white dwarf(WD)maintains an envelope mass of≈0.03 Mthat causes a later helium shell flash.I estimate the number of pre-explosion helium shell flash events to be less than a few per cent of all CD scenario SNe Ia.A helium shell flash while the star moves to the left on the HR diagram as a post-AGB star(late thermal pulse—LTP)or along the WD cooling track(very LTP—VLTP)causes the star to expand and become a“born again”AGB star.Merger remnants exploding while still on the AGB form hydrogen-polluted peculiar SNe Ia,while an explosion inside an inflated born-again star results in an early flux excess in the light curve of the SN Ia.The fraction of systems that might show an early flux excess due to LTP/VLTP is<few×10^(-4) of all SNe Ia,much below the observed fraction.In the frame of the CD scenario SNe Ia with early flux excess result from SN ejecta collision with planetary nebula fallback gas,or from mixing of ^(56) Ni to the outer regions of the SN ejecta.Ongoing sky surveys might find about one case per year where LTP/VLTP influences the SN light curve.