arXiv subjects

Jessica Braudo

Publications and source records attributed to Jessica Braudo.

7 recordsLinked to original sources

arXiv2026

One Precessing Jet Pair, Diverse Core-Collapse Supernova Remnant Morphologies

We produce a diverse set of observed core-collapse supernova (CCSN)-type morphologies using a precessing pair of opposite jets within the jittering-jets explosion mechanism (JJEM) framework. We conduct a three-dimensional hydrodynamical simulation of a precessing pair of jets that explode a massive star, and find that a single precessing pair of opposite jets can generate S-shaped structures, pipe-spout-blowout features as observed in the Cygnus Loop, multiple apparent pairs of opposite protrusions similar to some morphological features in S147, and H-shaped structures with a prominent bar, similar to the one observed in the 3C 397 remnant. At small scales, the jets form clumps and filaments, resulting from instabilities and vortices that the jets induce in the ejecta as they interact with the stellar material. We did not aim the simulation to reproduce any particular CCSN remnant, but rather to explore the resulting morphological features. Our finding of simulated features similar to observed ones supports the role of jets in exploding CCSNe and, in turn, supports the claim that the JJEM is the primary explosion mechanism of CCSNe.

astro-ph.HE↗

arXiv2026

Simulating observed point-symmetric core-collapse supernova morphologies with the jittering jets explosion mechanism

We conduct two three-dimensional hydrodynamic simulations of the jittering-jets explosion mechanism (JJEM) of core-collapse supernova (CCSN), launching three pairs of inclined opposite jets into the core of an enveloped-stripped stellar model, and reproduce some morphological features of observed CCSN remnants (CCSNRs) that a single pair of jets or instabilities alone cannot reproduce. We launch the three pairs of jets within about a second, and follow the ejecta for more than 10 seconds until after shock breakout. Our main findings are: (1) Although the jets are choked deep inside the star, they manage to form a pronounced multipolar (point-symmetric) morphology. (2) Instabilities and vortices resulting from the jet-star interaction form small clumps and narrow filaments, some of which form point-symmetric morphology, resembling some observed CCSNRs. (3) The most energetic jet of one simulation forms a large low-density blowout ahead of the ejecta, with filaments dragging behind it, resembling the blowout of the Cygnus Loop. (4) The inner ejecta presents two symmetry axes along two of the three jet axes: one of a pair of rings and one of a pair of nozzles, resembling the structure of the point-symmetric SNR J0450.4-7050. (5) The three pairs of jets compress two dense blocks between their axes. The blocks exhibit a Doppler-shift bipolar outflow highly inclined to the morphological axes along the jet axes. The inclined Doppler-bipolar outflow and morphology axis resembles the CCSNRe W49B and SNR G292.0+1.8. Our study supports the claim that the JJEM is the primary explosion mechanism of CCSNe.

astro-ph.HE↗

arXiv2026

The jet-shaped pipe morphology in planetary nebulae and core-collapse supernova remnants

We compare images of core-collapse supernova (CCSN) remnants (CCSNRs) and jet-shaped planetary nebulae (PNe) that have a narrow, faint zone extending from side to side, termed a pipe, with a hydrodynamical numerical simulation exploding a massive star with three pairs of jets in the framework of the jittering jets explosion mechanism (JJEM), and conclude that jets shaped the pipes in these CCSNRs and PNe. We present two jet-shaped PNe with a pipe and three PNe with two opposite narrow jet-shaped lobes, and argue that in some cases the two opposite narrow lobes might merge to form one long, faint zone extending from side to side of the PN, namely, a pipe. From the qualitative similarity of the pipe morphology of the two CCSNRs we analyze with the pipe of the PNe, we suggest that jets also shaped the pipe of these CCSNRs. We strengthen this conclusion with a three-dimensional hydrodynamic simulation that reproduces two opposite narrow lobes, similar to those observed in PNe with lobes. These lobes can merge later to form a pipe. This paper is another in a series that strengthen the case for the JJEM as the primary explosion mechanism of CCSNe by comparing CCSNR morphologies with those of jet-shaped PNe.

astro-ph.HE↗

arXiv2025

Simulating the shaping of point-symmetric structures in the jittering jets explosion mechanism

We conduct three-dimensional hydrodynamical simulations of core-collapse supernovae by launching several pairs of jets into a collapsing core model and show that the jittering jets explosion mechanism (JJEM) can form a point-symmetric morphology that accounts for observed morphologies of about a dozen core-collapse supernovae (CCSN) remnants. Point-symmetric morphologies are composed of pairs of opposite structures around the center of the CCSN remnant. In the JJEM, the newly born neutron star launches several to a few tens of pairs of jets with stochastically varying directions, and these jets explode the star. In the simulations with the FLASH numerical code, we launch pairs of jets with varying directions, energies, opening angles, and durations into the massive stellar core and follow their evolution for about two seconds. We show that the jets form pairs of opposite filaments, clumps, bubbles, and lobes, namely, prominent point-symmetric morphologies. The interaction of the jets with the core leads to vigorous Rayleigh-Taylor instabilities and excites many vortices, which also shape clumps and filaments. Our results suggest that the JJEM could play a central role in the explosion mechanism of CCSNe; neutrino heating can boost the role of jets.

astro-ph.HE↗

arXiv2024

Difficulties of two exploding white dwarfs to account for type Ia supernovae with bimodal nebular emission profiles

We use a simple dynamical scheme to simulate the ejecta of type Ia supernova (SN Ia) scenarios with two exploding white dwarfs (WDs) and find that the velocity distribution of the ejecta has difficulties accounting for bimodal emission line profiles with a large separation between the two emission peaks. The essence of the dynamical code is in including the fact that the ejecta does not leave the system instantaneously. We find that the final separation velocity between the centers of masses of the two WDs' ejecta is ~80% of the pre-explosion WDs' orbital velocity, i.e., we find separation velocities of 4200-5400 km/s for two WDs of masses M1=M2=0.94 Mo. The lower separation velocities we find challenge scenarios with two exploding WDs to explain bimodal emission line profiles with observed velocity separations of up to ~7000 km/s. Only the mass in the ejecta of one WD with an explosion velocity lower than the separation velocity contributes to one peak of the bimodal profile; this is the inner ejecta. We find the inner ejecta to be only <15% of the ejecta mass in energetic explosions. Less energetic explosions yield higher inner mass but lower separation velocities. We encourage searching for alternative explanations of bimodal line profiles.

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arXiv2023

The runaway velocity of the white dwarf companion in the double detonation scenario of supernovae

We consider the finite velocity of the ejecta of a type Ia supernova (SN Ia) in the double detonation (DDet) scenario with a white dwarf (WD) mass-donor companion, and find that the runaway velocity of the surviving (mass donor) WD is lower than its pre-explosion orbital velocity by about 8-11%. This implies that the fastest runaway WDs in the Galaxy, if come from the DDet scenario, require even more massive WDs than what a simple calculation that neglects the finite ejecta velocity gives. This extreme set of initial conditions makes such binaries less common. We also tentatively find that the inner ejecta deviates from spherical symmetry, but not to the degree that we can use observations to make any claim. Our findings support the claim that the DDet scenario leads mostly to peculiar SNe Ia but not to normal SNe Ia.

astro-ph.HE↗

arXiv2021

Accretion induced merger leading to core collapse supernovae in old stellar populations

We examine a triple-star evolution that might lead to core collapse supernovae (CCSNe) in stellar populations that are too old to allow for single or binary evolution to form CCSNe, i.e., where the most massive stars that evolve off the main sequence have masses of ~4-5Mo. In the scenario we examine the most massive star in the triple system, of mass ~4-5Mo, transfers mass to an inner binary system at an orbital separation of ~100-1000Ro. The initial orbital separation of the inner binary is ~10-50Ro. The inner binary accretes most of the mass that the primary star loses and the two stars expand and their mutual orbit contracts until merger. The merger product is a main sequence star of mass ~8-10Mo that later experiences a CCSN explosion and leaves a NS remnant, bound or unbound to the white dwarf (WD) remnant of the primary star. We estimate the event rate of this WD-NS reverse evolution scenario to be a fraction of ~5e-5 of all CCSNe. We expect that in the coming decade sky surveys will detect 1-5 such events.

astro-ph.HE↗