PoS(ICRC2021)982 International th 12–23 July 2021 July 12–23 37 SICS CONFERENCE SICS CONFERENCE Berlin | Germany Berlin Berlin | Germany Cosmic Ray Conference Ray Cosmic ICRC 2021 THE ASTROPARTICLE PHY ICRC 2021 THEASTROPARTICLE PHY https://pos.sissa.it/ fast-moving

b,d 35 M ONLINE , respectively. The magnetic 1 − and L. Oskinova c 40 km s and 20 M. Petrov a,b M. Pohl, ∗ a, [email protected] International Cosmic Ray Conference (ICRC 2021) Presenter ∗ Copyright owned by the author(s) under the terms of the Creative Commons th Max Planck Computing andGermany Data Facility (MPCDF), Gieÿenbachstrasse 2,Department D-85748 of Garching, Astronomy, Kazan FederalE-mail: University, Kremlevskaya Str 18, Kazan, Russia When a massive star isrunaway swung stellar away object from the is stellar produced,can cluster and in be its which surroundings observed. it is forms, shapeda Such a as supernova so-called arc-like a explosion, bow circumstellar shock and, nebularoundings which the results is interaction in the an of site asymmetricappearance the of of supernova supernova those remnant. the supernova shock remnants, star's We by wave investigatelations death means with the and of via radiative synchrotron 2D its transfer magneto-hydrodynamical calculations sur- simu- of the remnant left behind a Institut für Physik undPotsdam, Astronomie, Germany Universität Potsdam, Karl-Liebknecht-Strasse 24/25,DESY 14476 Platanenallee 6, D-15738 Zeuthen, Germany star. The progenitor starmotion evolves through up the to magnetised the ISMeld Wolf-Rayet is of phase of the and ISM thein has considered the a space tail stabilising of eectsynchrotron the regarding radiation pre-supernova to of stellar the our wind wind/ISM simulationhas bubble. models interface characteristic indicate developing features Radiative that accounting transfer non-thermal for radio calculations theRayet emission morphology for progenitor of stars. our exiled remnantsthe The of non-thermal Wolf- synthetic radio prediction appearance ofCTB109, are Kes several qualitatively 17 remnants in and from G296.5+10.0. massive accordance progenitors with such as b c d a © Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). D. M.-A. Meyer, 37 July 12th  23rd,Online 2021  Berlin, Germany Non-thermal radio supernova remnantsWolf-Rayet of stars exiled PoS(ICRC2021)982 high-mass

D. M.-A. Meyer 20 M ≥ in2. Section Our results

35 M code [1214] in a 2D fashion, using an 2 pluto code [19] to obtain normalised non-thermal synchrotron emission radmc-3d Wolf-Rayet stars are a possible nal evolutionary phase of some Indeed, amongst the several mechanisms at work in the shaping of core-collapse super- In this study, we investigate the morphologies of supernova remnants from Wolf-Rayet We rst simulate the interaction between the stellar wind of the moving progenitor nova remnants, the gasthe distribution ambient generated medium by is the ofinitial prime stellar progenitor importance. wind mass at of Itsthrough level the the a of zero-age progenitor larger complexity main-sequence with is number phase,gas, proportional of i.e. such to evolutionary as the higher-mass the phases, red stars each supergiantFamous evolve example of and of Wolf-Rayet them materials, such into core-collapse releasing their supernova shells remnantsor stellar are surroundings of RWC the [9]. 86 enriched Cygnus Loop [11], nebulatics which [10], both of an exhibit o-centered featuresprogenitor supernova that star explosion are animated inside in by of accordance a the fast, with stellar supersonic the wind bulk characteris- bubble motion. stars. of By an means evolved ofchrotron radiative emission transfer maps. calculations, We detail we theemission predict methods their of used to non-thermal supernova perform radio remnants the syn- simulations of of a synthetic runaway high-mass star, then the supernova happeningof in the it, supernova and, remnantsnamical nally, for we simulations non-thermal estimate are the synchrotron performed emission emission. with properties the The magnetohydrody- Non-thermal remnants of Wolf-Rayet stars 1. Introduction stars. A fraction ofhaving Wolf-Rayet been stars ejected fast-move through fromtravel their the to the local stellar high-galactic ambient latitudes, cluster low-density medium theylive, regions after they of form experience the ISM in, a [14]. so-called and, core-collapsecircumstellar At supernova sometimes, medium the explosion pre-shaped end that they of by happens can the their inside strong of even strong, winds the dense of the wind, progenitor runaway star Wolf-Rayet-evolving [57].candidates stellar for objects Expelling the are production rst of choice progenitor asymmetric core-collapse supernova remnants [8]. for the remnant structure andin Section4. their emission are in Section3. We present our2. conclusions Methods axisymmetric cylindrical coordinate system.centered onto We its inject origin, the and,from the stellar pre-calculated stellar evolutionary wind wind tracks in properties [15].releasing a are The in time-dependently small supernova the interpolated remnant region circumstellar phase medium isblastwave at calculated [16, the in 17]. pre-supernova phase Several ainvolved core-collapse passive in supernova scalar our problem, tracers i.e. permitejecta. the to unperturbed separate Then, ambient the medium, for dierent stellarreconstruct representative material wind 3D selected and emissivity supernova times cubes oftion using with the the the supernova recipe remnant's ofmaps. evolution, [18] we and perform line-of-sight integra- PoS(ICRC2021)982

M - . The 35 1 and its − 3 -long trail − 78 cm D. M.-A. Meyer 100 pc . = 20 km s ∼ ? = 0 v . Since the progenitor 1 − ISM n , and, the blue lines highlight the = 40 km s K 7 ? v 10 and 6 . The two inset boxes zoom on two particular 3 = 10 channel which pierced the wind bubble formed µG T 7 contribution of ejecta in number density. The stellar 70 pc ∼ 10% progenitor runaway star moving with (see text for details).

1 − 35 M -axis, is of strength = 20 km s z ? v Number density eld in our simulation of a supernova remnant of a runaway Fig.2 is as Fig.1 for our simulation model with Fig.1 shows the number density eld of in our magneto-hydrodynamical model of a star moves faster, itsscale circumstellar bow medium shock. adopts Thetrace a elongation of cone-like of the shape the pre-main-sequence cavity ratherof stellar of than the wind stellar a bubble stellar wind remains large surroundings issupernova within more at shock the pronounced, the wave and has pre-supernova no laments. interacted time. It against interacts At the with the walls themedium former plotted of while bow the time recovering shock, sphericity, cavity, instance, expanding and, creating into the it the long, is unperturbed dense quickly ambient channelled into the unshocked wind. regions, the lamentary ejecta-wind-ISMof the interactions wind (left cavity inset)contours generated mark and temperature by contours the the for unstable motion of walls the progenitor star (right inset). The red ambient medium in whichmagnetization, the parallel star to the moves symmetry is axismotion, of of along the number the simulation and density to the direction of stellar location of the remnantmotion with produced a anduring elongated the main-sequence phase ofthe the star. dense The bow supernova shockexpands shock wave freely of has in the interacted the with progenitor opposite ahead direction. of the direction of stellar motion, while it supernova remnant of a Figure 1: star moving with 3. Results Non-thermal remnants of Wolf-Rayet stars PoS(ICRC2021)982 . After ◦ = 0 . obs 1 θ D. M.-A. Meyer − = 40 km s ? v and to a lesser degree at the remnants look rounder. One and the ◦ ◦ , shown at several evolutionary times, and 1 4 − = 45 = 45 obs obs θ θ after the explosion, the shock wave has already been and the brightest region on the sides adopt a bilateral = 20 km s . Once distorted by the interaction with its circumstellar ? 6 kyr v , each of them corresponding to a ring in the trail of shocked obs ◦ 20 kyr θ As Fig.1 for our progenitor moving with = 90 . At time obs 1 θ − the observer's line-of-sight is aligned with the direction of stellar motion, ◦ Figure 2: = 40 km s = 90 ? v , the remnant has an bulb-like morphology which arises from both the shock wave obs In4 Fig. we show the emission maps corresponding to the simulation with progenitor In Fig.3 we plot emission maps for non-thermal radio synchrotron emission of the θ same remnant can appear with bilateralFor or arced structures depending on the viewing angle. greatly distorted by the Wolf-Rayet circumstellar materialan and ovoid-like has structure. lost sphericity Later toappears become in spherical time, in the the shock radio wave map adopts for a hour-glass-like shape that speed for dierent viewing angles, morphology. For an inclination angle and the projected remnantnature appears of as the magneto-hydrodynamical a models. ring-like structure in the sky, because of the 2D medium, the supernova shock wave isthe well traced expanding by shock the non-thermal wave radioarcs arrives radiation. are at When larger the than unperturbed at ISM, time it becomes bright. The radio remnant model with velocity Non-thermal remnants of Wolf-Rayet stars 40 kyr expansion into the ISMof and unshocked the stellar channeling wind of inthe the the shock tail. shock wave intercepts wave The the into radioconcentric trail the rings intensity of for peak low-density stellar cavity shifts wind to (Fig.4d,e).stellar the wind We location would interacting observe where with a the series channelled of supernova shock wave. PoS(ICRC2021)982 (right 40 kyr ◦ = 90 obs θ D. M.-A. Meyer (top panels), 6 kyr at times 1 − (middle panels), and ◦ = 45 = 20 km s ? obs v θ 5 (left panels), ◦ = 0 (bottom panels) after the explosion of the supernova, respectively. The obs θ 80 kyr Emission maps of radio synchrotron intensity plotted in normalised units for our simula- panels). (middle panels), and viewing angle between is Figure 3: tion of supernova remnants moving with velocity Non-thermal remnants of Wolf-Rayet stars PoS(ICRC2021)982 1 − and

30 M = 40 km s ? v D. M.-A. Meyer ts the bilateral . 1 1 − − = 40 km s = 20 km s ? v ? ]. v ? 6 As for Fig.1 for a stellar motion of Figure 4: progenitors, respectively, are consistent with our simulation with

Our models are qualitatively consistent with the radio appearance of several remnants 40 M - of high-mass progenitors [8]. Particularly our model with supernova remnant G296.5+10.0 [20] hasISM been and to constrained host to a neutron by star. expanding in The shell-type magnetised remnants CTB109 and Kes 17, of Non-thermal remnants of Wolf-Rayet stars 20 from which we produced shelled supernova remnants [21 PoS(ICRC2021)982 D. M.-A. Meyer stellar progenitors that

M 40 - 25 7 N. Ramiaramanantsoa T., 2017, MNRAS, 467, 3 949-958 680 The explosion of a core-collapse explosion into the circumstellar medium of a runaway The authors acknowledge the North-German Supercomputing Alliance (HLRN) for [1] Munoz M., Moat A. F. J., Hill G. M., Shenar T., Richardson[2] N. D.,Toalá Pablo J. H, A., St-Louis Oskinova L. M.,[3] Hamann W.-R.,Moat Ignace A. R. F. et J., Marchenko al., S. 2018, V., MNRAS, Seggewiss 869, W., 1 van der Hucht[4] et al.,Meyer, 1998, D. AAp, M. 331, -A., Oskinova L.[5] M., PohlFranco M., J., Petrov Tenorio-Tagle G., M., Bodenheimer 2020, P., MNRAS, Rozyczka[6] 496, M., 3 1991,Rozyczka PASP, M., 103, Tenorio-Tagle 803-810 G., Franco J., Bodenheimer P., 1993, MNRAS, 261,[7] 674- Dwarkadas V. V., 2007, ApJ, 667, 226-247 massive Wolf-Rayet star generatesof complex magneto-hydrodynamical remnant shocks, nebula.winds contact of It discontinuities the is between defunctrials made the progenitor therein of dierent and is a supernova stellar ecient ejecta, succession of when respectively. the the explosion The supernova after mixing blastwaveSuch having is region of interacted are reverberated mate- believed with towards to theing the the circumstellar site center magneto-hydrodynamical medium location simulations of of and non-thermalsynthetic the particles non-thermal radiative progenitor. acceleration. radio-intensity transfer maps Combin- revealing calculations, seriesin we of projection, large-scale produce which arcs we and interpret laments from as runaway being Wolf-Rayet the stars. typicalthe characteristic morphology of These of supernova radio many remnants observedand emission core-collapse G296.5+10.0 maps which supernova have remnants are probably like qualitatively been CTB produced similar 109, by Kes to 17 Non-thermal remnants of Wolf-Rayet stars 4. Conclusion providing HPC resourcespaper. that have MP contributed acknowledges toproviding data the the storage resources Max research and Planck HPC resultsthe resources PLUTO Computing reported which code. contributed and in to This test Data researchof this and made Facility optimize Torino use (MPCDF) by of the for A.PYTHON PLUTO Mignone programming code language developed and at collaborators, the University the MATPLOTLIB plotting libraryReferences for the might have experienced a Wolf-Rayet evolutionary phase [8]. Acknowledgement PoS(ICRC2021)982 D. M.-A. Meyer 8 Green A. J., 2010, ApJ, 712, 2 450 ApJs&A, 198 A., 2007, ApJ, 170 127 [8] Katsuda S., Takiwaki T., Tominaga N., Moriya T. J., Nakamura[9] K.,Meyer 2018, D. ApJ, M. 863, -A., Pohl M., Petrov M., Oskinova L. M., 2021, MNRAS 502, 4 [21] Kothes R., Foster T. , 2012, ApJ Letters, 746, L4 [17] Meyer, D. M. -A., Petrov, M.[18] ;Jun Pohl, B.-I., M. Norman , M. 2020, L., MNRAS, 1996, 493,[19] ApJ, 3 Dullemond 472, C. 245 P., Astrophysics Source Code[20] Library, SoftwareHarvey-Smith 1202.015 L., Gaensler B. M., Kothes R., Townsend R., Heald G. H., Ng C. -Y., [14] Vaidya B., Mignone A., Bodo G.,[15] RossiMeyer P., Massaglia D. S., M.-A., 2018, van Marle ApJ, A.-J., 865,[16] Kuiper 144 Meyer R., D. Kley M.-A., W., Langer 2016, MNRAS, N., 459 Mackey J., Velázquez P. F., Gusdorf A., 2015, MNRAS, [13] Mignone A., Zanni C., Tzeferacos P., van Straalen B., Colella P., Bodo G., 2012, [10] Fang J., Yu H., Zhang L.,[11] 2017, MNRAS,Broersen 464 S., Chiotellis A., Vink J.,[12] BambaMignone A., A., 2014, Bodo MNRAS, G., 441, Massaglia 2 S., Matsakos T., Tesileanu O., Zanni, C. and Ferrari, Non-thermal remnants of Wolf-Rayet stars