PoS(ICRC2021)983 International th 12–23 July 2021 July 12–23 37 SICS CONFERENCE SICS CONFERENCE Berlin | Germany Berlin Berlin | Germany Conference Ray Cosmic ICRC 2021 THE ASTROPARTICLE PHY ICRC 2021 THEASTROPARTICLE PHY https://pos.sissa.it/ ONLINE massive

a,c 60 M and M. Pohl b . These rare objects can evolve to exotic phases of stellar

60 M , into the warm phase of the (ISM), these 1 M. Petrov − ∗ a, 40 km s - 20 [email protected] ∼ large stellar bubble. In the context of a fast-moving stellar motion of the International Cosmic Ray Conference (ICRC 2021) Presenter 100 pc ∗ Copyright owned by the author(s) under the terms of the Creative Commons th DESY Platanenallee 6, D-15738 Zeuthen,E-mail: Germany The initial mass function predictssequence that mass very exceeding few massive starsevolution, can such have as a the zero-age-main- Luminous-Blue-Variabletheir and lives Wolf-Rayet via phases, and a might core-collapsedynamical nish simulations explosion. of the Weboth present surroundings 2D a of high axisymmetric such mass-loss hydro- very ratea massive and , by characterised strong by windorder velocities. of We found that it is shaped as Institut für Physik undPotsdam, Astronomie, Germany Universität Potsdam, Karl-Liebknecht-Strasse 24/25,Max 14476 Planck Computing andGermany Data Facility (MPCDF), Gieÿenbachstrasse 2, D-85748 Garching, stars can escape their own circumstellarwhere bubble. the star The location dies, of iscumstellar the therefore , supernova o-set explosion, and, to as the a geometricalasymmetries consequence, center of the of the subsequent its shaped supernova pre- medium.wind cir- reects We in the nd which that the thewind enriched formed, and distorted, supernova cavity ejecta ISM of materials. expand stellar as hosts We a an propose tracer ecient that of mixing peculiar theremnants. of runaway enrichment nature stellar of of the the ISM high-mass can stellar progenitors be of used these supernova b c a © Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). D. M.-A. Meyer, July 12th  23rd,Online 2021  Berlin, Germany Supernova remnants of a 37 PoS(ICRC2021)983 D. M.-A. Meyer 2 ) are rare stellar objects of huge importance in the cycle

8 M ≥ ? M of all OB-typed stars [3]. When bow-shock-carrying massive stars reach 10% Good candidates are the very high-mass stars evolving through eruptive stellar evo- Our methods in presented in Section2 and show our results in3. Section We conclude In the context of runaway massive stars moving supersonically through their local ISM, High-mass stars ( lutionary phases like thecharacterised Luminous by Blue a Variable strong and/orproperties. increase Wolf-Rayet of These phases, the shells both mass-lossphases and being rate eruptive generate and accumulation a over brutal complexmotion the changes of circumstellar dierent in the post-main-sequence medium, their progenitor wind and,the engenders the as supernova asymmetries remnants an and of additionalstars inhomogeneous those nevertheless eect, cavities exist in stars the and which develop bulk lanic have asymmetric been Cloud. observed shapes. in They bothcircumstellar are So-evolving nebulae our believed, massive and from hence and the toWe the investigate theoretical produce Large the asymmetric point eects Magel- core-collapse of of these supernovathe view, consecutive remnants. shaping post-main-sequence to of evolutionary generate phases wind-blown onto nebulae, distorted stellar see motion also to [12], the and, remnant's we morphology. pay attention of thein eects Section4. of the the end of theirstellar evolution medium and in die which [4,5], theexpanding their supernova supernova surroundings explosion shock are happens wave and the [6].deviations the pre-supernova The circumstellar circum- from interaction medium between sphericity of the to theCygnus defunct the Loop star nebula growing induces [7], supernova Tycho'sthem remnant. [8] involve and lower-mass Kepler's Famous binary supernova companions examples remnant toalso are [9, the directly10], the supernova albeit progenitor. form some Asymmetries during of high-mass can the stars explosion can itself generate,asymmetric [11]. throughout to generate The their the main lives, most question a aspherical is remnants? circumstellar therefore, medium which suciently the symmetry of their circumstellarshape wind called bubble a is stellar-wind broken bowsimilar and shock. it to It is those is distorted constituted in asaround of the an layers, about wind arc-like discontinuities and bubbles shocks forming around a static star. Such bow shocks form of matter of oursurface replenish Galaxy. the interstellar medium The (ISM) with fast,elements. momentum, The energy dense and wind-ISM and heavy interaction chemical of enriched thesescale main-sequence stellar large massive circumstellar stars wind form bubbles, expelled huge whichnebula parsec- classical from are description composed their can of be an found innerwhich in termination encompass [1]. shock a and contact These an discontinuity outer where forward thecold, shock, hot, dense respectively, diluted shocked shocked ISM stellar materials wind andmedium, meet. the and Without considering a any static strong massive perturbationconserve star, of this the their wind-blown symmetry bubbles ambient throughout grow spherically the and several evolutionary phases of the massive star [2]. Supernova remnants of very massive stars 1. Introduction PoS(ICRC2021)983 zero-age

star in which 60 M

D. M.-A. Meyer ). The evolution of 60 M . The ISM properties ? v 40 pc (panel c). 1 ∼ − code [1315] in a 2D axisymmetric = 20 km s ? v pluto (runaway case), respectively. , respectively. Importantly, the advection of 1 3 − 3 − ) in three simulations of supernova remnants 3 − cm 79 cm . (panel a) to 0 1 = 20 km s − ? v = 0 km s ? v (static star) to ), generated during the main-sequence phase of the star. The unstable 1 − massive progenitor. The gures dier by the space velocity of the progenitor

80 pc for a gas number density of ∼ 60 M = 0 km s Numerical simulations are performed with the In Fig.1a we plot the pre-supernova wind bubble of the static We rst simulate the wind-ISM interaction. The corresponding wind-blown bubble is Fig.1 shows the density eld (in ? v 8000 K Supernova remnants of very massive stars 2. Methods are those of the warmof phase of the Galactic plane, which we initially set to a generated by a supernovaof explosion its expanding into thestar, pre-shaped which spans circumstellar from medium the supernova shock wave2D has equivalent of already the started classicalstructure expanding. picture for is The stellar composed wind modelled ofradius bubbles situation [1]. an is The inner the overall termination circumstellar contact discontinuity shock separates and the of shocked,ISM diluted, gas an swept-up evolved during outer stellar the forward wind evolutionwave of and is shock the the clearly massive (at shocked star. visible inthe The expanding the shock supernova center of is atremains still the far spherical from nebula as the (at it ejecta. radius has not interacted with any dense structure, which calculated in the frame of the runaway star, moving with velocity fashion. We use awind-ISM cylindrical coordinate calculations system, [12, as],17 computational utilised domain, and in by previous the interpolating studies tabulated stellarmain-sequence devoted an wind to star evolution is model [16]. of injectedare a within Our therefore modelled the stellar using origin windmedium of the of bubbles, massive stars, formalism the generated see developed e.g. byhydrodynamics, [18]. in with wind-ISM Throughout the an the interaction, simulations, context additional we energy of solveheating the loss the equations and term of circumstellar cooling, accounting for usedHarten-Lax-van optically-thin within Leer radiative a approximate second Riemannat order solver. the nite-volume Max Our scheme Planck calculations makingSupercomputing Computing are Alliance. use and both of Data performed the Facility in Garching and at the North-German 3. Results the gas into theproblem ISM (ambient can medium, be supernova tracked ejecta) and making separatedThen, use from we of the a a other release species a passive core-collapse scalar of supernovainteraction that tracers blastwave in, [13 of our14]. pre-shaped the medium. supernovaextra The ejecta early one-dimensional, high-resolution blastwave simulation with which thecircumstellar we medium map stellar [19, into wind20]. the 2D is Ourto pre-supernova series calculated of with 3 models an dier by the star's bulk motion, taken PoS(ICRC2021)983 = (c) ? v 40 indicates (b) 1 20 D. M.-A. Meyer , i.e. the stellar (a), 1 − 10 20 km s (d) after the explosion, respectively. , shown at times 1 − 200 kyr In Fig.2 we show the time evolution of the Fig.1b shows the density eld in the super- means absence of a given specie, 4 0 motion is supersonic withspeed respect in to the the ISM. sound ter In of this the simulation,shell explosion the of is shocked cen- ISM directlywind and located materials, main-sequence in stellar as the velocity a result of of the theels star faster Fig. 1a,b. compare space Hence, tohas the already that been expanding constrained in and blastwave shaped mod- supernova by gas pre- distribution: itthe expands direction faster opposite in of thatmotion, of the whereas progenitor's itdense interacts bubble strongly in with the the while beginning direction to of further penetrate stellar intoperturbed the motion un- ISM. mixing between stellar wind,and ISM supernova ejecta materials moving20 km s with velocity and Left-hand part of each panelgas is in the the ratio each of grid ISM cell, right-hand part is that remnant simulation generated bymoving a slowly- progenitor. The centeris of shifted from the the explosion geometrical center ofbubble. the wind Whileof the Fig.1a, remnant the is northernshock as wave part is old nearly of interacting as with the thediscontinuity expanding that contact of the stellarresults wind in bubble, mild which changesthe in blastwave. the forward The shock reectionRayet of stellar of wind the against lastface the Wolf- is wind-ISM dierent inter- fromtesties that the in instabilities the in staticrial the case, located between turbulent as the mate- blastwave and theISM wind- interface, as well asing the that same instabilities interface, aect- moresouthern pronounced part in the of the windplot bubble. the In supernova Fig.1c remnant we genitor of moving a with runaway pro- ) of (a), 3 0 − massive cm

60 M (c). 1 − 20 km s Density eld (plotted in (b), and progenitor star, moving with10 velocity Figure 1: the supernova remnants of a of the stellar wind material, respectively ( Supernova remnants of very massive stars that the zone is exclusively made of a particular specie). PoS(ICRC2021)983 can enor-

D. M.-A. Meyer 60 M ∼ of the gas in number density. 10% (left), and where the gas number density K 7 5 10 (right). Moreover, the blue contours mark the 3 − , and after the explosion, which corresponds to the number 6 cm 10 3 , ) can not break the sphericity of the supernova remnant. 5 10 1 10 kyr − = 10 , and T 2 10 km s 10 ∼ , after the supernova explosion. The supernova shock wave has largely 1 10 , 0 . 200 kyr = 1 n Fig.2a shows the remnant Several black (left) and white (right) contours highlight the regions in the remnant In Fig.2b the shock wave has expanded in the low-density cavity of stellar wind, while it The last panel of the gure (Fig.2d) highlights the supernova remnant at even much Our simulations demonstrate that a very massive star of initial mass regions in the remnant where the ejecta contributes where the temperature is has much less progressed in thewith direction the of regions stellar of motion shocked because ISMTaylor gas. of instabilities its at Notably, ongoing both the interaction fronts ejecta-wind seethe and the progression development ejecta-ISM of interfaces. mechanism Rayleight- of Atof later the times, stellar supernova in blastwave wind Fig.2c, keeps andSimilarly, going, shocked the as generation ISM well of materials asmore instabitilies the taking pronounced, at mixing place and, the in a forward theat small shock the region surrounding of apex of of environment. of hot the the mixted shock still ISM, wave runaway stellar is supernova wind even remnant. later and times, ISM gas forms expanded and its forward shockwhile has structure reached is the therefore bottomand lled of shocked with ISM the a material. cavity mixture of Theshock of stellar ecient wave along supernova deceleration wind. the ejecta, of direction The the shocked of forwardwith stellar stellar shock the motion wind of unperturbed makes the the ambient supernova part mediumin of almost it size. static which Only directly and interacts a thethe thin, remnant does elongated mixing region not processes, grow of and much thethe remain interior geometry of made the of of supernova the supernovathese remnant ejecta escape question. calculations, exclusively. from and This further may 3D rely MHD of models are4. necessary to Conclusion address Supernova remnants of very massive stars density eld in Fig.1c.with The the shocked mixing ISM of gas,colored main-sequence aects particle and the tracer evolved entire stellar interior elds).less of winds, aected the Note together by pre-supernova that this wind the mixing bubbleThe of central (see blue gases, region contours which of highlight might the thesynthetised rely young in on wind region the the bubble made 2D core is of nature of slightly supernova of the ejecta the stellar such simulations. progenitor as prior the to metals the supernova explosion. mously impact its surroundings,regarding with to or without its being localstar, animated ambient undergoing by medium. both a The several stellarcircumstellar Luminous-Blue-Variable peculiar bulk shells and motion evolution resulting Wolf-Rayet of episodes in prokoving our [16],their and/or considered eject circumstellar emphasizing massive the medium asymmetric at characterif the of the pre-supernova time. star is Thea suciently outows path they close for produce to theslowly-moving might, the subsequent stars shock shell ( wave of of their the wind defunct bubble, progenitor pierce star. it Inversely, and static thus or open with is PoS(ICRC2021)983 and displayed at D. M.-A. Meyer 1 − 20 km s 6 star moving with velocity

60 M Supernova remnant of a contribution of ejecta material in number density. 10% Figure 2: several characteristic times of itsmaterial, evolution. right-hand part Left-hand is part thecontours of proportion are each the of gure temperature stellar is wind elda the gas and proportion in white of contours the ISM are computational number domain. density. Black Blue contours highlight Supernova remnants of very massive stars PoS(ICRC2021)983 ), since they D. M.-A. Meyer 1 Myr . 0 7 ApJ, 649, 779-787 229-238 Meyer D. M.-A., Kami«ski, T., 2014, Mnras, 437, 843-856 L10 Schneiter E., 2011, ApJ, 727, 32 The authors acknowledge the North-German Supercomputing Alliance (HLRN) for [1] Weaver R., McCray R., Castor J.,[2] Shapiro P.,Freyer, Moore Tim R., and 1977, Hensler, ApJ, Gerhard 218 and[3] Yorke, HaroldGies, W., D. 2003, R., ApJ, 1987, 594 ApJs, 64,[4] 545-563 Gvaramadze, V. V., Menten K. M., Kniazev A. Y.,[5] Langer N.,Mackey J., Mackey Mohamed J., S., Kraus Neilson A., H. R., Langer N., Meyer[6] D. M.-A.,Franco J., 2012, Tenorio-Tagle ApjL, G., 751, Bodenheimer P., Rozyczka[7] M., 1991,Fang Jun, PASP, 103, Yu 803-810 Huan, Zhang Li,[8] 2017, MNRAS,Vigh 464, C. 940-945 D., Velázquez P. F., Gómez[9] D.Chiotellis A., O., Schure Reynoso K. M., E. Vink M., J., 2012, Esquivel A&A, A., 537, A139 Matias Supernova remnants of very massive stars The expanding supernova blastwaveinside remains of the trapped layer of andmassive shocked experiences moving stellar star wind. several is Our reections able simulationsa to demonstrate region that modify of a the the unique entireof ISM. very gas the These dynamical results surroundings and stress of chemical the properties middle-age need of to for old investigating supernova the remnants chemical (up evolution to [10] Velázquez P. F., Vigh C. D., Reynoso E.[11] M.,Toledo-Roy Gómez J. D. C., O., Esquivel A., Schneiter Velázquez E. P. M., F., 2006, Reynoso E. M., 2014, MNRAS, 442, 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 still bear the traceshould of be the potential further runaway explored nature3D over of magneto-hydrodynamical a the simulations. wider dead parameter progenitors. space, for This problem example by meansAcknowledgement of global, PoS(ICRC2021)983 D. M.-A. Meyer 8 450 ApJs&A, 198 A., 2007, ApJ, 170 [20] Meyer D. M. -A., Pohl M., Petrov M., Oskinova L. M., 2021, MNRAS 502, 4 [15] Vaidya B., Mignone A., Bodo G.,[16] RossiGroh P., Massaglia J. S., H., 2018, Meynet ApJ, G., 865, Ekström[17] 144 S.,Comerón Georgy F., C., Kaper 2014, L., A&A, 1998, 564, A&A,[18] A30 338 Meyer D. M.-A., van Marle A.-J.,[19] KuiperMeyer R., D. Kley M.-A., W., Langer 2016, MNRAS, N., 459 Mackey J., Velázquez P. F., Gusdorf A., 2015, MNRAS, [14] Mignone A., Zanni C., Tzeferacos P., van Straalen B., Colella P., Bodo G., 2012, Supernova remnants of very massive stars [12] van Marle A. J., Meliani Z.,[13] KeppensMignone R., A., Decin Bodo L., G., 2011, Massaglia ApJ S., Letters, Matsakos L26 T., Tesileanu O., Zanni, C. and Ferrari,