TY - JOUR A1 - Meyer, Dominique M.-A. A1 - Velazquez, Pablo F. A1 - Petruk, Oleh A1 - Chiotellis, Alexandros A1 - Pohl, Martin A1 - Camps-Farina, Artemi A1 - Petrov, Miroslav A1 - Reynoso, Estela M. A1 - Toledo-Roy, Juan C. A1 - Schneiter, E. Matias A1 - Castellanos-Ramirez, Antonio A1 - Esquivel, Alejandro T1 - Rectangular core-collapse supernova remnants BT - application to Puppis A JF - Monthly notices of the Royal Astronomical Society N2 - Core-collapse supernova remnants are the gaseous nebulae of galactic interstellar media (ISM) formed after the explosive death of massive stars. Their morphology and emission properties depend both on the surrounding circumstellar structure shaped by the stellar wind-ISM interaction of the progenitor star and on the local conditions of the ambient medium. In the warm phase of the Galactic plane (n approximate to 1 cm(-3), T approximate to 8000 K), an organized magnetic field of strength 7 mu G has profound consequences on the morphology of the wind bubble of massive stars at rest. In this paper, we show through 2.5D magnetohydrodynamical simulations, in the context of a Wolf-Rayet-evolving 35 M 0 star, that it affects the development of its supernova remnant. When the supernova remnant reaches its middle age (15-20 kyr), it adopts a tubular shape that results from the interaction between the isotropic supernova ejecta and the anisotropic, magnetized, shocked stellar progenitor bubble into which the supernova blast wave expands. Our calculations for non-thermal emission, i.e. radio synchrotron and inverse-Compton radiation, reveal that such supernova remnants can, due to projection effects, appear as rectangular objects in certain cases. This mechanism for shaping a supernova remnant is similar to the bipolar and elliptical planetary nebula production by wind-wind interaction in the low-mass regime of stellar evolution. If such a rectangular core-collapse supernova remnant is created, the progenitor star must not have been a runaway star. We propose that such a mechanism is at work in the shaping of the asymmetric core-collapse supernova remnant Puppis A. KW - stars: evolution KW - stars: massive KW - ISM: supernova remnants KW - methods: MHD Y1 - 2022 U6 - https://doi.org/10.1093/mnras/stac1832 SN - 0035-8711 SN - 1365-2966 VL - 515 IS - 1 SP - 594 EP - 605 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Aguilera-Dena, David R. A1 - Langer, Norbert A1 - Antoniadis, John A1 - Pauli, Daniel A1 - Dessart, Luc A1 - Vigna-Gómez, Alejandro A1 - Gräfener, Götz A1 - Yoon, Sung-Chul T1 - Stripped-envelope stars in different metallicity environments: I. Evolutionary phases, classification, and populations JF - Astronomy and astrophysics N2 - Massive stars that become stripped of their hydrogen envelope through binary interaction or winds can be observed either as Wolf-Rayet stars, if they have optically thick winds, or as transparent-wind stripped-envelope stars. We approximate their evolution through evolutionary models of single helium stars, and compute detailed model grids in the initial mass range 1.5-70 M. for metallicities between 0.01 and 0.04, from core helium ignition until core collapse. Throughout their lifetimes some stellar models expose the ash of helium burning. We propose that models that have nitrogen-rich envelopes are candidate WN stars, while models with a carbon-rich surface are candidate WC stars during core helium burning, and WO stars afterwards. We measure the metallicity dependence of the total lifetimes of our models and the duration of their evolutionary phases. We propose an analytic estimate of the wind's optical depth to distinguish models of Wolf-Rayet stars from transparent-wind stripped-envelope stars, and find that the luminosity ranges at which WN-, WC-, and WO-type stars can exist is a strong function of metallicity. We find that all carbon-rich models produced in our grids have optically thick winds and match the luminosity distribution of observed populations. We construct population models and predict the numbers of transparent-wind stripped-envelope stars and Wolf-Rayet stars, and derive their number ratios at different metallicities. We find that as metallicity increases, the number of transparent-wind stripped-envelope stars decreases and the number of Wolf-Rayet stars increases. At high metallicities WC- and WO-type stars become more common. We apply our population models to nearby galaxies, and find that populations are more sensitive to the transition luminosity between Wolf-Rayet stars and transparent-wind helium stars than to the metallicity-dependent mass loss rates. KW - stars: massive KW - stars: Wolf-Rayet KW - stars: winds, outflows KW - binaries: general KW - supernovae: general Y1 - 2022 U6 - https://doi.org/10.1051/0004-6361/202142895 SN - 0004-6361 SN - 1432-0746 VL - 661 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Bozzo, Enrico A1 - Romano, Patrizia A1 - Ferrigno, Carlo A1 - Oskinova, Lida T1 - The symbiotic X-ray binaries Sct X-1, 4U 1700+24, and IGR J17329-2731 JF - Monthly notices of the Royal Astronomical Society N2 - Symbiotic X-ray binaries are systems hosting a neutron star accreting form the wind of a late-type companion. These are rare objects and so far only a handful of them are known. One of the most puzzling aspects of the symbiotic X-ray binaries is the possibility that they contain strongly magnetized neutron stars. These are expected to be evolutionary much younger compared to their evolved companions and could thus be formed through the (yet poorly known) accretion induced collapse of a white dwarf. In this paper, we perform a broad-band X-ray and soft gamma-ray spectroscopy of two known symbiotic binaries, Sct X-1 and 4U 1700+24, looking for the presence of cyclotron scattering features that could confirm the presence of strongly magnetized NSs. We exploited available Chandra, Swift, and NuSTAR data. We find no evidence of cyclotron resonant scattering features (CRSFs) in the case of Sct X-1 but in the case of 4U 1700+24 we suggest the presence of a possible CRSF at similar to 16 keV and its first harmonic at similar to 31 keV, although we could not exclude alternative spectral models for the broad-band fit. If confirmed by future observations, 4U 1700+24 could be the second symbiotic X-ray binary with a highly magnetized accretor. We also report about our long-term monitoring of the last discovered symbiotic X-ray binary IGR J17329-2731 performed with Swift/XRT. The monitoring revealed that, as predicted, in 2017 this object became a persistent and variable source, showing X-ray flares lasting for a few days and intriguing obscuration events that are interpreted in the context of clumpy wind accretion. KW - accretion KW - accretion discs KW - stars: massive KW - stars: neutron KW - X-rays: binaries KW - X-rays: individual: SctX-1 KW - X-rays: individual: 4U1700+24; KW - X-rays: stars KW - X-rays: individual: IGRJ17329-2731 Y1 - 2022 U6 - https://doi.org/10.1093/mnras/stac907 SN - 0035-8711 SN - 1365-2966 VL - 513 IS - 1 SP - 42 EP - 54 PB - Oxford University Press CY - Oxford ER -