Zobrazeno 1 - 10
of 2 038
pro vyhledávání: '"SCHNEIDER, P. R."'
One-dimensional (1D) methods for simulating the common-envelope (CE) phase offer advantages over three-dimensional (3D) simulations regarding their computational speed and feasibility. We present the 1D CE method from Bronner et al. (2024), including
Externí odkaz:
http://arxiv.org/abs/2412.04543
Autor:
Vetter, M., Roepke, F. K., Schneider, F. R. N., Pakmor, R., Ohlmann, S. T., Lau, M. Y. M., Andrassy, R.
Three-dimensional simulations usually fail to cover the entire dynamical common-envelope phase of gravitational wave progenitor systems due to the vast range of spatial and temporal scales involved. We investigated the common-envelope interactions of
Externí odkaz:
http://arxiv.org/abs/2410.07841
In the age of gravitational-wave (GW) sources and newly discovered local black holes (BH) and neutron stars (NS), understanding the fate of stars is a key question. Not every massive star is expected to successfully explode as a supernova and leave b
Externí odkaz:
http://arxiv.org/abs/2409.02058
Autor:
Shenar, T., Bodensteiner, J., Sana, H., Crowther, P. A., Lennon, D. J., Abdul-Masih, M., Almeida, L. A., Backs, F., Berlanas, S. R., Bernini-Peron, M., Bestenlehner, J. M., Bowman, D. M., Bronner, V. A., Britavskiy, N., de Koter, A., de Mink, S. E., Deshmukh, K., Evans, C. J., Fabry, M., Gieles, M., Gilkis, A., González-Torà, G., Gräfener, G., Götberg, Y., Hawcroft, C., Hénault-Brunet, V., Herrero, A., Holgado, G., Janssens, S., Johnston, C., Josiek, J., Justham, S., Kalari, V. M., Katabi, Z. Z., Keszthelyi, Z., Klencki, J., Kubát, J., Kubátová, B., Langer, N., Lefever, R. R., Ludwig, B., Mackey, J., Mahy, L., Apellániz, J. Maíz, Mandel, I., Maravelias, G., Marchant, P., Menon, A., Najarro, F., Oskinova, L. M., Ovadia, A. J. G. O'Grady R., Patrick, L. R., Pauli, D., Pawlak, M., Ramachandran, V., Renzo, M., Rocha, D. F., Sander, A. A. C., Sayada, T., Schneider, F. R. N., Schootemeijer, A., Schösser, E. C., Schürmann, C., Sen, K., Shahaf, S., Simón-Díaz, S., Stoop, M., van Loon, J. Th., Toonen, S., Tramper, F., Valli, R., van Son, L. A. C., Vigna-Gómez, A., Villaseñor, J. I., Vink, J. S., Wang, C., Willcox, R.
Publikováno v:
A&A 690, A289 (2024)
Surveys in the Milky Way and Large Magellanic Cloud revealed that the majority of massive stars will interact with companions during their lives. However, knowledge of the binary properties of massive stars at low metallicity, which approaches the co
Externí odkaz:
http://arxiv.org/abs/2407.14593
Autor:
Pakmor, Rüdiger, Pelisoli, Ingrid, Justham, Stephen, Rajamuthukumar, Abinaya S., Röpke, Friedrich K., Schneider, Fabian R. N., de Mink, Selma E., Ohlmann, Sebastian T., Podsiadlowski, Philipp, Fraile, Javier Moran, Vetter, Marco, Andrassy, Robert
Publikováno v:
A&A 691, A179 (2024)
Stellar mergers are one important path to highly magnetised stars. Mergers of two low-mass white dwarfs may create up to every third hot subdwarf star. The merging process is usually assumed to dramatically amplify magnetic fields. However, so far on
Externí odkaz:
http://arxiv.org/abs/2407.02566
Products of stellar mergers are predicted to be common in stellar populations and can potentially explain stars with peculiar properties. When the merger occurs after the initially more massive star has evolved into the Hertzsprung gap (HG), the merg
Externí odkaz:
http://arxiv.org/abs/2406.14416
Autor:
Kozyreva, Alexandra, Shingles, Luke, Baklanov, Petr, Mironov, Alexey, Schneider, Fabian R. N.
Publikováno v:
A&A 689, A60 (2024)
We examine the pair-instability origin of superluminous supernova 2018ibb. As the base model, we use a non-rotating stellar model with an initial mass of 250 Msun at about 1/15 solar metallicity. We consider three versions of the model as input for r
Externí odkaz:
http://arxiv.org/abs/2405.20009
Autor:
Frost, A. J., Sana, H., Mahy, L., Wade, G., Barron, J., Bouquin, J. -B. Le, Mérand, A., Schneider, F. R. N., Shenar, T., Barbá, R. H., Bowman, D. M., Fabry, M., Farhang, A., Marchant, P., Morrell, N. I., Smoker, J. V.
Publikováno v:
Science, 11 Apr 2024, Vol 384, Issue 6692, pp. 214-217
Massive stars (those larger than 8 solar masses at formation) have radiative envelopes that cannot sustain a dynamo, the mechanism that produces magnetic fields in lower-mass stars. Despite this, approximately 7\% of massive stars have observed magne
Externí odkaz:
http://arxiv.org/abs/2404.10167
Publikováno v:
A&A 686, A45 (2024)
The majority of massive stars are expected to exchange mass or merge with a companion during their lives. This immediately implies that most supernovae (SNe) are from such post-mass-exchange objects. Here, we explore how mass accretion and merging af
Externí odkaz:
http://arxiv.org/abs/2403.03984
Stellar mergers lead to diverse phenomena: rejuvenated blue stragglers, magnetised and peculiar stars, transients and nebulae. Using a grid of about 6000 detailed 1D binary evolution models (initial component masses of 0.5-20$\,\text{M}_{\odot}$ at s
Externí odkaz:
http://arxiv.org/abs/2311.12124