Eva Laplace

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About Eva Laplace:

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SEEK ID: https://publications.h-its.org/people/181

Location: Germany

ORCID: https://orcid.org/0000-0003-1009-5691

Joined: 20th Dec 2022

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Stellar Evolution Theory

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Start date: 1st Jan 2021

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Heidelberg Institute for Theoretical Studies

Country: Germany

City: Heidelberg

Web page: https://www.h-its.org

Showing 5 out of a possible 12 Publications Advanced Publications list for this Person with search and filtering

Finding the Fuse: Prospects for the Detection and Characterization of Hydrogen-rich Core-collapse Supernova Precursor Emission with the LSST

Stellar Evolution Theory

Abstract (Expand)

Abstract Enhanced emission in the months to years preceding explosion has been detected for several core-collapse supernovae (SNe). Though the physical mechanisms driving the emission remain hotly …

Authors: A. Gagliano, E. Berger, V. A. Villar, D. Hiramatsu, R. Kessler, T. Matsumoto, A. Gilkis, E. Laplace

Date Published: 30th Dec 2024

Publication Type: Journal

DOI: 10.3847/1538-4357/ad9748

Citation: ApJ 978(1):110

Created: 31st Jan 2025 at 14:07, Last updated: 31st Jan 2025 at 14:07

Stripped Helium Star and Compact Object Binaries in Coeval Populations: Predictions Based on Detailed Binary Evolution Models

Stellar Evolution Theory

Abstract (Expand)

Abstract Massive stars mainly form in close binaries, where their mutual interactions can profoundly alter their evolutionary paths. Evolved binaries consisting of a massive OB-type main-sequence star …

Authors: Chen Wang, Julia Bodensteiner, Xiao-Tian Xu, Selma E. de Mink, Norbert Langer, Eva Laplace, Alejandro Vigna-Gómez, Stephen Justham, Jakub Klencki, Aleksandra Olejak, Ruggero Valli, Abel Schootemeijer

Date Published: 30th Oct 2024

Publication Type: Journal

DOI: 10.3847/2041-8213/ad86b7

Citation: ApJL 975(1):L20

Created: 31st Jan 2025 at 14:08, Last updated: 31st Jan 2025 at 14:08

Evolution and final fate of massive post-common-envelope binaries

Stellar Evolution Theory

Abstract

Not specified

Authors: Dandan Wei, Fabian R. N. Schneider, Philipp Podsiadlowski, Eva Laplace, Friedrich K. Röpke, Marco Vetter

Date Published: 1st Aug 2024

Publication Type: Journal

DOI: 10.1051/0004-6361/202348560

Citation: A&A 688:A87

Created: 21st Jan 2025 at 20:40

Contact tracing of binary stars: Pathways to stellar mergers

Stellar Evolution Theory

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Abstract (Expand)

Stellar mergers are responsible for a wide variety of phenomena such as rejuvenated blue stragglers, highly magnetised stars, spectacular transients, iconic nebulae, and stars with peculiar surface … chemical abundances and rotation rates. Before stars merge, they enter a contact phase. Here, we investigate which initial binary-star configurations lead to contact and classical common-envelope (CE) phases and assess the likelihood of a subsequent merger. To this end, we computed a grid of about 6000 detailed 1D binary evolution models with initial component masses of 0.5 − 20.0 M⊙ at solar metallicity. Both components were evolved, and rotation and tides were taken into account. We identified five mechanisms that lead to contact and mergers: runaway mass transfer, mass loss through the outer Lagrange point L2, expansion of the accretor, orbital decay because of tides, and non-conservative mass transfer. At least 40% of mass-transferring binaries with initial primary-star masses of 5 − 20 M⊙ evolve into a contact phase; > 12% and > 19% likely merge and evolve into a CE phase, respectively. Because of the non-conservative mass transfer in our models, classical CE evolution from late Case-B and Case-C binaries is only found for initial mass ratios qi < 0.15 − 0.35. For larger mass ratios, we find stable mass transfer. In early Case-B binaries, contact occurs for initial mass ratios qi < 0.15 − 0.35, while in Case-A mass transfer, this is the case for all qi in binaries with the initially closest orbits and qi < 0.35 for initially wider binaries. Our models predict that most Case-A binaries with mass ratios of q < 0.5 upon contact mainly get into contact because of runaway mass transfer and accretor expansion on a thermal timescale, with subsequent L2-overflow in more than half of the cases. Thus, these binaries likely merge quickly after establishing contact or remain in contact only for a thermal timescale. On the contrary, Case-A contact binaries with higher mass ratios form through accretor expansion on a nuclear timescale and can thus give rise to long-lived contact phases before a possible merger. Observationally, massive contact binaries are almost exclusively found with mass ratios q > 0.5, confirming our model expectations. Because of non-conservative mass transfer with mass transfer efficiencies of 15 − 65%, 5 − 25%, and 25 − 50% in Case-A, -B, and -C mass transfer, respectively (for primary-star masses above 3 M⊙), our contact, merger, and classical CE incidence rates are conservative lower limits. With more conservative mass transfer, these incidences would increase. Moreover, in most binaries, the non-accreted mass cannot be ejected, raising the question of the further evolution of such systems. The non-accreted mass may settle into circumstellar and circumbinary disks, but could also lead to further contact systems and mergers. Overall, contact binaries are a frequent and fascinating result of binary mass transfer of which the exact outcomes still remain to be understood and explored further.

Authors: J. Henneco, F. R. N. Schneider, E. Laplace

Date Published: 1st Feb 2024

Publication Type: Journal

DOI: 10.1051/0004-6361/202347893

Citation: A&A 682:A169

Created: 5th Mar 2024 at 15:53, Last updated: 5th Mar 2024 at 21:25

X-Shooting ULLYSES: Massive stars at low metallicity. I. Project description

Stellar Evolution Theory

Abstract (Expand)

Observations of individual massive stars, super-luminous supernovae, gamma-ray bursts, and gravitational wave events involving spectacular black hole mergers indicate that the low-metallicity Universe …

Authors: Jorick S. Vink, A. Mehner, P. A. Crowther, A. Fullerton, M. Garcia, F. Martins, N. Morrell, L. M. Oskinova, N. St-Louis, A. ud-Doula, A. A. C. Sander, H. Sana, J. -C. Bouret, B. Kubátová, P. Marchant, L. P. Martins, A. Wofford, J. Th. van Loon, O. Grace Telford, Y. Götberg, D. M. Bowman, C. Erba, V. M. Kalari, M. Abdul-Masih, T. Alkousa, F. Backs, C. L. Barbosa, S. R. Berlanas, M. Bernini-Peron, J. M. Bestenlehner, R. Blomme, J. Bodensteiner, S. A. Brands, C. J. Evans, A. David-Uraz, F. A. Driessen, K. Dsilva, S. Geen, V. M. A. Gómez-González, L. Grassitelli, W. -R. Hamann, C. Hawcroft, A. Herrero, E. R. Higgins, D. John Hillier, R. Ignace, A. G. Istrate, L. Kaper, N. D. Kee, C. Kehrig, Z. Keszthelyi, J. Klencki, A. de Koter, R. Kuiper, E. Laplace, C. J. K. Larkin, R. R. Lefever, C. Leitherer, D. J. Lennon, L. Mahy, J. Maíz Apellániz, G. Maravelias, W. Marcolino, A. F. McLeod, S. E. de Mink, F. Najarro, M. S. Oey, T. N. Parsons, D. Pauli, M. G. Pedersen, R. K. Prinja, V. Ramachandran, M. C. Ramírez-Tannus, G. N. Sabhahit, A. Schootemeijer, S. Reyero Serantes, T. Shenar, G. S. Stringfellow, N. Sudnik, F. Tramper, L. Wang

Date Published: 1st Jul 2023

Publication Type: Journal

DOI: 10.1051/0004-6361/202245650

Citation: A&A 675:A154

Created: 15th Jan 2024 at 11:09, Last updated: 5th Mar 2024 at 21:25

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