X-Shooting ULLYSES: Massive stars at low metallicity: VIII. Stellar and wind parameters of newly revealed stripped stars in Be binaries

被引：0
作者：
Ramachandran, V. [1 ]
Sander, A.A.C. [1 ]
Pauli, D. [2 ]
Klencki, J. [3 ]
Backs, F. [4 ]
Tramper, F. [5 ]
Bernini-Peron, M. [1 ]
Crowther, P. [6 ]
Hamann, W.-R. [2 ]
Ignace, R. [7 ]
Kuiper, R. [8 ]
Oey, M.S. [9 ]
Oskinova, L.M. [2 ]
Shenar, T. [10 ]
Todt, H. [2 ]
Vink, J.S. [11 ]
Wang, L. [12 ]
Wofford, A. [13 ]
机构：
[1] Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12-14, Heidelberg
[2] Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. 24/25, Potsdam
[3] European Southern Observatory, Karl-Schwarzschild-Strasse 2, Garching bei München
[4] Anton Pannekoek Institute for Astronomy, Universiteit van Amsterdam, Science Park 904, Amsterdam
[5] Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, Leuven
[6] Dept of Physics & Astronomy, University of Sheffield, Hounsfield Road, Sheffield
[7] Department of Physics & Astronomy, East Tennessee State University, Johnson City, 37614, TN
[8] Fakultät für Physik, Universität Duisburg-Essen, Lotharstraße 1, Duisburg
[9] University of Michigan, Department of Astronomy, 323 West Hall, Ann Arbor, 48109, MI
[10] The School of Physics and Astronomy, Tel Aviv University, Tel Aviv
[11] Armagh Observatory and Planetarium, College Hill, Northern Ireland, Armagh
[12] Yunnan Observatories, Chinese Academy of Sciences, Yunnan, Kunming
[13] Instituto de Astronomía, Universidad Nacional Autónoma de México, Unidad Académica en Ensenada, Km 103 Carr. TijuanaEnsenada, B.C., Ensenada
来源：
Astronomy and Astrophysics | 2024年 / 692卷
基金：
英国科学技术设施理事会;
关键词：
Be; Binaries: spectroscopic; Stars: early-type; Stars: emission-line; Stars: evolution; Stars: fundamental parameters; Stars: mass-loss;
D O I：
10.1051/0004-6361/202449665
中图分类号：
学科分类号：
摘要：
On the route toward merging neutron stars and stripped-envelope supernovae, binary population synthesis predicts a large number of post-interaction systems with massive stars that have been stripped of their outer layers. However, observations of such stars in the intermediate-mass regime below the Wolf-Rayet masses are rare. Using X-Shooting ULLYSES (XShootU) data, we have discovered three partially stripped star + Be/Oe binaries in the Magellanic Clouds. We analyzed the UV and optical spectra using the Potsdam Wolf-Rayet (PoWR) model atmosphere code by superimposing model spectra that correspond to each component. The estimated current masses of the partially stripped stars fall within the intermediate-mass range of ≈ 4-8 M⊙. These objects are found to be over-luminous for their corresponding stellar masses, which aligns with the luminosities during core He-burning. Their accompanying Be/Oe secondaries are found to have much higher masses than their stripped primaries (mass ratio ≳2). The surfaces of all three partially stripped stars exhibit clear indications of significant nitrogen enrichment as well as a depletion of carbon and oxygen. Furthermore, one of our sample stars shows signs of substantial helium enrichment. Our study provides the first comprehensive determination of the wind parameters of partially stripped stars in the intermediate-mass range. The wind mass-loss rates of these stars are estimated to be on the order of 10-7 M⊙ yr-1, which is more than ten times higher than that of OB stars with the same luminosity. The current mass-loss recipes commonly employed in evolutionary models to characterize this phase are based on OB or WR mass-loss rates, and they significantly underestimate or overestimate the observed mass-loss rates of (partially) stripped stars by an order of magnitude. Binary evolution models suggest that the observed primaries had initial masses in the range of 12-17 M⊙, and are potential candidates for stripped-envelope supernovae resulting in the formation of a neutron star. If these systems survive the explosion, they will likely evolve to become Be X-ray binaries and later double neutron stars. © The Authors 2024.
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