[{"_id":"13457","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","type":"journal_article","article_type":"original","extern":"1","date_updated":"2023-08-21T11:49:36Z","oa_version":"Published Version","abstract":[{"lang":"eng","text":"Context. Observations of massive stars in open clusters younger than ∼8 Myr have shown that a majority of them are in binary systems, most of which will interact during their life. While these can be used as a proxy of the initial multiplicity properties, studying populations of massive stars older than ∼20 Myr allows us to probe the outcome of these interactions after a significant number of systems have experienced mass and angular momentum transfer and may even have merged.\r\n\r\nAims. Using multi-epoch integral-field spectroscopy, we aim to investigate the multiplicity properties of the massive-star population in the dense core of the ∼40 Myr old cluster NGC 330 in the Small Magellanic Cloud in order to search for possible imprints of stellar evolution on the multiplicity properties.\r\n\r\nMethods. We obtained six epochs of VLT/MUSE observations operated in wide-field mode with the extended wavelength setup and supported by adaptive optics. We extracted spectra and measured radial velocities for stars brighter than mF814W = 19. We identified single-lined spectroscopic binaries through significant RV variability with a peak-to-peak amplitude larger than 20 km s−1. We also identified double-lined spectroscopic binaries, and quantified the observational biases for binary detection. In particular, we took into account that binary systems with similar line strengths are difficult to detect in our data set.\r\n\r\nResults. The observed spectroscopic binary fraction among stars brighter than mF814W = 19 (approximately 5.5 M⊙ on the main sequence) is fSBobs = 13.2 ± 2.0%. Considering period and mass ratio ranges from log(P) = 0.15−3.5 (about 1.4 to 3160 d), q = 0.1−1.0, and a representative set of orbital parameter distributions, we find a bias-corrected close binary fraction of fcl = 34−7+8%. This fraction seems to decline for the fainter stars, which indicates either that the close binary fraction drops in the B-type domain, or that the period distribution becomes more heavily weighted toward longer orbital periods. We further find that both fractions vary strongly in different regions of the color-magnitude diagram, which corresponds to different evolutionary stages. This probably reveals the imprint of the binary history of different groups of stars. In particular, we find that the observed spectroscopic binary fraction of Be stars (fSBobs = 2 ± 2%) is significantly lower than that of B-type stars (fSBobs = 9 ± 2%).\r\n\r\nConclusions. We provide the first homogeneous radial velocity study of a large sample of B-type stars at a low metallicity ([Fe/H] ≲ −1.0). The overall bias-corrected close binary fraction (log(P) < 3.5 d) of the B-star population in NGC 330 is lower than the fraction reported for younger Galactic and Large Magellanic Cloud clusters in previous works. More data are needed, however, to establish whether the observed differences are caused by an age or a metallicity effect."}],"intvolume":" 652","month":"08","main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/202140507","open_access":"1"}],"scopus_import":"1","language":[{"iso":"eng"}],"publication_status":"published","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"volume":652,"article_number":"A70","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"short":"J. Bodensteiner, H. Sana, C. Wang, N. Langer, L. Mahy, G. Banyard, A. de Koter, S.E. de Mink, C.J. Evans, Y.L.L. Götberg, L.R. Patrick, F.R.N. Schneider, F. Tramper, Astronomy & Astrophysics 652 (2021).","ieee":"J. Bodensteiner et al., “The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population,” Astronomy & Astrophysics, vol. 652. EDP Sciences, 2021.","apa":"Bodensteiner, J., Sana, H., Wang, C., Langer, N., Mahy, L., Banyard, G., … Tramper, F. (2021). The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202140507","ama":"Bodensteiner J, Sana H, Wang C, et al. The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population. Astronomy & Astrophysics. 2021;652. doi:10.1051/0004-6361/202140507","mla":"Bodensteiner, J., et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE. II. Multiplicity Properties of the Massive-Star Population.” Astronomy & Astrophysics, vol. 652, A70, EDP Sciences, 2021, doi:10.1051/0004-6361/202140507.","ista":"Bodensteiner J, Sana H, Wang C, Langer N, Mahy L, Banyard G, de Koter A, de Mink SE, Evans CJ, Götberg YLL, Patrick LR, Schneider FRN, Tramper F. 2021. The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population. Astronomy & Astrophysics. 652, A70.","chicago":"Bodensteiner, J., H. Sana, C. Wang, N. Langer, L. Mahy, G. Banyard, A. de Koter, et al. “The Young Massive SMC Cluster NGC 330 Seen by MUSE. II. Multiplicity Properties of the Massive-Star Population.” Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202140507."},"title":"The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population","article_processing_charge":"No","external_id":{"arxiv":["2104.13409"]},"author":[{"first_name":"J.","full_name":"Bodensteiner, J.","last_name":"Bodensteiner"},{"first_name":"H.","last_name":"Sana","full_name":"Sana, H."},{"last_name":"Wang","full_name":"Wang, C.","first_name":"C."},{"first_name":"N.","full_name":"Langer, N.","last_name":"Langer"},{"full_name":"Mahy, L.","last_name":"Mahy","first_name":"L."},{"last_name":"Banyard","full_name":"Banyard, G.","first_name":"G."},{"first_name":"A.","full_name":"de Koter, A.","last_name":"de Koter"},{"first_name":"S. E.","last_name":"de Mink","full_name":"de Mink, S. E."},{"full_name":"Evans, C. J.","last_name":"Evans","first_name":"C. J."},{"first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911"},{"last_name":"Patrick","full_name":"Patrick, L. R.","first_name":"L. R."},{"last_name":"Schneider","full_name":"Schneider, F. R. N.","first_name":"F. R. N."},{"full_name":"Tramper, F.","last_name":"Tramper","first_name":"F."}],"oa":1,"publisher":"EDP Sciences","quality_controlled":"1","publication":"Astronomy & Astrophysics","day":"12","year":"2021","date_created":"2023-08-03T10:11:34Z","doi":"10.1051/0004-6361/202140507","date_published":"2021-08-12T00:00:00Z"},{"date_updated":"2023-08-21T11:49:15Z","article_type":"original","type":"journal_article","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"_id":"13455","volume":656,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"publication_status":"published","language":[{"iso":"eng"}],"scopus_import":"1","main_file_link":[{"url":"https://doi.org/10.1051/0004-6361/202140506","open_access":"1"}],"month":"12","intvolume":" 656","abstract":[{"lang":"eng","text":"The majority of massive stars live in binary or multiple systems and will interact with a companion during their lifetimes, which helps to explain the observed diversity of core-collapse supernovae. Donor stars in binary systems can lose most of their hydrogen-rich envelopes through mass transfer. As a result, not only are the surface properties affected, but so is the core structure. However, most calculations of the core-collapse properties of massive stars rely on single-star models. We present a systematic study of the difference between the pre-supernova structures of single stars and stars of the same initial mass (11–21 M⊙) that have been stripped due to stable post-main-sequence mass transfer at solar metallicity. We present the pre-supernova core composition with novel diagrams that give an intuitive representation of the isotope distribution. As shown in previous studies, at the edge of the carbon-oxygen core, the binary-stripped star models contain an extended gradient of carbon, oxygen, and neon. This layer remains until core collapse and is more extended in mass for higher initial stellar masses. It originates from the receding of the convective helium core during core helium burning in binary-stripped stars, which does not occur in single-star models. We find that this same evolutionary phase leads to systematic differences in the final density and nuclear energy generation profiles. Binary-stripped star models have systematically higher total masses of carbon at the moment of core collapse compared to single-star models, which likely results in systematically different supernova yields. In about half of our models, the silicon-burning and oxygen-rich layers merge after core silicon burning. We discuss the implications of our findings for the “explodability”, supernova observations, and nucleosynthesis of these stars. Our models are publicly available and can be readily used as input for detailed supernova simulations."}],"oa_version":"Published Version","author":[{"last_name":"Laplace","full_name":"Laplace, E.","first_name":"E."},{"first_name":"S.","full_name":"Justham, S.","last_name":"Justham"},{"full_name":"Renzo, M.","last_name":"Renzo","first_name":"M."},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter","last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911"},{"full_name":"Farmer, R.","last_name":"Farmer","first_name":"R."},{"full_name":"Vartanyan, D.","last_name":"Vartanyan","first_name":"D."},{"last_name":"de Mink","full_name":"de Mink, S. E.","first_name":"S. E."}],"external_id":{"arxiv":["2102.05036"]},"article_processing_charge":"No","title":"Different to the core: The pre-supernova structures of massive single and binary-stripped stars","citation":{"mla":"Laplace, E., et al. “Different to the Core: The Pre-Supernova Structures of Massive Single and Binary-Stripped Stars.” Astronomy & Astrophysics, vol. 656, A58, EDP Sciences, 2021, doi:10.1051/0004-6361/202140506.","ama":"Laplace E, Justham S, Renzo M, et al. Different to the core: The pre-supernova structures of massive single and binary-stripped stars. Astronomy & Astrophysics. 2021;656. doi:10.1051/0004-6361/202140506","apa":"Laplace, E., Justham, S., Renzo, M., Götberg, Y. L. L., Farmer, R., Vartanyan, D., & de Mink, S. E. (2021). Different to the core: The pre-supernova structures of massive single and binary-stripped stars. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202140506","short":"E. Laplace, S. Justham, M. Renzo, Y.L.L. Götberg, R. Farmer, D. Vartanyan, S.E. de Mink, Astronomy & Astrophysics 656 (2021).","ieee":"E. Laplace et al., “Different to the core: The pre-supernova structures of massive single and binary-stripped stars,” Astronomy & Astrophysics, vol. 656. EDP Sciences, 2021.","chicago":"Laplace, E., S. Justham, M. Renzo, Ylva Louise Linsdotter Götberg, R. Farmer, D. Vartanyan, and S. E. de Mink. “Different to the Core: The Pre-Supernova Structures of Massive Single and Binary-Stripped Stars.” Astronomy & Astrophysics. EDP Sciences, 2021. https://doi.org/10.1051/0004-6361/202140506.","ista":"Laplace E, Justham S, Renzo M, Götberg YLL, Farmer R, Vartanyan D, de Mink SE. 2021. Different to the core: The pre-supernova structures of massive single and binary-stripped stars. Astronomy & Astrophysics. 656, A58."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A58","date_published":"2021-12-02T00:00:00Z","doi":"10.1051/0004-6361/202140506","date_created":"2023-08-03T10:11:09Z","year":"2021","day":"02","publication":"Astronomy & Astrophysics","quality_controlled":"1","publisher":"EDP Sciences","oa":1},{"abstract":[{"text":"Helium star–carbon-oxygen white dwarf (CO WD) binaries are potential single-degenerate progenitor systems of thermonuclear supernovae. Revisiting a set of binary evolution calculations using the stellar evolution code MESA, we refine our previous predictions about which systems can lead to a thermonuclear supernova and then characterize the properties of the helium star donor at the time of explosion. We convert these model properties to near-UV/optical magnitudes assuming a blackbody spectrum and support this approach using a matched stellar atmosphere model. These models will be valuable to compare with pre-explosion imaging for future supernovae, though we emphasize the observational difficulty of detecting extremely blue companions. The pre-explosion source detected in association with SN 2012Z has been interpreted as a helium star binary containing an initially ultra-massive WD in a multiday orbit. However, extending our binary models to initial CO WD masses of up to 1.2 M⊙, we find that these systems undergo off-center carbon ignitions and thus are not expected to produce thermonuclear supernovae. This tension suggests that, if SN 2012Z is associated with a helium star–WD binary, then the pre-explosion optical light from the system must be significantly modified by the binary environment and/or the WD does not have a carbon-rich interior composition.","lang":"eng"}],"oa_version":"Preprint","main_file_link":[{"url":"https://arxiv.org/abs/2109.14817","open_access":"1"}],"scopus_import":"1","intvolume":" 922","month":"12","publication_status":"published","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"language":[{"iso":"eng"}],"volume":922,"issue":"2","_id":"13454","article_type":"original","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","date_updated":"2023-08-21T11:52:05Z","extern":"1","oa":1,"quality_controlled":"1","publisher":"American Astronomical Society","year":"2021","publication":"The Astrophysical Journal","day":"03","date_created":"2023-08-03T10:10:58Z","doi":"10.3847/1538-4357/ac27ae","date_published":"2021-12-03T00:00:00Z","article_number":"241","citation":{"ama":"Wong TLS, Schwab J, Götberg YLL. Pre-explosion properties of Helium star donors to thermonuclear supernovae. The Astrophysical Journal. 2021;922(2). doi:10.3847/1538-4357/ac27ae","apa":"Wong, T. L. S., Schwab, J., & Götberg, Y. L. L. (2021). Pre-explosion properties of Helium star donors to thermonuclear supernovae. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ac27ae","short":"T.L.S. Wong, J. Schwab, Y.L.L. Götberg, The Astrophysical Journal 922 (2021).","ieee":"T. L. S. Wong, J. Schwab, and Y. L. L. Götberg, “Pre-explosion properties of Helium star donors to thermonuclear supernovae,” The Astrophysical Journal, vol. 922, no. 2. American Astronomical Society, 2021.","mla":"Wong, Tin Long Sunny, et al. “Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae.” The Astrophysical Journal, vol. 922, no. 2, 241, American Astronomical Society, 2021, doi:10.3847/1538-4357/ac27ae.","ista":"Wong TLS, Schwab J, Götberg YLL. 2021. Pre-explosion properties of Helium star donors to thermonuclear supernovae. The Astrophysical Journal. 922(2), 241.","chicago":"Wong, Tin Long Sunny, Josiah Schwab, and Ylva Louise Linsdotter Götberg. “Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae.” The Astrophysical Journal. American Astronomical Society, 2021. https://doi.org/10.3847/1538-4357/ac27ae."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"No","external_id":{"arxiv":["2109.14817"]},"author":[{"full_name":"Wong, Tin Long Sunny","last_name":"Wong","first_name":"Tin Long Sunny"},{"first_name":"Josiah","full_name":"Schwab, Josiah","last_name":"Schwab"},{"last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"}],"title":"Pre-explosion properties of Helium star donors to thermonuclear supernovae"},{"issue":"2","volume":923,"publication_status":"published","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"language":[{"iso":"eng"}],"main_file_link":[{"url":"https://arxiv.org/abs/2107.10933","open_access":"1"}],"scopus_import":"1","intvolume":" 923","month":"12","abstract":[{"lang":"eng","text":"Most massive stars are born in binaries close enough for mass transfer episodes. These modify the appearance, structure, and future evolution of both stars. We compute the evolution of a 100-day-period binary, consisting initially of a 25 M⊙ star and a 17 M⊙ star, which experiences stable mass transfer. We focus on the impact of mass accretion on the surface composition, internal rotation, and structure of the accretor. To anchor our models, we show that our accretor broadly reproduces the properties of ζ Ophiuchi, which has long been proposed to have accreted mass before being ejected as a runaway star when the companion exploded. We compare our accretor to models of single rotating stars and find that the later and stronger spin-up provided by mass accretion produces significant differences. Specifically, the core of the accretor retains higher spin at the end of the main sequence, and a convective layer develops that changes its density profile. Moreover, the surface of the accretor star is polluted by CNO-processed material donated by the companion. Our models show effects of mass accretion in binaries that are not captured in single rotating stellar models. This possibly impacts the further evolution (either in a binary or as single stars), the final collapse, and the resulting spin of the compact object."}],"oa_version":"Preprint","date_updated":"2023-08-21T11:59:34Z","extern":"1","article_type":"original","type":"journal_article","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","_id":"13453","date_created":"2023-08-03T10:10:48Z","date_published":"2021-12-29T00:00:00Z","doi":"10.3847/1538-4357/ac29c5","year":"2021","publication":"The Astrophysical Journal","day":"29","oa":1,"publisher":"American Astronomical Society","quality_controlled":"1","article_processing_charge":"No","external_id":{"arxiv":["2107.10933"]},"author":[{"full_name":"Renzo, M.","last_name":"Renzo","first_name":"M."},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg"}],"title":"Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi","citation":{"ista":"Renzo M, Götberg YLL. 2021. Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi. The Astrophysical Journal. 923(2), 277.","chicago":"Renzo, M., and Ylva Louise Linsdotter Götberg. “Evolution of Accretor Stars in Massive Binaries: Broader Implications from Modeling ζ Ophiuchi.” The Astrophysical Journal. American Astronomical Society, 2021. https://doi.org/10.3847/1538-4357/ac29c5.","ieee":"M. Renzo and Y. L. L. Götberg, “Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi,” The Astrophysical Journal, vol. 923, no. 2. American Astronomical Society, 2021.","short":"M. Renzo, Y.L.L. Götberg, The Astrophysical Journal 923 (2021).","apa":"Renzo, M., & Götberg, Y. L. L. (2021). Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/1538-4357/ac29c5","ama":"Renzo M, Götberg YLL. Evolution of accretor stars in massive binaries: Broader implications from modeling ζ Ophiuchi. The Astrophysical Journal. 2021;923(2). doi:10.3847/1538-4357/ac29c5","mla":"Renzo, M., and Ylva Louise Linsdotter Götberg. “Evolution of Accretor Stars in Massive Binaries: Broader Implications from Modeling ζ Ophiuchi.” The Astrophysical Journal, vol. 923, no. 2, 277, American Astronomical Society, 2021, doi:10.3847/1538-4357/ac29c5."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"277"},{"citation":{"ista":"Baykusheva DR, Chacón A, Lu J, Bailey TP, Sobota JA, Soifer H, Kirchmann PS, Rotundu C, Uher C, Heinz TF, Reis DA, Ghimire S. 2021. All-optical probe of three-dimensional topological insulators based on high-harmonic generation by circularly polarized laser fields. Nano Letters. 21(21), 8970–8978.","chicago":"Baykusheva, Denitsa Rangelova, Alexis Chacón, Jian Lu, Trevor P. Bailey, Jonathan A. Sobota, Hadas Soifer, Patrick S. Kirchmann, et al. “All-Optical Probe of Three-Dimensional Topological Insulators Based on High-Harmonic Generation by Circularly Polarized Laser Fields.” Nano Letters. American Chemical Society, 2021. https://doi.org/10.1021/acs.nanolett.1c02145.","apa":"Baykusheva, D. R., Chacón, A., Lu, J., Bailey, T. P., Sobota, J. A., Soifer, H., … Ghimire, S. (2021). All-optical probe of three-dimensional topological insulators based on high-harmonic generation by circularly polarized laser fields. Nano Letters. American Chemical Society. https://doi.org/10.1021/acs.nanolett.1c02145","ama":"Baykusheva DR, Chacón A, Lu J, et al. All-optical probe of three-dimensional topological insulators based on high-harmonic generation by circularly polarized laser fields. Nano Letters. 2021;21(21):8970-8978. doi:10.1021/acs.nanolett.1c02145","short":"D.R. Baykusheva, A. Chacón, J. Lu, T.P. Bailey, J.A. Sobota, H. Soifer, P.S. Kirchmann, C. Rotundu, C. Uher, T.F. Heinz, D.A. Reis, S. Ghimire, Nano Letters 21 (2021) 8970–8978.","ieee":"D. R. Baykusheva et al., “All-optical probe of three-dimensional topological insulators based on high-harmonic generation by circularly polarized laser fields,” Nano Letters, vol. 21, no. 21. American Chemical Society, pp. 8970–8978, 2021.","mla":"Baykusheva, Denitsa Rangelova, et al. “All-Optical Probe of Three-Dimensional Topological Insulators Based on High-Harmonic Generation by Circularly Polarized Laser Fields.” Nano Letters, vol. 21, no. 21, American Chemical Society, 2021, pp. 8970–78, doi:10.1021/acs.nanolett.1c02145."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"first_name":"Denitsa Rangelova","id":"71b4d059-2a03-11ee-914d-dfa3beed6530","full_name":"Baykusheva, Denitsa Rangelova","last_name":"Baykusheva"},{"last_name":"Chacón","full_name":"Chacón, Alexis","first_name":"Alexis"},{"full_name":"Lu, Jian","last_name":"Lu","first_name":"Jian"},{"first_name":"Trevor P.","last_name":"Bailey","full_name":"Bailey, Trevor P."},{"last_name":"Sobota","full_name":"Sobota, Jonathan A.","first_name":"Jonathan A."},{"first_name":"Hadas","full_name":"Soifer, Hadas","last_name":"Soifer"},{"last_name":"Kirchmann","full_name":"Kirchmann, Patrick S.","first_name":"Patrick S."},{"first_name":"Costel","last_name":"Rotundu","full_name":"Rotundu, Costel"},{"last_name":"Uher","full_name":"Uher, Ctirad","first_name":"Ctirad"},{"first_name":"Tony F.","last_name":"Heinz","full_name":"Heinz, Tony F."},{"first_name":"David A.","full_name":"Reis, David A.","last_name":"Reis"},{"full_name":"Ghimire, Shambhu","last_name":"Ghimire","first_name":"Shambhu"}],"article_processing_charge":"No","external_id":{"arxiv":["2109.15291"],"pmid":["34676752"]},"title":"All-optical probe of three-dimensional topological insulators based on high-harmonic generation by circularly polarized laser fields","quality_controlled":"1","publisher":"American Chemical Society","oa":1,"year":"2021","day":"22","publication":"Nano Letters","page":"8970-8978","date_published":"2021-10-22T00:00:00Z","doi":"10.1021/acs.nanolett.1c02145","date_created":"2023-08-09T13:09:15Z","_id":"13996","type":"journal_article","article_type":"original","status":"public","keyword":["Mechanical Engineering","Condensed Matter Physics","General Materials Science","General Chemistry","Bioengineering"],"date_updated":"2023-08-22T07:32:00Z","extern":"1","abstract":[{"lang":"eng","text":"We report the observation of an anomalous nonlinear optical response of the prototypical three-dimensional topological insulator bismuth selenide through the process of high-order harmonic generation. We find that the generation efficiency increases as the laser polarization is changed from linear to elliptical, and it becomes maximum for circular polarization. With the aid of a microscopic theory and a detailed analysis of the measured spectra, we reveal that such anomalous enhancement encodes the characteristic topology of the band structure that originates from the interplay of strong spin–orbit coupling and time-reversal symmetry protection. The implications are in ultrafast probing of topological phase transitions, light-field driven dissipationless electronics, and quantum computation."}],"pmid":1,"oa_version":"Published Version","scopus_import":"1","main_file_link":[{"url":"https://doi.org/10.1021/acs.nanolett.1c02145","open_access":"1"}],"month":"10","intvolume":" 21","publication_identifier":{"issn":["1530-6984"],"eissn":["1530-6992"]},"publication_status":"published","language":[{"iso":"eng"}],"issue":"21","volume":21}]