{"scopus_import":"1","quality_controlled":"1","date_published":"2020-04-04T00:00:00Z","volume":493,"article_processing_charge":"No","citation":{"mla":"Renzo, M., et al. “Sensitivity of the Lower Edge of the Pair-Instability Black Hole Mass Gap to the Treatment of Time-Dependent Convection.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 3, Oxford University Press, 2020, pp. 4333–41, doi:<a href=\"https://doi.org/10.1093/mnras/staa549\">10.1093/mnras/staa549</a>.","ista":"Renzo M, Farmer RJ, Justham S, de Mink SE, Götberg YLL, Marchant P. 2020. Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection. Monthly Notices of the Royal Astronomical Society. 493(3), 4333–4341.","ieee":"M. Renzo, R. J. Farmer, S. Justham, S. E. de Mink, Y. L. L. Götberg, and P. Marchant, “Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 493, no. 3. Oxford University Press, pp. 4333–4341, 2020.","short":"M. Renzo, R.J. Farmer, S. Justham, S.E. de Mink, Y.L.L. Götberg, P. Marchant, Monthly Notices of the Royal Astronomical Society 493 (2020) 4333–4341.","ama":"Renzo M, Farmer RJ, Justham S, de Mink SE, Götberg YLL, Marchant P. Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;493(3):4333-4341. doi:<a href=\"https://doi.org/10.1093/mnras/staa549\">10.1093/mnras/staa549</a>","apa":"Renzo, M., Farmer, R. J., Justham, S., de Mink, S. E., Götberg, Y. L. L., &#38; Marchant, P. (2020). Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa549\">https://doi.org/10.1093/mnras/staa549</a>","chicago":"Renzo, M, R J Farmer, S Justham, S E de Mink, Ylva Louise Linsdotter Götberg, and P Marchant. “Sensitivity of the Lower Edge of the Pair-Instability Black Hole Mass Gap to the Treatment of Time-Dependent Convection.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa549\">https://doi.org/10.1093/mnras/staa549</a>."},"intvolume":"       493","title":"Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/staa549"}],"page":"4333-4341","day":"04","language":[{"iso":"eng"}],"author":[{"full_name":"Renzo, M","last_name":"Renzo","first_name":"M"},{"last_name":"Farmer","first_name":"R J","full_name":"Farmer, R J"},{"last_name":"Justham","first_name":"S","full_name":"Justham, S"},{"full_name":"de Mink, S E","last_name":"de Mink","first_name":"S E"},{"id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter"},{"full_name":"Marchant, P","first_name":"P","last_name":"Marchant"}],"abstract":[{"text":"Gravitational-wave detections are now probing the black hole (BH) mass distribution, including the predicted pair-instability mass gap. These data require robust quantitative predictions, which are challenging to obtain. The most massive BH progenitors experience episodic mass ejections on time-scales shorter than the convective turnover time-scale. This invalidates the steady-state assumption on which the classic mixing length theory relies. We compare the final BH masses computed with two different versions of the stellar evolutionary code MESA\r\n⁠: (i) using the default implementation of Paxton et al. (2018) and (ii) solving an additional equation accounting for the time-scale for convective deceleration. In the second grid, where stronger convection develops during the pulses and carries part of the energy, we find weaker pulses. This leads to lower amounts of mass being ejected and thus higher final BH masses of up to ∼5M⊙\r\n⁠. The differences are much smaller for the progenitors that determine the maximum mass of BHs below the gap. This prediction is robust at MBH,max≃48M⊙\r\n⁠, at least within the idealized context of this study. This is an encouraging indication that current models are robust enough for comparison with the present-day gravitational-wave detections. However, the large differences between individual models emphasize the importance of improving the treatment of convection in stellar models, especially in the light of the data anticipated from the third generation of gravitational-wave detectors.","lang":"eng"}],"oa":1,"year":"2020","extern":"1","_id":"13465","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","article_type":"original","oa_version":"Published Version","doi":"10.1093/mnras/staa549","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","date_updated":"2023-08-09T12:53:37Z","issue":"3","publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","external_id":{"arxiv":["2002.08200"]},"month":"04","date_created":"2023-08-03T10:13:20Z","publication_status":"published"}