{"type":"journal_article","citation":{"ista":"Wong TLS, Schwab J, Götberg YLL. 2021. Pre-explosion properties of Helium star donors to thermonuclear supernovae. The Astrophysical Journal. 922(2), 241.","ama":"Wong TLS, Schwab J, Götberg YLL. Pre-explosion properties of Helium star donors to thermonuclear supernovae. <i>The Astrophysical Journal</i>. 2021;922(2). doi:<a href=\"https://doi.org/10.3847/1538-4357/ac27ae\">10.3847/1538-4357/ac27ae</a>","chicago":"Wong, Tin Long Sunny, Josiah Schwab, and Ylva Louise Linsdotter Götberg. “Pre-Explosion Properties of Helium Star Donors to Thermonuclear Supernovae.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2021. <a href=\"https://doi.org/10.3847/1538-4357/ac27ae\">https://doi.org/10.3847/1538-4357/ac27ae</a>.","ieee":"T. L. S. Wong, J. Schwab, and Y. L. L. Götberg, “Pre-explosion properties of Helium star donors to thermonuclear supernovae,” <i>The Astrophysical Journal</i>, 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.” <i>The Astrophysical Journal</i>, vol. 922, no. 2, 241, American Astronomical Society, 2021, doi:<a href=\"https://doi.org/10.3847/1538-4357/ac27ae\">10.3847/1538-4357/ac27ae</a>.","short":"T.L.S. Wong, J. Schwab, Y.L.L. Götberg, The Astrophysical Journal 922 (2021).","apa":"Wong, T. L. S., Schwab, J., &#38; Götberg, Y. L. L. (2021). Pre-explosion properties of Helium star donors to thermonuclear supernovae. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.3847/1538-4357/ac27ae\">https://doi.org/10.3847/1538-4357/ac27ae</a>"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"oa_version":"Preprint","title":"Pre-explosion properties of Helium star donors to thermonuclear supernovae","month":"12","issue":"2","doi":"10.3847/1538-4357/ac27ae","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"_id":"13454","publication_status":"published","oa":1,"scopus_import":"1","publisher":"American Astronomical Society","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","author":[{"full_name":"Wong, Tin Long Sunny","first_name":"Tin Long Sunny","last_name":"Wong"},{"first_name":"Josiah","full_name":"Schwab, Josiah","last_name":"Schwab"},{"orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter","full_name":"Götberg, Ylva Louise Linsdotter","last_name":"Götberg","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"}],"language":[{"iso":"eng"}],"date_published":"2021-12-03T00:00:00Z","article_processing_charge":"No","year":"2021","date_created":"2023-08-03T10:10:58Z","article_number":"241","publication":"The Astrophysical Journal","article_type":"original","external_id":{"arxiv":["2109.14817"]},"volume":922,"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2109.14817"}],"extern":"1","quality_controlled":"1","day":"03","status":"public","abstract":[{"lang":"eng","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."}],"date_updated":"2023-08-21T11:52:05Z","intvolume":"       922"}