The double white dwarf merger progenitors of SDSS J2211+1136 and ZTF J1901+1458

Detalhes bibliográficos
Autor(a) principal: Sousa, Manoel Felipe
Data de Publicação: 2022
Outros Autores: Coelho, Jaziel Goulart, Araujo, José Carlos Neves de, Kepler, Souza Oliveira, Rueda Hernández, Jorge Armando
Tipo de documento: Artigo
Idioma: eng
Título da fonte: Repositório Institucional da UFRGS
Texto Completo: http://hdl.handle.net/10183/254155
Resumo: Double white dwarf (DWD) mergers are possibly the leading formation channel of massive, rapidly rotating, highfield magnetic white dwarfs (HFMWDs). However, a direct link connecting a DWD merger to any observed HFMWD is still missing. We here show that the HFMWDs SDSS J221141.80+113604.4 (hereafter J2211+1136) and ZTF J190132.9+145808.7 (hereafter J1901+1458) might be DWD merger products. J2211+1136 is a 1.27 Me white dwarf (WD) with a rotation period of 70.32 s and a surface magnetic field of 15 MG. J1901+1458 is a 1.327–1.365 Me WD with a rotation period of 416.20 s, and a surface magnetic field in the range 600–900 MG. With the assumption of single-star evolution and the currently measured WD masses and surface temperatures, the cooling ages of J2211+1136 and J1901+1458 are, respectively, 2.61–2.85 Gyr and 10–100 Myr. We hypothesize that these WDs are DWD merger products and compute the evolution of the postmerged configuration formed by a central WD surrounded by a disk. We show that the postmerger system evolves through three phases depending on whether accretion, mass ejection (propeller), or magnetic braking dominates the torque onto the central WD. We calculate the time the WD spends in each of these phases and obtain the accretion rate and disk mass for which the WD rotational age, i.e., the total time elapsed since the merger to the instant where the WD central remnant reaches the current measured rotation period, agrees with the estimated WD cooling age. We infer the mass values of the primary and secondary WD components of the DWD merger that lead to a postmerger evolution consistent with the observations.
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spelling Sousa, Manoel FelipeCoelho, Jaziel GoulartAraujo, José Carlos Neves deKepler, Souza OliveiraRueda Hernández, Jorge Armando2023-02-07T05:01:25Z20220004-637Xhttp://hdl.handle.net/10183/254155001160272Double white dwarf (DWD) mergers are possibly the leading formation channel of massive, rapidly rotating, highfield magnetic white dwarfs (HFMWDs). However, a direct link connecting a DWD merger to any observed HFMWD is still missing. We here show that the HFMWDs SDSS J221141.80+113604.4 (hereafter J2211+1136) and ZTF J190132.9+145808.7 (hereafter J1901+1458) might be DWD merger products. J2211+1136 is a 1.27 Me white dwarf (WD) with a rotation period of 70.32 s and a surface magnetic field of 15 MG. J1901+1458 is a 1.327–1.365 Me WD with a rotation period of 416.20 s, and a surface magnetic field in the range 600–900 MG. With the assumption of single-star evolution and the currently measured WD masses and surface temperatures, the cooling ages of J2211+1136 and J1901+1458 are, respectively, 2.61–2.85 Gyr and 10–100 Myr. We hypothesize that these WDs are DWD merger products and compute the evolution of the postmerged configuration formed by a central WD surrounded by a disk. We show that the postmerger system evolves through three phases depending on whether accretion, mass ejection (propeller), or magnetic braking dominates the torque onto the central WD. We calculate the time the WD spends in each of these phases and obtain the accretion rate and disk mass for which the WD rotational age, i.e., the total time elapsed since the merger to the instant where the WD central remnant reaches the current measured rotation period, agrees with the estimated WD cooling age. We infer the mass values of the primary and secondary WD components of the DWD merger that lead to a postmerger evolution consistent with the observations.application/pdfengThe astrophysical journal. Bristol. Vol. 941, no. 1 (Dec. 2022), 28, 10 p.Anãs brancasFormacao de estrelasRotacao estelarStellar remnantsWhite dwarf starsStellar mergersCompact binary starsCompact objectsStellar rotationThe double white dwarf merger progenitors of SDSS J2211+1136 and ZTF J1901+1458Estrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSTEXT001160272.pdf.txt001160272.pdf.txtExtracted Texttext/plain54263http://www.lume.ufrgs.br/bitstream/10183/254155/2/001160272.pdf.txt0bf10246dafffa12427399b2678bd06fMD52ORIGINAL001160272.pdfTexto completo (inglês)application/pdf891685http://www.lume.ufrgs.br/bitstream/10183/254155/1/001160272.pdfa47fcb93c5ec5808809a5eb17441eac5MD5110183/2541552023-02-08 06:01:18.257855oai:www.lume.ufrgs.br:10183/254155Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2023-02-08T08:01:18Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false
dc.title.pt_BR.fl_str_mv The double white dwarf merger progenitors of SDSS J2211+1136 and ZTF J1901+1458
title The double white dwarf merger progenitors of SDSS J2211+1136 and ZTF J1901+1458
spellingShingle The double white dwarf merger progenitors of SDSS J2211+1136 and ZTF J1901+1458
Sousa, Manoel Felipe
Anãs brancas
Formacao de estrelas
Rotacao estelar
Stellar remnants
White dwarf stars
Stellar mergers
Compact binary stars
Compact objects
Stellar rotation
title_short The double white dwarf merger progenitors of SDSS J2211+1136 and ZTF J1901+1458
title_full The double white dwarf merger progenitors of SDSS J2211+1136 and ZTF J1901+1458
title_fullStr The double white dwarf merger progenitors of SDSS J2211+1136 and ZTF J1901+1458
title_full_unstemmed The double white dwarf merger progenitors of SDSS J2211+1136 and ZTF J1901+1458
title_sort The double white dwarf merger progenitors of SDSS J2211+1136 and ZTF J1901+1458
author Sousa, Manoel Felipe
author_facet Sousa, Manoel Felipe
Coelho, Jaziel Goulart
Araujo, José Carlos Neves de
Kepler, Souza Oliveira
Rueda Hernández, Jorge Armando
author_role author
author2 Coelho, Jaziel Goulart
Araujo, José Carlos Neves de
Kepler, Souza Oliveira
Rueda Hernández, Jorge Armando
author2_role author
author
author
author
dc.contributor.author.fl_str_mv Sousa, Manoel Felipe
Coelho, Jaziel Goulart
Araujo, José Carlos Neves de
Kepler, Souza Oliveira
Rueda Hernández, Jorge Armando
dc.subject.por.fl_str_mv Anãs brancas
Formacao de estrelas
Rotacao estelar
topic Anãs brancas
Formacao de estrelas
Rotacao estelar
Stellar remnants
White dwarf stars
Stellar mergers
Compact binary stars
Compact objects
Stellar rotation
dc.subject.eng.fl_str_mv Stellar remnants
White dwarf stars
Stellar mergers
Compact binary stars
Compact objects
Stellar rotation
description Double white dwarf (DWD) mergers are possibly the leading formation channel of massive, rapidly rotating, highfield magnetic white dwarfs (HFMWDs). However, a direct link connecting a DWD merger to any observed HFMWD is still missing. We here show that the HFMWDs SDSS J221141.80+113604.4 (hereafter J2211+1136) and ZTF J190132.9+145808.7 (hereafter J1901+1458) might be DWD merger products. J2211+1136 is a 1.27 Me white dwarf (WD) with a rotation period of 70.32 s and a surface magnetic field of 15 MG. J1901+1458 is a 1.327–1.365 Me WD with a rotation period of 416.20 s, and a surface magnetic field in the range 600–900 MG. With the assumption of single-star evolution and the currently measured WD masses and surface temperatures, the cooling ages of J2211+1136 and J1901+1458 are, respectively, 2.61–2.85 Gyr and 10–100 Myr. We hypothesize that these WDs are DWD merger products and compute the evolution of the postmerged configuration formed by a central WD surrounded by a disk. We show that the postmerger system evolves through three phases depending on whether accretion, mass ejection (propeller), or magnetic braking dominates the torque onto the central WD. We calculate the time the WD spends in each of these phases and obtain the accretion rate and disk mass for which the WD rotational age, i.e., the total time elapsed since the merger to the instant where the WD central remnant reaches the current measured rotation period, agrees with the estimated WD cooling age. We infer the mass values of the primary and secondary WD components of the DWD merger that lead to a postmerger evolution consistent with the observations.
publishDate 2022
dc.date.issued.fl_str_mv 2022
dc.date.accessioned.fl_str_mv 2023-02-07T05:01:25Z
dc.type.driver.fl_str_mv Estrangeiro
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dc.identifier.uri.fl_str_mv http://hdl.handle.net/10183/254155
dc.identifier.issn.pt_BR.fl_str_mv 0004-637X
dc.identifier.nrb.pt_BR.fl_str_mv 001160272
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url http://hdl.handle.net/10183/254155
dc.language.iso.fl_str_mv eng
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dc.relation.ispartof.pt_BR.fl_str_mv The astrophysical journal. Bristol. Vol. 941, no. 1 (Dec. 2022), 28, 10 p.
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