Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel
Black hole (BH) ultracompact X-ray binaries (UCXBs) are potential Galactic low-frequency gravitational wave (GW) sources. As an alternative channel, BH UCXBs can evolve from BH+He star binaries. In this work, we perform a detailed stellar evolution model for the formation and evolution of BH UCXBs e...
| Main Authors: | , , , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2024-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/ad12d3 |
| _version_ | 1797352293858803712 |
|---|---|
| author | Ke Qin Kun Xu Dong-Dong Liu Long Jiang Bo Wang Wen-Cong Chen |
| author_facet | Ke Qin Kun Xu Dong-Dong Liu Long Jiang Bo Wang Wen-Cong Chen |
| author_sort | Ke Qin |
| collection | DOAJ |
| description | Black hole (BH) ultracompact X-ray binaries (UCXBs) are potential Galactic low-frequency gravitational wave (GW) sources. As an alternative channel, BH UCXBs can evolve from BH+He star binaries. In this work, we perform a detailed stellar evolution model for the formation and evolution of BH UCXBs evolving from the He star channel to diagnose their detectability as low-frequency GW sources. Our calculations found that some nascent BH+He star binaries after the common-envelope (CE) phase could evolve into UCXB-LISA sources with a maximum GW frequency of ∼5 mHz, which can be detected in a distance of 10 kpc (or 100 kpc). Once BH+He star systems become UCXBs through mass transfer, they would emit X-ray luminosities of ∼10 ^38 erg s ^−1 , making them ideal multimessenger objects. If the initial He-star masses are ≥0.7 M _⊙ , those systems are likely to experience two Roche lobe overflows, and the X-ray luminosity can reach a maximum of 3.5 × 10 ^39 erg s ^−1 in the second mass-transfer stage. The initial He-star masses and initial orbital periods of progenitors of Galactic BH UCXB-LISA sources are in the range of 0.32–2.9 M _⊙ and 0.02–0.19 days, respectively. Nearly all BH+He star binaries in the above parameter space can evolve into GW sources whose chirp masses can be accurately measured. Employing a population synthesis simulation, we predict the birthrate and detection number of Galactic BH UCXB-LISA sources evolving from the He star channel are R = 2.2 × 10 ^−6 yr ^−1 and 33 for an optimistic CE parameter, respectively. |
| first_indexed | 2024-03-08T13:14:23Z |
| format | Article |
| id | doaj.art-72681df996a74053bbe80805b0804586 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-08T13:14:23Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-72681df996a74053bbe80805b08045862024-01-18T10:20:46ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01961111010.3847/1538-4357/ad12d3Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star ChannelKe Qin0https://orcid.org/0000-0001-9206-1641Kun Xu1https://orcid.org/0000-0002-9739-8929Dong-Dong Liu2https://orcid.org/0000-0002-3007-8197Long Jiang3https://orcid.org/0000-0002-2479-1295Bo Wang4https://orcid.org/0000-0002-3231-1167Wen-Cong Chen5https://orcid.org/0000-0002-0785-5349School of Science, Qingdao University of Technology , Qingdao 266525, People's Republic of China ; chenwc@pku.edu.cn; School of Physics, Zhengzhou University , Zhengzhou 450001, People's Republic of ChinaSchool of Science, Qingdao University of Technology , Qingdao 266525, People's Republic of China ; chenwc@pku.edu.cnKey Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People's Republic of ChinaSchool of Science, Qingdao University of Technology , Qingdao 266525, People's Republic of China ; chenwc@pku.edu.cn; School of Physics and Electrical Information, Shangqiu Normal University , Shangqiu 476000, People's Republic of ChinaKey Laboratory for the Structure and Evolution of Celestial Objects, Yunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People's Republic of ChinaSchool of Science, Qingdao University of Technology , Qingdao 266525, People's Republic of China ; chenwc@pku.edu.cn; School of Physics and Electrical Information, Shangqiu Normal University , Shangqiu 476000, People's Republic of ChinaBlack hole (BH) ultracompact X-ray binaries (UCXBs) are potential Galactic low-frequency gravitational wave (GW) sources. As an alternative channel, BH UCXBs can evolve from BH+He star binaries. In this work, we perform a detailed stellar evolution model for the formation and evolution of BH UCXBs evolving from the He star channel to diagnose their detectability as low-frequency GW sources. Our calculations found that some nascent BH+He star binaries after the common-envelope (CE) phase could evolve into UCXB-LISA sources with a maximum GW frequency of ∼5 mHz, which can be detected in a distance of 10 kpc (or 100 kpc). Once BH+He star systems become UCXBs through mass transfer, they would emit X-ray luminosities of ∼10 ^38 erg s ^−1 , making them ideal multimessenger objects. If the initial He-star masses are ≥0.7 M _⊙ , those systems are likely to experience two Roche lobe overflows, and the X-ray luminosity can reach a maximum of 3.5 × 10 ^39 erg s ^−1 in the second mass-transfer stage. The initial He-star masses and initial orbital periods of progenitors of Galactic BH UCXB-LISA sources are in the range of 0.32–2.9 M _⊙ and 0.02–0.19 days, respectively. Nearly all BH+He star binaries in the above parameter space can evolve into GW sources whose chirp masses can be accurately measured. Employing a population synthesis simulation, we predict the birthrate and detection number of Galactic BH UCXB-LISA sources evolving from the He star channel are R = 2.2 × 10 ^−6 yr ^−1 and 33 for an optimistic CE parameter, respectively.https://doi.org/10.3847/1538-4357/ad12d3X-ray binary starsBlack holesGravitational wave sourcesStellar evolution |
| spellingShingle | Ke Qin Kun Xu Dong-Dong Liu Long Jiang Bo Wang Wen-Cong Chen Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel The Astrophysical Journal X-ray binary stars Black holes Gravitational wave sources Stellar evolution |
| title | Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel |
| title_full | Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel |
| title_fullStr | Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel |
| title_full_unstemmed | Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel |
| title_short | Black Hole Ultracompact X-Ray Binaries as Galactic Low-frequency Gravitational Wave Sources: The He Star Channel |
| title_sort | black hole ultracompact x ray binaries as galactic low frequency gravitational wave sources the he star channel |
| topic | X-ray binary stars Black holes Gravitational wave sources Stellar evolution |
| url | https://doi.org/10.3847/1538-4357/ad12d3 |
| work_keys_str_mv | AT keqin blackholeultracompactxraybinariesasgalacticlowfrequencygravitationalwavesourcesthehestarchannel AT kunxu blackholeultracompactxraybinariesasgalacticlowfrequencygravitationalwavesourcesthehestarchannel AT dongdongliu blackholeultracompactxraybinariesasgalacticlowfrequencygravitationalwavesourcesthehestarchannel AT longjiang blackholeultracompactxraybinariesasgalacticlowfrequencygravitationalwavesourcesthehestarchannel AT bowang blackholeultracompactxraybinariesasgalacticlowfrequencygravitationalwavesourcesthehestarchannel AT wencongchen blackholeultracompactxraybinariesasgalacticlowfrequencygravitationalwavesourcesthehestarchannel |