Double White Dwarf Mergers as Progenitors of Long-Period Transients
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2026
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| author | Malheiro, Manuel Borges, Sarah V. Coelho, Jaziel G. Kianfar, Khashayar Lobato, Ronaldo V. Otoniel, Edson Rueda, Jorge A. Sousa, Manoel F. Weber, Fridolin |
| author_facet | Malheiro, Manuel Borges, Sarah V. Coelho, Jaziel G. Kianfar, Khashayar Lobato, Ronaldo V. Otoniel, Edson Rueda, Jorge A. Sousa, Manoel F. Weber, Fridolin |
| contents | There is an ongoing discussion in the literature on the nature of long-period transients (LPTs), radio-emitting sources with periods ranging from hundreds to tens of thousands of seconds. Although some of these objects have been identified as white dwarf (WD) + M-dwarf binaries, this description currently does not fit the entire class. An example is GLEAM-X J162759.5-523504.3 (hereafter GLEAM-X J1627-5235), with a period of 1091 s, for which the lack of an optical counterpart disfavors the presence of such a binary system. In this case, GLEAM-X J1627-5235 could be interpreted as an isolated, massive, fast-rotating, and highly magnetized (~ 1e+9 G) WD pulsar. Its properties are consistent with a carbon-oxygen WD of mass ~1.3 Msun and radius ~2500 km, possibly supported by small-scale multipolar magnetosphere structures that keep it above the death line for WD-pulsars. We assess a double WD merger origin, modeling the post-merger rotational evolution under accretion, propeller, and magnetic braking torques. We find rotational age of ~572 Myr for GLEAM-X J1627-5235, i.e., the post-merger time required to reach its observed period. This result is consistent with current optical upper limits for GLEAM-X J1627-5235 and support the WD pulsar interpretation for this source. We also discuss how the same model can apply to other LPTs. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2603_08416 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Double White Dwarf Mergers as Progenitors of Long-Period Transients Malheiro, Manuel Borges, Sarah V. Coelho, Jaziel G. Kianfar, Khashayar Lobato, Ronaldo V. Otoniel, Edson Rueda, Jorge A. Sousa, Manoel F. Weber, Fridolin High Energy Astrophysical Phenomena Solar and Stellar Astrophysics There is an ongoing discussion in the literature on the nature of long-period transients (LPTs), radio-emitting sources with periods ranging from hundreds to tens of thousands of seconds. Although some of these objects have been identified as white dwarf (WD) + M-dwarf binaries, this description currently does not fit the entire class. An example is GLEAM-X J162759.5-523504.3 (hereafter GLEAM-X J1627-5235), with a period of 1091 s, for which the lack of an optical counterpart disfavors the presence of such a binary system. In this case, GLEAM-X J1627-5235 could be interpreted as an isolated, massive, fast-rotating, and highly magnetized (~ 1e+9 G) WD pulsar. Its properties are consistent with a carbon-oxygen WD of mass ~1.3 Msun and radius ~2500 km, possibly supported by small-scale multipolar magnetosphere structures that keep it above the death line for WD-pulsars. We assess a double WD merger origin, modeling the post-merger rotational evolution under accretion, propeller, and magnetic braking torques. We find rotational age of ~572 Myr for GLEAM-X J1627-5235, i.e., the post-merger time required to reach its observed period. This result is consistent with current optical upper limits for GLEAM-X J1627-5235 and support the WD pulsar interpretation for this source. We also discuss how the same model can apply to other LPTs. |
| title | Double White Dwarf Mergers as Progenitors of Long-Period Transients |
| topic | High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2603.08416 |