Double White Dwarf Mergers as Progenitors of Long-Period Transients
Manuel Malheiro, Sarah V. Borges, Jaziel G. Coelho, Khashayar Kianfar, Ronaldo V. Lobato, Edson Otoniel, Jorge A. Rueda, Manoel F. Sousa, Fridolin Weber

TL;DR
This paper proposes that long-period transients like GLEAM-X J1627-5235 are isolated, highly magnetized white dwarf pulsars formed from double white dwarf mergers, supported by modeling their rotational evolution and observational constraints.
Contribution
It introduces a model where double white dwarf mergers produce isolated, magnetized WD pulsars explaining long-period transients, supported by rotational evolution calculations.
Findings
The rotational age of GLEAM-X J1627-5235 is about 572 million years.
The model aligns with optical upper limits for GLEAM-X J1627-5235.
The approach can be applied to other long-period transients.
Abstract
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…
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Taxonomy
TopicsPulsars and Gravitational Waves Research · Astronomy and Astrophysical Research · Gamma-ray bursts and supernovae
