A 99-minute Double-lined White Dwarf Binary from SDSS-V
Vedant Chandra, Hsiang-Chih Hwang, Nadia L. Zakamska, Boris T., Gaensicke, J.J. Hermes, Axel Schwope, Carles Badenes, Gagik Tovmassian, Evan, B. Bauer, Dan Maoz, Matthias R. Schreiber, Odette F. Toloza, Keith P. Inight,, Hans-Walter Rix, Warren R. Brown

TL;DR
This paper reports the discovery and detailed analysis of a nearby double-lined white dwarf binary from SDSS-V, highlighting its potential as a gravitational wave source and its evolutionary future.
Contribution
The paper presents the first detailed characterization of a nearby double-lined WD+WD binary from SDSS-V, including orbital and stellar parameters, and discusses its implications for gravitational wave detection and supernova progenitors.
Findings
Binary will merge in approximately 220 million years.
System is a strong gravitational wave source detectable by future space interferometers.
Likely evolution into a helium star, not a Type Ia supernova.
Abstract
We report the discovery of SDSS J133725.26+395237.7 (hereafter SDSS J1337+3952), a double-lined white dwarf (WD+WD) binary identified in early data from the fifth generation Sloan Digital Sky Survey (SDSS-V). The double-lined nature of the system enables us to fully determine its orbital and stellar parameters with follow-up Gemini spectroscopy and Swift UVOT ultraviolet fluxes. The system is nearby ( pc), and consists of a primary and a secondary. SDSS J1337+3952 is a powerful source of gravitational waves in the millihertz regime, and will be detectable by future space-based interferometers. Due to this gravitational wave emission, the binary orbit will shrink down to the point of interaction in Myr. The inferred stellar masses indicate that SDSS J1337+3952 will likely not explode as a Type Ia supernova (SN Ia). Instead, the…
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