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Published January 1, 2024 | Version v1
Journal article Open

A joint SRG/eROSITA plus ZTF search: Discovery of a 97-min period eclipsing cataclysmic variable with evidence of a brown dwarf secondary

Creators

  • 1. Kazan Fed Univ, Kremlevskaya St 18, Kazan 420008, Russia
  • 2. CALTECH, Dept Astron, 1200 E Calif Blvd, Pasadena, CA 91125 USA
  • 3. Russian Acad Sci, Inst Astron, 48 Pyatnitskaya St, Moscow 109017, Russia
  • 4. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands
  • 5. Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England
  • 6. Univ Washington, Dept Astron, 3910 15th Ave NE, Seattle, WA 98195 USA
  • 7. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA

Description

Cataclysmic variables (CVs) that have evolved past the period minimum during their lifetimes are predicted to be systems with a brown dwarf donor. While population synthesis models predict that around 40-70 per cent of the Galactic CVs are post-period minimum systems referred to as 'period bouncers', only a few dozen confirmed systems are known. We report the study and characterization of a new eclipsing CV, SRGeJ041130.3+685350 (SRGeJ0411), discovered from a joint SRG/eROSITA and ZTF programme. The optical spectrum of SRGeJ0411 shows prominent hydrogen and helium emission lines, typical for CVs. We obtained optical high-speed photometry to confirm the eclipse of SRGeJ0411 and determine the orbital period to be P-orb approximate to 97.530 min. The spectral energy distribution suggests that the donor has an effective temperature of less than or similar to 1800 K. We constrain the donor mass with the period-density relationship for Roche lobe-filling stars and find that M-donor less than or similar to 0.04 M-circle dot. The binary parameters are consistent with evolutionary models for post-period minimum CVs, suggesting that SRGeJ0411 is a new period bouncer. The optical emission lines of SRGeJ0411 are single-peaked despite the system being eclipsing, which is typically only seen due to stream-fed accretion in polars. X-ray spectroscopy hints that the white dwarf in SRGeJ0411 could be magnetic, but verifying the magnetic nature of SRGeJ0411 requires further investigation. The lack of optical outbursts has made SRGeJ0411 elusive in previous surveys, and joint X-ray and optical surveys highlight the potential for discovering similar systems in the near future.

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