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PreprintCC BY 4.0arXiv

On the Nature of the BeWD System Nova FQ Circinus

  • Shatakshi Chamoli
  • Philip A. Charles
  • Judhajeet Basu
  • G. C. Anupama
  • Sudhanshu Barway
  • Przemek Mróz
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Abstract

The classical nova FQ Cir (Schaefer et al. 2026) has recently been shown to have a Be star donor, and has been identified as a High Mass Cataclysmic Variable (HMCV), with an orbital period of ∼ 2.04d (twice the 1.02d periodogram peak). Using the extensive OGLE optical archive, together with existing observations from ASAS-SN we instead find significant modulation between ∼ 50−60~days and propose that the orbital period is likely closer to ∼ 62d. We interpret the low amplitude 1.02 d modulation as a non-radial pulsation of the Be star. We also reassess the HMCV classification based on properties of known Be star-white dwarf systems.

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Cite

BibTeXRIS
BibTeX
@misc{chamoli2026nature,
  title = {{On the Nature of the BeWD System Nova FQ Circinus}},
  author = {Shatakshi Chamoli and Philip A. Charles and Judhajeet Basu and G. C. Anupama and Sudhanshu Barway and Przemek Mróz},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.26957},
  eprint = {2610.26957},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.26957},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - On the Nature of the BeWD System Nova FQ Circinus
AU  - Shatakshi Chamoli
AU  - Philip A. Charles
AU  - Judhajeet Basu
AU  - G. C. Anupama
AU  - Sudhanshu Barway
AU  - Przemek Mróz
PY  - 2026
DA  - 2026/10/18
PB  - arXiv
DO  - 10.48550/arxiv.2610.26957
UR  - https://arxiv.org/abs/2610.26957
AB  - The classical nova FQ Cir (Schaefer et al. 2026) has recently been shown to have a Be star donor, and has been identified as a High Mass Cataclysmic Variable (HMCV), with an orbital period of ∼ 2.04d (twice the 1.02d periodogram peak). Using the extensive OGLE optical archive, together with existing observations from ASAS-SN we instead find significant modulation between ∼ 50−60~days and propose that the orbital period is likely closer to ∼ 62d. We interpret the low amplitude 1.02 d modulation as a non-radial pulsation of the Be star. We also reassess the HMCV classification based on properties of known Be star-white dwarf systems.
ER  -