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V392 Persei: A γ-ray bright nova eruption from a known dwarf nova

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posted on 2024-10-01, 09:26 authored by FJ Murphy-Glaysher, MJ Darnley, J Harvey, AM Newsam, KL Page, S Starrfield, RM Wagner, CE Woodward, DM Terndrup, S Kafka, T Arranz Heras, P Berardi, E Bertrand, R Biernikowicz, C Boussin, D Boyd, Y Buchet, M Bundas, D Coulter, D Dejean, A Diepvens, S Dvorak, J Edlin, T Eenmae, H Eggenstein, R Fournier, O Garde, J Gout, D Janzen, P Jordanov, H Kiiskinen, D Lane, R Larochelle, R Leadbeater, D Mankel, G Martineau, I Miller, R Modic, J Montier, M Morales Aimar, E Muyllaert, R Naves Nogues, D O'Keeffe, A Oksanen, M Pyatnytskyy, R Rast, B Rodgers, D Rodriguez Perez, F Schorr, E Schwendeman, S Shadick, S Sharpe, F Soldán Alfaro, T Sove, G Stone, T Tordai, R Venne, W Vollmann, M Vrastak, K Wenzel
V392 Persei is a known dwarf nova (DN) that underwent a classical nova eruption in 2018. Here we report ground-based optical, Swift UV and X-ray, and Fermi-LAT γ-ray observations following the eruption for almost three years. V392 Per is one of the fastest evolving novae yet observed, with a t2 decline time of 2 d. Early spectra present evidence for multiple and interacting mass ejections, with the associated shocks driving both the γ-ray and early optical luminosity. V392 Per entered Sun-constraint within days of eruption. Upon exit, the nova had evolved to the nebular phase, and we saw the tail of the supersoft X-ray phase. Subsequent optical emission captured the fading ejecta alongside a persistent narrow line emission spectrum from the accretion disc. Ongoing hard X-ray emission is characteristic of a standing accretion shock in an intermediate polar. Analysis of the optical data reveals an orbital period of 3.230 ± 0.003 d, but we see no evidence for a white dwarf (WD) spin period. The optical and X-ray data suggest a high mass WD, the pre-nova spectral energy distribution (SED) indicates an evolved donor, and the post-nova SED points to a high mass accretion rate. Following eruption, the system has remained in a nova-like high mass transfer state, rather than returning to the pre-nova DN low mass transfer configuration. We suggest that this high state is driven by irradiation of the donor by the nova eruption. In many ways, V392 Per shows similarity to the well-studied nova and DN GK Persei.

Funding

Liverpool John Moores University ARI Consolidated Grant 2021-2024

Science and Technology Facilities Council

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STFC Liverpool John Moores 2018 DTP

Science and Technology Facilities Council

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Liverpool Telescope Operations 2019-2020

Science and Technology Facilities Council

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Liverpool Telescope Operations 2020-2023

Science and Technology Facilities Council

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History

Citation

F J Murphy-Glaysher, M J Darnley, É J Harvey, A M Newsam, K L Page, S Starrfield, R M Wagner, C E Woodward, D M Terndrup, S Kafka, T Arranz Heras, P Berardi, E Bertrand, R Biernikowicz, C Boussin, D Boyd, Y Buchet, M Bundas, D Coulter, D Dejean, A Diepvens, S Dvorak, J Edlin, T Eenmae, H Eggenstein, R Fournier, O Garde, J Gout, D Janzen, P Jordanov, H Kiiskinen, D Lane, R Larochelle, R Leadbeater, D Mankel, G Martineau, I Miller, R Modic, J Montier, M Morales Aimar, E Muyllaert, R Naves Nogues, D O’Keeffe, A Oksanen, M Pyatnytskyy, R Rast, B Rodgers, D Rodriguez Perez, F Schorr, E Schwendeman, S Shadick, S Sharpe, F Soldán Alfaro, T Sove, G Stone, T Tordai, R Venne, W Vollmann, M Vrastak, K Wenzel, V392 Persei: A γ-ray bright nova eruption from a known dwarf nova, Monthly Notices of the Royal Astronomical Society, Volume 514, Issue 4, August 2022, Pages 6183–6202, https://doi.org/10.1093/mnras/stac1577

Author affiliation

School of Physics and Astronomy, University of Leicester

Version

  • VoR (Version of Record)

Published in

Monthly Notices of the Royal Astronomical Society

Volume

514

Issue

4

Pagination

6183 - 6202

Publisher

Oxford University Press (OUP)

issn

0035-8711

eissn

1365-2966

Acceptance date

2022-06-06

Copyright date

2022

Available date

2024-10-01

Language

en

Data Access Statement

For the purpose of open access, the author has applied a Creative Commons Attribution (CC BY) license to any Author Accepted Manuscript version arising. All data supporting this study are available from the respective telescope archives, in the supplementary information, or on reasonable request from the author.

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