J/MNRAS/514/6183 V392 Per. A gamma-ray bright nova (Murphy-Glaysher+, 2022)
V392 Persei: A gamma-ray bright nova eruption from a known dwarf nova.
Murphy-Glaysher F.J., Darnley M.J., Harvey E.J., Newsam A.M., Page K.L.,
Starrfield S., Wagner R.M., Woodward C.E., Terndrup T.M., Kafka S.,
Arranz Heras T., Berardi P., Bertrand E., Biernikowicz R., Boussin C.,
Boyd D., Buchet Y., Bundas M., Coulter D., Dejean D., Diepvens A.,
Dvorak S., Edlin J., Eenmae T., Eggenstein H., Fournier R., Garde O.,
Gout J., Janzen D., Jordanov P., Kiiskinen H., Lane D., Larochelle R.,
Leadbeater R., Mankel D., Martineau G., Miller I., Modic R., Montier J.,
Morales Aimar M., Muyllaert E., Naves Nogues R., O'Keeffe D., Oksanen A.,
Pyatnytskyy M., Rast R., Rodgers B., Rodriguez Perez D., Schorr F.,
Schwendeman E., Shadick S., Sharpe S., Soldan Alfaro F., Sove T., Stone G.,
Tordai T., Venne R., Vollmann W., Vrastak M., Wenzel K.
<Mon. Not. R. Astron. Soc. 514, 6183-6202 (2022)>
=2022MNRAS.514.6183M 2022MNRAS.514.6183M (SIMBAD/NED BibCode)
ADC_Keywords: Novae ; Photometry, CCD ; Photometry, ultraviolet
Keywords: accretion, accretion discs - stars: individual (V392 Per) -
novae, cataclysmic variables - X-rays: stars - transients, novae
Abstract:
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 days. 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 super-soft X-ray phase. Subsequent optical emission
captured the fading ejecta alongside a persistent narrow line emission
spectrum from the accretion disk. 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 days, 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.
Description:
The photometry were collected using Liverpool Telescope IO:O, various
AAVSO observers (indicated by 'AAVSO' then the observer's initials),
Las Cumbres Observatory (LCOGT), and the Neil Gehrels Swift
Observatory UV/Optical Telescope (UVOT). For each set of observations,
the MJD at the midpoint of the observation, the date (UT), the time
since eruption, the Telescope (and observer for AAVSO observations),
passband, number of exposures, exposure time (unknown, and indicated
as "0" in the case of AAVSO observations), magnitude and magnitude
error are provided.
Objects:
----------------------------------------------------
RA (2000) DE Designation(s)
----------------------------------------------------
04 43 21.37 +47 21 25.87 V392 Per = NOVA Per 2018
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
phot.dat 75 1663 V392 Per observations in B, V, u, r, z, i,
UVM2, UVW1 and UVW2 bands
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Byte-by-byte Description of file: phot.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Band [BVuriz UVM2 UVW1 UVW2] Observed band
7- 15 F9.3 d MJD Midpoint of observation
17- 31 A15 --- Obs.date Midpoint of observation (UT), YYYY/MMMM/DD.ddd
33- 40 F8.3 d Time Time since eruption
42- 51 A10 --- Tel Telescope used (1)
53- 56 A4 --- Filter [BVurIz uvm2 uvw1 uvw2] Filter used for
observations
58 I1 --- Nexp Number of single exposures making up the
observation (0=unknown)
60- 62 I3 s ExpTime Exposure time of each single exposure
(0=unknown)
64- 69 F6.3 mag mag Apparent magnitude in Filter
71- 75 F5.3 mag e_mag Apparent magnitude uncertainty
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Note (1): "AAVSO observer_initials" for AAVSO observations.
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History:
From Fiona Murphy-Glaysher, F.J.MurphyGlaysher(at)2018.ljmu.ac.uk
Acknowledgements:
This work was funded by UK Research and Innovation (UKRI) grants. FMG
acknowledges a PhD studentship from the Science and Technology
Facilities Council (STFC), from grant number ST/V00087X/1. MJD and EJH
receive funding from STFC grant number ST/S505559/1. KLP acknowledges
funding from the UK Space Agency. The Liverpool Telescope was funded
by UKRI grants ST/S006176/1 and ST/T00147X/1. The Liverpool Telescope
is operated on the island of La Palma by Liverpool John Moores
University in the Spanish Observatorio del Roque de los Muchachos of
the Instituto de Astrofisica de Canarias with financial support from
STFC. This work uses observations from the Las Cumbres Observatory
global telescope network. We acknowledge with thanks the variable star
observations from the American Association of Variable Star Observers
(AAVSO) International Database contributed by observers worldwide and
used in this research.
(End) Fiona Murphy-Glaysher [LJMU, UK], Patricia Vannier [CDS] 29-Jun-2022