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Bow-shocks, nova shells, disc winds and tilted discs: the Nova-like V341 ara has it all

Bow-shocks, nova shells, disc winds and tilted discs: the Nova-like V341 ara has it all
Bow-shocks, nova shells, disc winds and tilted discs: the Nova-like V341 ara has it all
V341 Ara was recently recognised as one of the closest (d ~ 150 pc) and brightest (V~ 10) nova-like cataclysmic variables. This unique system is surrounded by a bright emission nebula, likely to be the remnant of a recent nova eruption. Embedded within this nebula is a prominent bow-shock, where the system's accretion disc wind runs into its own nova shell. In order to establish its fundamental properties, we present the first comprehensive multi-wavelength study of the system. Long-term photometry reveals quasi-periodic, super-orbital variations with a characteristic time-scale of 10-16 days and typical amplitude of ~1 mag. High-cadence photometry from TESS reveals for the first time both the orbital period and a "negative superhump" period. The latter is usually interpreted as the signature of a tilted accretion disc. We propose a recently developed disc instability model as a plausible explanation for the photometric behaviour. In our spectroscopic data, we clearly detect anti-phased absorption and emission line components. Their radial velocities suggest a high mass ratio, which in turn implies an unusually low white dwarf mass. We also constrain the wind mass-loss rate of the system from the spatially resolved [O iii] emission produced in the bow-shock; this can be used to test and calibrate accretion disc wind models. We suggest a possible association between V341 Ara and a "guest star" mentioned in Chinese historical records in AD1240. If this marks the date of the system's nova eruption, V341 Ara would be the oldest recovered nova of its class and an excellent laboratory for testing nova theory.
astro-ph.SR, astro-ph.HE
0035-8711
Segura, N. Castro
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Knigge, C.
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Acosta-Pulido, J. A.
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Altamirano, D.
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Palacio, S. del
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Santisteban, J. V. Hernandez
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Pahari, M.
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Rodriguez-Gil, P.
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Belardi, C.
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Buckley, D. A. H.
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Burleigh, M. R.
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Childress, M.
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Fender, R. P.
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Hewitt, D. M.
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James, D. J.
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Kuhn, R. B.
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Kuin, N. P. M.
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Pepper, J.
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Ponomareva, A. A.
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Pretorius, M. L.
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Rodríguez, J. E.
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Stassun, K. G.
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Williams, D. R. A.
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Woudt, P. A.
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Segura, N. Castro
26dfa223-df20-4ae1-98cc-7900dfe49fa3
Knigge, C.
ac320eec-631a-426e-b2db-717c8bf7857e
Acosta-Pulido, J. A.
d9c92523-3167-4c2b-9a0c-ca6e2076c904
Altamirano, D.
d5ccdb09-0b71-4303-9538-05b467be075b
Palacio, S. del
8d761da8-0ef9-4792-93fe-35390629a2fc
Santisteban, J. V. Hernandez
115e9657-d594-487b-b871-5c61cc32f692
Pahari, M.
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Rodriguez-Gil, P.
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Belardi, C.
be616a7e-15ff-40c1-862a-f37c116749ba
Buckley, D. A. H.
2b82e4e2-d175-4cb3-9868-46b13f4f890c
Burleigh, M. R.
b089db59-fe18-4409-8c14-848dc77eb40a
Childress, M.
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Fender, R. P.
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Hewitt, D. M.
712f3a35-1b74-4f42-ad32-bb55392a3c98
James, D. J.
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Kuhn, R. B.
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Kuin, N. P. M.
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Pepper, J.
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Ponomareva, A. A.
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Pretorius, M. L.
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Rodríguez, J. E.
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Stassun, K. G.
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Williams, D. R. A.
c9ded967-198f-4c26-96b1-8c03d7d26445
Woudt, P. A.
078a12fd-3894-42c5-b3b6-1747a9325c51

Segura, N. Castro, Knigge, C., Acosta-Pulido, J. A., Altamirano, D., Palacio, S. del, Santisteban, J. V. Hernandez, Pahari, M., Rodriguez-Gil, P., Belardi, C., Buckley, D. A. H., Burleigh, M. R., Childress, M., Fender, R. P., Hewitt, D. M., James, D. J., Kuhn, R. B., Kuin, N. P. M., Pepper, J., Ponomareva, A. A., Pretorius, M. L., Rodríguez, J. E., Stassun, K. G., Williams, D. R. A. and Woudt, P. A. (2020) Bow-shocks, nova shells, disc winds and tilted discs: the Nova-like V341 ara has it all. Monthly Notices of the Royal Astronomical Society. (In Press)

Record type: Article

Abstract

V341 Ara was recently recognised as one of the closest (d ~ 150 pc) and brightest (V~ 10) nova-like cataclysmic variables. This unique system is surrounded by a bright emission nebula, likely to be the remnant of a recent nova eruption. Embedded within this nebula is a prominent bow-shock, where the system's accretion disc wind runs into its own nova shell. In order to establish its fundamental properties, we present the first comprehensive multi-wavelength study of the system. Long-term photometry reveals quasi-periodic, super-orbital variations with a characteristic time-scale of 10-16 days and typical amplitude of ~1 mag. High-cadence photometry from TESS reveals for the first time both the orbital period and a "negative superhump" period. The latter is usually interpreted as the signature of a tilted accretion disc. We propose a recently developed disc instability model as a plausible explanation for the photometric behaviour. In our spectroscopic data, we clearly detect anti-phased absorption and emission line components. Their radial velocities suggest a high mass ratio, which in turn implies an unusually low white dwarf mass. We also constrain the wind mass-loss rate of the system from the spatially resolved [O iii] emission produced in the bow-shock; this can be used to test and calibrate accretion disc wind models. We suggest a possible association between V341 Ara and a "guest star" mentioned in Chinese historical records in AD1240. If this marks the date of the system's nova eruption, V341 Ara would be the oldest recovered nova of its class and an excellent laboratory for testing nova theory.

Text
2008.07462v1 - Accepted Manuscript
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Accepted/In Press date: 17 August 2020
Keywords: astro-ph.SR, astro-ph.HE

Identifiers

Local EPrints ID: 443666
URI: http://eprints.soton.ac.uk/id/eprint/443666
ISSN: 0035-8711
PURE UUID: 19797c95-da84-42ef-af72-80efb86ff8a3
ORCID for D. Altamirano: ORCID iD orcid.org/0000-0002-3422-0074
ORCID for D. R. A. Williams: ORCID iD orcid.org/0000-0001-7361-0246

Catalogue record

Date deposited: 08 Sep 2020 16:30
Last modified: 25 Feb 2021 02:43

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Contributors

Author: C. Knigge
Author: J. A. Acosta-Pulido
Author: D. Altamirano ORCID iD
Author: S. del Palacio
Author: J. V. Hernandez Santisteban
Author: M. Pahari
Author: P. Rodriguez-Gil
Author: C. Belardi
Author: D. A. H. Buckley
Author: M. R. Burleigh
Author: M. Childress
Author: R. P. Fender
Author: D. M. Hewitt
Author: D. J. James
Author: R. B. Kuhn
Author: N. P. M. Kuin
Author: J. Pepper
Author: A. A. Ponomareva
Author: M. L. Pretorius
Author: J. E. Rodríguez
Author: K. G. Stassun
Author: D. R. A. Williams ORCID iD
Author: P. A. Woudt

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