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dc.contributor.author
Castro Segura, N.
dc.contributor.author
Knigge, C.
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Acosta Pulido, J. A.
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Altamirano, D.
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del Palacio, Santiago
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Hernández Santisteban, Juan V.
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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.
dc.date.available
2021-08-19T15:01:10Z
dc.date.issued
2021-02
dc.identifier.citation
Castro Segura, N.; Knigge, C.; Acosta Pulido, J. A.; Altamirano, D.; del Palacio, Santiago; et al.; Bow shocks, nova shells, disc winds and tilted discs: The nova-like V341 Ara has it all; Wiley Blackwell Publishing, Inc; Monthly Notices of the Royal Astronomical Society; 501; 2; 2-2021; 1951-1969
dc.identifier.issn
0035-8711
dc.identifier.uri
http://hdl.handle.net/11336/138522
dc.description.abstract
V341 Ara was recently recognized 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 multiwavelength study of the system. Long-term photometry reveals quasi-periodic, super-orbital variations with a characteristic time-scale of 10-16 d and typical amplitude of ~1 mag. High-cadence photometry from theTransiting Exoplanet Survey Satellite (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 antiphased 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 AD 1240. 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.
dc.format
application/pdf
dc.language.iso
eng
dc.publisher
Wiley Blackwell Publishing, Inc
dc.rights
info:eu-repo/semantics/openAccess
dc.rights.uri
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.subject
ACCRETION
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ACCRETION DISCS
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BINARIES: SPECTROSCOPIC
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NOVAE, CATACLYSMIC VARIABLES
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SHOCK WAVES
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WINDS, OUTFLOWS
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Astronomía
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Ciencias Físicas
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CIENCIAS NATURALES Y EXACTAS
dc.title
Bow shocks, nova shells, disc winds and tilted discs: The nova-like V341 Ara has it all
dc.type
info:eu-repo/semantics/article
dc.type
info:ar-repo/semantics/artículo
dc.type
info:eu-repo/semantics/publishedVersion
dc.date.updated
2021-08-17T15:53:14Z
dc.journal.volume
501
dc.journal.number
2
dc.journal.pagination
1951-1969
dc.journal.pais
Reino Unido
dc.description.fil
Fil: Castro Segura, N.. University of Southampton; Reino Unido
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Fil: Knigge, C.. University of Southampton; Reino Unido
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Fil: Acosta Pulido, J. A.. Universidad de La Laguna; España
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Fil: Altamirano, D.. University of Southampton; Reino Unido
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Fil: del Palacio, Santiago. Provincia de Buenos Aires. Gobernación. Comisión de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomía; Argentina
dc.description.fil
Fil: Hernández Santisteban, Juan V.. University of St. Andrews; Reino Unido
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Fil: Pahari, M.. University of Southampton; Reino Unido
dc.description.fil
Fil: Rodriguez-Gil, P.. Universidad de La Laguna; España
dc.description.fil
Fil: Belardi, C.. University of Southampton; Reino Unido
dc.description.fil
Fil: Buckley, D. A. H.. South African Astronomical Observatory; Sudáfrica
dc.description.fil
Fil: Burleigh, M. R.. University of Southampton; Reino Unido
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Fil: Childress, M.. University of Southampton; Reino Unido
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Fil: Fender, R.P.. University of Oxford; Reino Unido
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Fil: Hewitt, D. M.. South African Astronomical Observatory; Sudáfrica
dc.description.fil
Fil: James, D.J.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
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Fil: Kuhn, R.B.. South African Astronomical Observatory; Sudáfrica
dc.description.fil
Fil: Kuin, N.P.M.. Ucl Mullard Space Science Laboratory; Reino Unido
dc.description.fil
Fil: Pepper, J.. Lehigh University; Estados Unidos
dc.description.fil
Fil: Ponomareva, A. A.. The Australian National University; Australia. University of Oxford; Reino Unido
dc.description.fil
Fil: Pretorius, M. L.. South African Astronomical Observatory; Sudáfrica
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Fil: Rodríguez, J.E.. Harvard-Smithsonian Center for Astrophysics; Estados Unidos
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Fil: Stassun, K. G.. Vanderbilt University; Estados Unidos
dc.description.fil
Fil: Williams, D. R. A.. University of Manchester; Reino Unido. University of Oxford; Reino Unido
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Fil: Woudt, P. A.. University Of Cape Town; Sudáfrica
dc.journal.title
Monthly Notices of the Royal Astronomical Society
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/doi/http://dx.doi.org/10.1093/mnras/staa2516
dc.relation.alternativeid
info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/mnras/article-abstract/501/2/1951/6059035
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