The orbital period of V458 Vulpeculae, a post-double common-envelope nova

P. Rodríguez-Gil; M. Santander-García; C. Knigge; R. L M Corradi; B. T. Gänsicke; M. J. Barlow; J. J. Drake; J. Drew; Brent Miszalski; R. Napiwotzki; D. Steeghs; Roger Wesson; Albert Auke Zijlstra; D. Jones; T. Liimets; T. Muñoz-Darias; S. Pyrzas; M. M. Rubio-Díez

doi:10.1111/j.1745-3933.2010.00895.x

The orbital period of V458 Vulpeculae, a post-double common-envelope nova

P. Rodríguez-Gil, M. Santander-García, C. Knigge, R. L M Corradi, B. T. Gänsicke, M. J. Barlow, J. J. Drake, J. Drew, Brent Miszalski, R. Napiwotzki, D. Steeghs, Roger Wesson, Albert Auke Zijlstra, D. Jones, T. Liimets, T. Muñoz-Darias, S. Pyrzas, M. M. Rubio-Díez

Research output: Contribution to journal › Letter › Other › peer-review

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Abstract

We present time-resolved optical spectroscopy of V458 Vulpeculae (Nova Vul 2007 No. 1) spread over a period of 15 months starting 301 d after its discovery. Our data reveal radial-velocity variations in the He II λ5412 and He II λ4686 emission lines. A period analysis of the radial-velocity curves resulted in a period of 98.09647 ± 0.000 25 min (0.068 122 55 ± 0.000000 17 d) which we identify with the orbital period of the binary system. V458 Vul is therefore the planetary nebula central binary star with the shortest period known. We explore the possibility of the system being composed of a relatively massive white dwarf (M₁ ≳ 1.0M⊙) accreting matter from a post-asymptotic giant branch star which produced the planetary nebula observed. In this scenario, the central binary system therefore underwent two common-envelope episodes. A combination of previous photoionization modelling of the nebular spectra, post-asymptotic giant branch evolutionary tracks and the orbital period favour a mass of M₂ ~ 0.6 M⊙ for the donor star. Therefore, the total mass of the system may exceed the Chandrasekhar mass, which makes V458 Vul a Type Ia supernova progenitor candidate.

Original language	English
Journal	Monthly Notices of the Royal Astronomical Society: Letters
Volume	407
Issue number	1
DOIs	https://doi.org/10.1111/j.1745-3933.2010.00895.x
Publication status	Published - Sept 2010
Externally published	Yes

Keywords

Accretion, accretion discs
Binaries: close
Novae, cataclysmic variables
Stars: individual: V458 Vul

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10.1111/j.1745-3933.2010.00895.x

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Rodríguez-Gil, P., Santander-García, M., Knigge, C., Corradi, R. L. M., Gänsicke, B. T., Barlow, M. J., Drake, J. J., Drew, J., Miszalski, B., Napiwotzki, R., Steeghs, D., Wesson, R., Zijlstra, A. A., Jones, D., Liimets, T., Muñoz-Darias, T., Pyrzas, S., & Rubio-Díez, M. M. (2010). The orbital period of V458 Vulpeculae, a post-double common-envelope nova. Monthly Notices of the Royal Astronomical Society: Letters, 407(1). https://doi.org/10.1111/j.1745-3933.2010.00895.x

@article{8b1f03263ebb4d78a8ca6c540b67351f,

title = "The orbital period of V458 Vulpeculae, a post-double common-envelope nova",

abstract = "We present time-resolved optical spectroscopy of V458 Vulpeculae (Nova Vul 2007 No. 1) spread over a period of 15 months starting 301 d after its discovery. Our data reveal radial-velocity variations in the He II λ5412 and He II λ4686 emission lines. A period analysis of the radial-velocity curves resulted in a period of 98.09647 ± 0.000 25 min (0.068 122 55 ± 0.000000 17 d) which we identify with the orbital period of the binary system. V458 Vul is therefore the planetary nebula central binary star with the shortest period known. We explore the possibility of the system being composed of a relatively massive white dwarf (M1 ≳ 1.0M⊙) accreting matter from a post-asymptotic giant branch star which produced the planetary nebula observed. In this scenario, the central binary system therefore underwent two common-envelope episodes. A combination of previous photoionization modelling of the nebular spectra, post-asymptotic giant branch evolutionary tracks and the orbital period favour a mass of M2 \textasciitilde{} 0.6 M⊙ for the donor star. Therefore, the total mass of the system may exceed the Chandrasekhar mass, which makes V458 Vul a Type Ia supernova progenitor candidate. ",

keywords = "Accretion, accretion discs, Binaries: close, Novae, cataclysmic variables, Stars: individual: V458 Vul",

author = "P. Rodr{\'i}guez-Gil and M. Santander-Garc{\'i}a and C. Knigge and Corradi, \{R. L M\} and G{\"a}nsicke, \{B. T.\} and Barlow, \{M. J.\} and Drake, \{J. J.\} and J. Drew and Brent Miszalski and R. Napiwotzki and D. Steeghs and Roger Wesson and Zijlstra, \{Albert Auke\} and D. Jones and T. Liimets and T. Mu{\~n}oz-Darias and S. Pyrzas and Rubio-D{\'i}ez, \{M. M.\}",

year = "2010",

month = sep,

doi = "10.1111/j.1745-3933.2010.00895.x",

language = "English",

volume = "407",

journal = "Monthly Notices of the Royal Astronomical Society: Letters",

issn = "1745-3933",

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Rodríguez-Gil, P, Santander-García, M, Knigge, C, Corradi, RLM, Gänsicke, BT, Barlow, MJ, Drake, JJ, Drew, J, Miszalski, B, Napiwotzki, R, Steeghs, D, Wesson, R, Zijlstra, AA, Jones, D, Liimets, T, Muñoz-Darias, T, Pyrzas, S & Rubio-Díez, MM 2010, 'The orbital period of V458 Vulpeculae, a post-double common-envelope nova', Monthly Notices of the Royal Astronomical Society: Letters, vol. 407, no. 1. https://doi.org/10.1111/j.1745-3933.2010.00895.x

TY - JOUR

T1 - The orbital period of V458 Vulpeculae, a post-double common-envelope nova

AU - Rodríguez-Gil, P.

AU - Santander-García, M.

AU - Knigge, C.

AU - Corradi, R. L M

AU - Gänsicke, B. T.

AU - Barlow, M. J.

AU - Drake, J. J.

AU - Drew, J.

AU - Miszalski, Brent

AU - Napiwotzki, R.

AU - Steeghs, D.

AU - Wesson, Roger

AU - Zijlstra, Albert Auke

AU - Jones, D.

AU - Liimets, T.

AU - Muñoz-Darias, T.

AU - Pyrzas, S.

AU - Rubio-Díez, M. M.

PY - 2010/9

Y1 - 2010/9

N2 - We present time-resolved optical spectroscopy of V458 Vulpeculae (Nova Vul 2007 No. 1) spread over a period of 15 months starting 301 d after its discovery. Our data reveal radial-velocity variations in the He II λ5412 and He II λ4686 emission lines. A period analysis of the radial-velocity curves resulted in a period of 98.09647 ± 0.000 25 min (0.068 122 55 ± 0.000000 17 d) which we identify with the orbital period of the binary system. V458 Vul is therefore the planetary nebula central binary star with the shortest period known. We explore the possibility of the system being composed of a relatively massive white dwarf (M1 ≳ 1.0M⊙) accreting matter from a post-asymptotic giant branch star which produced the planetary nebula observed. In this scenario, the central binary system therefore underwent two common-envelope episodes. A combination of previous photoionization modelling of the nebular spectra, post-asymptotic giant branch evolutionary tracks and the orbital period favour a mass of M2 ~ 0.6 M⊙ for the donor star. Therefore, the total mass of the system may exceed the Chandrasekhar mass, which makes V458 Vul a Type Ia supernova progenitor candidate.

AB - We present time-resolved optical spectroscopy of V458 Vulpeculae (Nova Vul 2007 No. 1) spread over a period of 15 months starting 301 d after its discovery. Our data reveal radial-velocity variations in the He II λ5412 and He II λ4686 emission lines. A period analysis of the radial-velocity curves resulted in a period of 98.09647 ± 0.000 25 min (0.068 122 55 ± 0.000000 17 d) which we identify with the orbital period of the binary system. V458 Vul is therefore the planetary nebula central binary star with the shortest period known. We explore the possibility of the system being composed of a relatively massive white dwarf (M1 ≳ 1.0M⊙) accreting matter from a post-asymptotic giant branch star which produced the planetary nebula observed. In this scenario, the central binary system therefore underwent two common-envelope episodes. A combination of previous photoionization modelling of the nebular spectra, post-asymptotic giant branch evolutionary tracks and the orbital period favour a mass of M2 ~ 0.6 M⊙ for the donor star. Therefore, the total mass of the system may exceed the Chandrasekhar mass, which makes V458 Vul a Type Ia supernova progenitor candidate.

KW - Accretion, accretion discs

KW - Binaries: close

KW - Novae, cataclysmic variables

KW - Stars: individual: V458 Vul

UR - https://www.scopus.com/pages/publications/79951712583

U2 - 10.1111/j.1745-3933.2010.00895.x

DO - 10.1111/j.1745-3933.2010.00895.x

M3 - Letter

AN - SCOPUS:79951712583

SN - 1745-3933

VL - 407

JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

IS - 1

ER -

The orbital period of V458 Vulpeculae, a post-double common-envelope nova

Abstract

Keywords

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