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; B. Miszalski; R. Napiwotzki; D. Steeghs; R. Wesson; A. A. Zijlstra; David 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, B. Miszalski, R. Napiwotzki, D. Steeghs, R. Wesson, A. A. Zijlstra, David Jones, T. Liimets, T. Muñoz-Darias, S. Pyrzas, M. M. Rubio-Díez

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

39 Citations (Scopus)

Abstract

We present time-resolved optical spectroscopy of V458 Vulpeculae (Nova Vul 2007 No. 1) spread over a period of 15 months starting 301d after its discovery. Our data reveal radial-velocity variations in the HeII λ5412 and HeII λ4686 emission lines. A period analysis of the radial-velocity curves resulted in a period of 98.09647 ± 0.00025min (0.06812255 ± 0.00000017d) 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 ≳ 1.0 M_⊙) 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
Pages (from-to)	L21-L25
Number of pages	5
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 - 2010
Externally published	Yes

Keywords

accretion, accretion discs
binaries: close
stars: individual: V458 Vul
novae, cataclysmic variables

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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), L21-L25. https://doi.org/10.1111/j.1745-3933.2010.00895.x

@article{8c39c5f77de74a79b3d44d00fd751474,

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 301d after its discovery. Our data reveal radial-velocity variations in the HeII λ5412 and HeII λ4686 emission lines. A period analysis of the radial-velocity curves resulted in a period of 98.09647 ± 0.00025min (0.06812255 ± 0.00000017d) 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 ≳ 1.0 M⊙) 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.",

keywords = "accretion, accretion discs, binaries: close, stars: individual: V458 Vul, novae, cataclysmic variables",

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 B. Miszalski and R. Napiwotzki and D. Steeghs and R. Wesson and Zijlstra, {A. A.} and David Jones and T. Liimets and T. Mu{\~n}oz-Darias and S. Pyrzas and Rubio-D{\'i}ez, {M. M.}",

year = "2010",

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

language = "English",

volume = "407",

pages = "L21--L25",

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

issn = "1745-3933",

publisher = "Oxford University Press",

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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, pp. L21-L25. 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, B.

AU - Napiwotzki, R.

AU - Steeghs, D.

AU - Wesson, R.

AU - Zijlstra, A. A.

AU - Jones, David

AU - Liimets, T.

AU - Muñoz-Darias, T.

AU - Pyrzas, S.

AU - Rubio-Díez, M. M.

PY - 2010

Y1 - 2010

N2 - We present time-resolved optical spectroscopy of V458 Vulpeculae (Nova Vul 2007 No. 1) spread over a period of 15 months starting 301d after its discovery. Our data reveal radial-velocity variations in the HeII λ5412 and HeII λ4686 emission lines. A period analysis of the radial-velocity curves resulted in a period of 98.09647 ± 0.00025min (0.06812255 ± 0.00000017d) 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 ≳ 1.0 M⊙) 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 301d after its discovery. Our data reveal radial-velocity variations in the HeII λ5412 and HeII λ4686 emission lines. A period analysis of the radial-velocity curves resulted in a period of 98.09647 ± 0.00025min (0.06812255 ± 0.00000017d) 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 ≳ 1.0 M⊙) 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 - stars: individual: V458 Vul

KW - novae, cataclysmic variables

U2 - 10.1111/j.1745-3933.2010.00895.x

DO - 10.1111/j.1745-3933.2010.00895.x

M3 - Article

SN - 1745-3933

VL - 407

SP - L21-L25

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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