SUZAKU OBSERVATION OF THE CLASSICAL NOVA V2491 Cyg IN QUIESCENCE

Zemko, P.; Mukai, K.

doi:10.1088/0004-637X/807/1/61

Title: SUZAKU OBSERVATION OF THE CLASSICAL NOVA V2491 Cyg IN QUIESCENCE

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Abstract

We present the Suzaku XIS observation of V2491 Cyg (Nova Cyg 2008 No. 2) obtained in quiescence, more than two years after the outburst. The nova was detected as a very luminous source in a wide spectral range from soft to hard X-rays. A very soft blackbody-like component peaking at 0.5 keV indicates that we observe either remaining, localized hydrogen burning on the surface of the white dwarf, or accretion onto a magnetized polar cap. In the second case, V2491 Cyg is a candidate “soft intermediate polar.” We obtained the best fit for the X-ray spectra with several components: two of thermal plasma, a blackbody and a complex absorber. The latter is typical of intermediate polars. The X-ray light curve shows a modulation with a period of ∼38 minutes. The amplitude of this modulation is strongly energy-dependent and reaches a maximum in the range 0.8–2.0 keV. We discuss the origin of the X-ray emission and pulsations, and the likelihood of the intermediate polar scenario.

Authors:

Zemko, P. ^[1]; Mukai, K. ^[2]

Department of Physics and Astronomy, Università di Padova, vicolo dell’ Osservatorio 3, I-35122 Padova (Italy)
CRESST and X-ray Astrophysics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States)

Publication Date:: Wed Jul 01 00:00:00 EDT 2015

OSTI Identifier:: 22522208

Resource Type:: Journal Article

Journal Name:: Astrophysical Journal

Additional Journal Information:: Journal Volume: 807; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X

Country of Publication:: United States

Language:: English

Subject:: 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; DIAGRAMS; ENERGY DEPENDENCE; HARD X RADIATION; HYDROGEN BURNING; KEV RANGE; MODULATION; NOVAE; PLASMA; PULSATIONS; SURFACES; VISIBLE RADIATION; WHITE DWARF STARS; X-RAY SPECTRA

Citation Formats


                    Zemko, P., Mukai, K., and Orio, M., E-mail: polina.zemko@studenti.unipd.it, E-mail: koji.mukai@umbc.edu, E-mail: marina.orio@oapd.inaf.it. SUZAKU OBSERVATION OF THE CLASSICAL NOVA V2491 Cyg IN QUIESCENCE.  United States: N. p., 2015. 
        Web.  doi:10.1088/0004-637X/807/1/61.

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                    Zemko, P., Mukai, K., & Orio, M., E-mail: polina.zemko@studenti.unipd.it, E-mail: koji.mukai@umbc.edu, E-mail: marina.orio@oapd.inaf.it. SUZAKU OBSERVATION OF THE CLASSICAL NOVA V2491 Cyg IN QUIESCENCE.  United States.  https://doi.org/10.1088/0004-637X/807/1/61

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                    Zemko, P., Mukai, K., and Orio, M., E-mail: polina.zemko@studenti.unipd.it, E-mail: koji.mukai@umbc.edu, E-mail: marina.orio@oapd.inaf.it. 2015.  
        "SUZAKU OBSERVATION OF THE CLASSICAL NOVA V2491 Cyg IN QUIESCENCE".  United States.  https://doi.org/10.1088/0004-637X/807/1/61.

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@article{osti_22522208,

  title        = {SUZAKU OBSERVATION OF THE CLASSICAL NOVA V2491 Cyg IN QUIESCENCE},

  author       = {Zemko, P. and Mukai, K. and Orio, M., E-mail: polina.zemko@studenti.unipd.it, E-mail: koji.mukai@umbc.edu, E-mail: marina.orio@oapd.inaf.it},

  abstractNote = {We present the Suzaku XIS observation of V2491 Cyg (Nova Cyg 2008 No. 2) obtained in quiescence, more than two years after the outburst. The nova was detected as a very luminous source in a wide spectral range from soft to hard X-rays. A very soft blackbody-like component peaking at 0.5 keV indicates that we observe either remaining, localized hydrogen burning on the surface of the white dwarf, or accretion onto a magnetized polar cap. In the second case, V2491 Cyg is a candidate “soft intermediate polar.” We obtained the best fit for the X-ray spectra with several components: two of thermal plasma, a blackbody and a complex absorber. The latter is typical of intermediate polars. The X-ray light curve shows a modulation with a period of ∼38 minutes. The amplitude of this modulation is strongly energy-dependent and reaches a maximum in the range 0.8–2.0 keV. We discuss the origin of the X-ray emission and pulsations, and the likelihood of the intermediate polar scenario.},

  doi          = {10.1088/0004-637X/807/1/61},

  url          = {https://www.osti.gov/biblio/22522208},
  journal      = {Astrophysical Journal},

  issn         = {0004-637X},

  number       = 1,

  volume       = 807,

  place        = {United States},

  year         = {Wed Jul 01 00:00:00 EDT 2015},

  month        = {Wed Jul 01 00:00:00 EDT 2015}

}

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