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Constraining the angular momentum evolution of V455 Andromedae
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Mukadam, Anjum S., Pyrzas, Stylianos, Townsley, D. M., Gänsicke, B. T. (Boris T.), Hermes, J. J., Szkody, Paula, Kemp, Jonathan, Patterson, J., Ding, Claire, Wolf, Katie, Gemma, Marina, Karamehmetoglu, Emir and Rock, John (2016) Constraining the angular momentum evolution of V455 Andromedae. The Astrophysical Journal, 821 (1). p. 14. doi:10.3847/0004-637X/821/1/14 ISSN 0004-637X.
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Official URL: http://dx.doi.org/10.3847/0004-637X/821/1/14
Abstract
Time-series photometry on the cataclysmic variable V455 Andromedae (hereafter V455 And, HS 2331+3905) reveals a rotation period shorter than the orbital period, implying the presence of a magnetic field. We expect that this magnetic field channels the accreted matter from the disk toward the white dwarf poles, classifying it as an Intermediate Polar. The two polar spinning emission areas are visible in the lightcurves at the rotation period of 67.61970396 ± 0.00000072 s, and its harmonic. Using photometric observations of V455 And obtained from 2007 October to 2015, we derive 3σ upper limits to the rate of change of the spin harmonic (SH) with time to be dPSH/dt ≤ −7.5 × 10−15 s s−1 employing the O–C method, and −5.4 × 10−15 s s−1 with a direct nonlinear least squares fit. There is no significant detection of a changing spin period for the duration of 2007 October–2015. The 3σ upper limit for the rate of change of spin period with time is dPspin/dt ≤ −10.8 × 10−15 s s−1 or −0.34 μs yr−1. V455 And underwent a large-amplitude dwarf nova outburst in 2007 September. The pre-outburst data reflect a period 4.8 ± 2.2 μs longer than the best-fit post-outburst spin period. The angular momentum gained by the white dwarf from matter accreted during outburst and its slight subsequent shrinking should both cause the star to spin slightly faster after the outburst. We estimate that the change in spin period due to the outburst should be 5 μs, consistent with the empirical determination of 4.8 ± 2.2 μs (3σ upper limit of 11.4 μs).
Item Type: | Journal Article | ||||||||
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Subjects: | Q Science > QB Astronomy Q Science > QC Physics |
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Divisions: | Faculty of Science, Engineering and Medicine > Science > Physics | ||||||||
Library of Congress Subject Headings (LCSH): | Astronomical photometry , Cataclysmic variable stars, Light curves, Mass transfer | ||||||||
Journal or Publication Title: | The Astrophysical Journal | ||||||||
Publisher: | Institute of Physics Publishing, Inc. | ||||||||
ISSN: | 0004-637X | ||||||||
Official Date: | 4 April 2016 | ||||||||
Dates: |
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Volume: | 821 | ||||||||
Number: | 1 | ||||||||
Page Range: | p. 14 | ||||||||
DOI: | 10.3847/0004-637X/821/1/14 | ||||||||
Status: | Peer Reviewed | ||||||||
Publication Status: | Published | ||||||||
Access rights to Published version: | Restricted or Subscription Access | ||||||||
Date of first compliant deposit: | 13 March 2017 | ||||||||
Date of first compliant Open Access: | 14 March 2017 | ||||||||
Funder: | National Science Foundation (U.S.) (NSF), United States. National Aeronautics and Space Administration (NASA), Seventh Framework Programme (European Commission) (FP7), European Research Council (ERC) | ||||||||
Grant number: | AST-1514737 (NSF), AST-1008734 (NSF), HST-GO-12231.01-A (NASA), FP/2007-2013 (FP7), No. 320964 (ERC), HST-HF2-51357.001-A (NASA) |
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