Light-curve Instabilities of β Lyrae Observed by the BRITE Satellites

Slavek M. Rucinski, Andrzej Pigulski, Adam Popowicz, Rainer Kuschnig, Szymon Kozłowski, Anthony F.J. Moffat, Krešimir Pavlovski, Gerald Handler, H. Pablo, G. A. Wade, Werner W. Weiss, Konstanze Zwintz

Publikation: Beitrag in einer FachzeitschriftArtikelForschungBegutachtung

Abstract

Photometric instabilities of β Lyrae (β Lyr) were observed in 2016 by two red-filter BRITE satellites over more than 10 revolutions of the binary, with ∼100 minute sampling. Analysis of the time series shows that flares or fading events take place typically three to five times per binary orbit. The amplitudes of the disturbances (relative to the mean light curve, in units of the maximum out-of-eclipse light flux, f.u.) are characterized by a Gaussian distribution with σ = 0.0130 ±0.0004 f.u. Most of the disturbances appear to be random, with a tendency to remain for one or a few orbital revolutions, sometimes changing from brightening to fading or the reverse. Phases just preceding the center of the deeper eclipse showed the most scatter while phases around the secondary eclipse were the quietest. This implies that the invisible companion is the most likely source of the instabilities. Wavelet transform analysis showed the domination of the variability scales at phase intervals 0.05-0.3 (0.65-4 days), with the shorter (longer) scales dominating in numbers (variability power) in this range. The series can be well described as a stochastic Gaussian process with the signal at short timescales showing a slightly stronger correlation than red noise. The signal decorrelation timescale, τ = (0.068 ±0.018) in phase or (0.88 ±0.23) days, appears to follow the same dependence on the accretor mass as that observed for active galactic nucleus and quasi-stellar object masses five to nine orders of magnitude larger than the β Lyr torus-hidden component.

Spracheenglisch
Aufsatznummer12
FachzeitschriftAstronomical Journal
Jahrgang156
Ausgabennummer1
DOIs
StatusVeröffentlicht - 1 Jul 2018

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eclipses
light curve
fading
timescale
disturbance
disturbances
wavelet
transform
time series
filter
normal density functions
active galactic nuclei
wavelet analysis
flares
sampling
tendencies
intervals
orbits
filters
orbitals

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    ASJC Scopus subject areas

    • !!Astronomy and Astrophysics
    • !!Space and Planetary Science

    Dies zitieren

    Rucinski, S. M., Pigulski, A., Popowicz, A., Kuschnig, R., Kozłowski, S., Moffat, A. F. J., ... Zwintz, K. (2018). Light-curve Instabilities of β Lyrae Observed by the BRITE Satellites. Astronomical Journal, 156(1), [12]. https://doi.org/10.3847/1538-3881/aac38b

    Light-curve Instabilities of β Lyrae Observed by the BRITE Satellites. / Rucinski, Slavek M.; Pigulski, Andrzej; Popowicz, Adam; Kuschnig, Rainer; Kozłowski, Szymon; Moffat, Anthony F.J.; Pavlovski, Krešimir; Handler, Gerald; Pablo, H.; Wade, G. A.; Weiss, Werner W.; Zwintz, Konstanze.

    in: Astronomical Journal, Jahrgang 156, Nr. 1, 12, 01.07.2018.

    Publikation: Beitrag in einer FachzeitschriftArtikelForschungBegutachtung

    Rucinski, SM, Pigulski, A, Popowicz, A, Kuschnig, R, Kozłowski, S, Moffat, AFJ, Pavlovski, K, Handler, G, Pablo, H, Wade, GA, Weiss, WW & Zwintz, K 2018, 'Light-curve Instabilities of β Lyrae Observed by the BRITE Satellites', Astronomical Journal, Jg. 156, Nr. 1, 12. https://doi.org/10.3847/1538-3881/aac38b
    Rucinski SM, Pigulski A, Popowicz A, Kuschnig R, Kozłowski S, Moffat AFJ et al. Light-curve Instabilities of β Lyrae Observed by the BRITE Satellites. Astronomical Journal. 2018 Jul 1;156(1). 12. https://doi.org/10.3847/1538-3881/aac38b
    Rucinski, Slavek M. ; Pigulski, Andrzej ; Popowicz, Adam ; Kuschnig, Rainer ; Kozłowski, Szymon ; Moffat, Anthony F.J. ; Pavlovski, Krešimir ; Handler, Gerald ; Pablo, H. ; Wade, G. A. ; Weiss, Werner W. ; Zwintz, Konstanze. / Light-curve Instabilities of β Lyrae Observed by the BRITE Satellites. in: Astronomical Journal. 2018 ; Jahrgang 156, Nr. 1.
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    abstract = "Photometric instabilities of β Lyrae (β Lyr) were observed in 2016 by two red-filter BRITE satellites over more than 10 revolutions of the binary, with ∼100 minute sampling. Analysis of the time series shows that flares or fading events take place typically three to five times per binary orbit. The amplitudes of the disturbances (relative to the mean light curve, in units of the maximum out-of-eclipse light flux, f.u.) are characterized by a Gaussian distribution with σ = 0.0130 ±0.0004 f.u. Most of the disturbances appear to be random, with a tendency to remain for one or a few orbital revolutions, sometimes changing from brightening to fading or the reverse. Phases just preceding the center of the deeper eclipse showed the most scatter while phases around the secondary eclipse were the quietest. This implies that the invisible companion is the most likely source of the instabilities. Wavelet transform analysis showed the domination of the variability scales at phase intervals 0.05-0.3 (0.65-4 days), with the shorter (longer) scales dominating in numbers (variability power) in this range. The series can be well described as a stochastic Gaussian process with the signal at short timescales showing a slightly stronger correlation than red noise. The signal decorrelation timescale, τ = (0.068 ±0.018) in phase or (0.88 ±0.23) days, appears to follow the same dependence on the accretor mass as that observed for active galactic nucleus and quasi-stellar object masses five to nine orders of magnitude larger than the β Lyr torus-hidden component.",
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    T1 - Light-curve Instabilities of β Lyrae Observed by the BRITE Satellites

    AU - Rucinski, Slavek M.

    AU - Pigulski, Andrzej

    AU - Popowicz, Adam

    AU - Kuschnig, Rainer

    AU - Kozłowski, Szymon

    AU - Moffat, Anthony F.J.

    AU - Pavlovski, Krešimir

    AU - Handler, Gerald

    AU - Pablo, H.

    AU - Wade, G. A.

    AU - Weiss, Werner W.

    AU - Zwintz, Konstanze

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    N2 - Photometric instabilities of β Lyrae (β Lyr) were observed in 2016 by two red-filter BRITE satellites over more than 10 revolutions of the binary, with ∼100 minute sampling. Analysis of the time series shows that flares or fading events take place typically three to five times per binary orbit. The amplitudes of the disturbances (relative to the mean light curve, in units of the maximum out-of-eclipse light flux, f.u.) are characterized by a Gaussian distribution with σ = 0.0130 ±0.0004 f.u. Most of the disturbances appear to be random, with a tendency to remain for one or a few orbital revolutions, sometimes changing from brightening to fading or the reverse. Phases just preceding the center of the deeper eclipse showed the most scatter while phases around the secondary eclipse were the quietest. This implies that the invisible companion is the most likely source of the instabilities. Wavelet transform analysis showed the domination of the variability scales at phase intervals 0.05-0.3 (0.65-4 days), with the shorter (longer) scales dominating in numbers (variability power) in this range. The series can be well described as a stochastic Gaussian process with the signal at short timescales showing a slightly stronger correlation than red noise. The signal decorrelation timescale, τ = (0.068 ±0.018) in phase or (0.88 ±0.23) days, appears to follow the same dependence on the accretor mass as that observed for active galactic nucleus and quasi-stellar object masses five to nine orders of magnitude larger than the β Lyr torus-hidden component.

    AB - Photometric instabilities of β Lyrae (β Lyr) were observed in 2016 by two red-filter BRITE satellites over more than 10 revolutions of the binary, with ∼100 minute sampling. Analysis of the time series shows that flares or fading events take place typically three to five times per binary orbit. The amplitudes of the disturbances (relative to the mean light curve, in units of the maximum out-of-eclipse light flux, f.u.) are characterized by a Gaussian distribution with σ = 0.0130 ±0.0004 f.u. Most of the disturbances appear to be random, with a tendency to remain for one or a few orbital revolutions, sometimes changing from brightening to fading or the reverse. Phases just preceding the center of the deeper eclipse showed the most scatter while phases around the secondary eclipse were the quietest. This implies that the invisible companion is the most likely source of the instabilities. Wavelet transform analysis showed the domination of the variability scales at phase intervals 0.05-0.3 (0.65-4 days), with the shorter (longer) scales dominating in numbers (variability power) in this range. The series can be well described as a stochastic Gaussian process with the signal at short timescales showing a slightly stronger correlation than red noise. The signal decorrelation timescale, τ = (0.068 ±0.018) in phase or (0.88 ±0.23) days, appears to follow the same dependence on the accretor mass as that observed for active galactic nucleus and quasi-stellar object masses five to nine orders of magnitude larger than the β Lyr torus-hidden component.

    KW - binaries: close

    KW - binaries: eclipsing

    KW - stars: individual (β Lyr)

    KW - techniques: photometric

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