High-cadence time-series photometry of v1647 Orionis

Fabienne A. Bastien, Keivan G. Stassun, David A. Weintraub

Research output: Contribution to journalArticle

4 Citations (Scopus)

Abstract

We present high-cadence (1-10hr-1) time-series photometry of the eruptive young variable star V1647 Orionis during its 2003-2004 and 2008-2009 outbursts. The 2003 light curve was obtained mid-outburst at the phase of steepest luminosity increase of the system, during which time the accretion rate of the system was presumably continuing to increase toward its maximum rate. The 2009 light curve was obtained after the system luminosity had plateaued, presumably when the rate of accretion had also plateaued. We detect a "flicker noise" signature in the power spectrum of the light curves, which may suggest that the stellar magnetosphere continued to interact with the accretion disk during each outburst event. Only the 2003 power spectrum, however, evinces a significant signal with a period of 0.13days. While the 0.13day period cannot be attributed to the stellar rotation period, we show that it may plausibly be due to short-lived radial oscillations of the star, possibly caused by the surge in the accretion rate.

Original languageEnglish (US)
Article number141
JournalAstronomical Journal
Volume142
Issue number4
DOIs
StatePublished - Oct 1 2011

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photometry
accretion
outburst
time series
light curve
power spectra
stellar magnetospheres
luminosity
stellar rotation
flicker
variable stars
accretion disks
magnetosphere
oscillation
signatures
stars
oscillations
rate

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Bastien, Fabienne A. ; Stassun, Keivan G. ; Weintraub, David A. / High-cadence time-series photometry of v1647 Orionis. In: Astronomical Journal. 2011 ; Vol. 142, No. 4.
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abstract = "We present high-cadence (1-10hr-1) time-series photometry of the eruptive young variable star V1647 Orionis during its 2003-2004 and 2008-2009 outbursts. The 2003 light curve was obtained mid-outburst at the phase of steepest luminosity increase of the system, during which time the accretion rate of the system was presumably continuing to increase toward its maximum rate. The 2009 light curve was obtained after the system luminosity had plateaued, presumably when the rate of accretion had also plateaued. We detect a {"}flicker noise{"} signature in the power spectrum of the light curves, which may suggest that the stellar magnetosphere continued to interact with the accretion disk during each outburst event. Only the 2003 power spectrum, however, evinces a significant signal with a period of 0.13days. While the 0.13day period cannot be attributed to the stellar rotation period, we show that it may plausibly be due to short-lived radial oscillations of the star, possibly caused by the surge in the accretion rate.",
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High-cadence time-series photometry of v1647 Orionis. / Bastien, Fabienne A.; Stassun, Keivan G.; Weintraub, David A.

In: Astronomical Journal, Vol. 142, No. 4, 141, 01.10.2011.

Research output: Contribution to journalArticle

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T1 - High-cadence time-series photometry of v1647 Orionis

AU - Bastien, Fabienne A.

AU - Stassun, Keivan G.

AU - Weintraub, David A.

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N2 - We present high-cadence (1-10hr-1) time-series photometry of the eruptive young variable star V1647 Orionis during its 2003-2004 and 2008-2009 outbursts. The 2003 light curve was obtained mid-outburst at the phase of steepest luminosity increase of the system, during which time the accretion rate of the system was presumably continuing to increase toward its maximum rate. The 2009 light curve was obtained after the system luminosity had plateaued, presumably when the rate of accretion had also plateaued. We detect a "flicker noise" signature in the power spectrum of the light curves, which may suggest that the stellar magnetosphere continued to interact with the accretion disk during each outburst event. Only the 2003 power spectrum, however, evinces a significant signal with a period of 0.13days. While the 0.13day period cannot be attributed to the stellar rotation period, we show that it may plausibly be due to short-lived radial oscillations of the star, possibly caused by the surge in the accretion rate.

AB - We present high-cadence (1-10hr-1) time-series photometry of the eruptive young variable star V1647 Orionis during its 2003-2004 and 2008-2009 outbursts. The 2003 light curve was obtained mid-outburst at the phase of steepest luminosity increase of the system, during which time the accretion rate of the system was presumably continuing to increase toward its maximum rate. The 2009 light curve was obtained after the system luminosity had plateaued, presumably when the rate of accretion had also plateaued. We detect a "flicker noise" signature in the power spectrum of the light curves, which may suggest that the stellar magnetosphere continued to interact with the accretion disk during each outburst event. Only the 2003 power spectrum, however, evinces a significant signal with a period of 0.13days. While the 0.13day period cannot be attributed to the stellar rotation period, we show that it may plausibly be due to short-lived radial oscillations of the star, possibly caused by the surge in the accretion rate.

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