V1647 Orionis: Optical Photometric and Spectroscopic Monitoring Through the 2003-2006 Outburst

Aspin, C.; Reipurth, Bo

doi:10.1088/0004-6256/138/4/1137

Cited by 33 publications

(32 citation statements)

References 57 publications

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“…Photometry was extracted from the images using the Starlink GAIA package. Similar imaging observations were obtained with Gemini-North/GMOS in 2004 and 2007 (Aspin & Reipurth 2009). …”

Section: Optical Imagingsupporting

confidence: 82%

“…Data were acquired on UT 2011 February 2. Photometric calibration was achieved using the field star sequence defined in Aspin & Reipurth (2009). We used the Sloan Digital Sky Survey (SDSS) r filter with a 0.…”

Section: Optical Imagingmentioning

confidence: 99%

“…Since its discovery in late 2003, soon after it had brightened by ∼5 mag, it was the subject of numerous observational studies at wavelengths spanning the electromagnetic spectrum from X-rays to radio. Rather than explicitly mention each of the 50+ papers published from 2004 to the present day, we refer the reader to Aspin & Reipurth (2009) for both a more comprehensive list and a discussion of the optical photometric and spectroscopic variability during the period 2003-2006. Soon after discovery, V1647 Ori exhibited a strong emission spectrum in both the optical and NIR. This eruption (henceforth referred to as the first outburst) lasted around two years, after which the star faded back to its pre-outburst quiescent brightness.…”

Section: Introductionmentioning

confidence: 99%

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The Continuing Outburst of V1647 Orionis: Winter/Spring 2011 Observations

Aspin

2011

The Astronomical Journal

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We present optical and near-IR observations of the young eruptive variable star V1647 Orionis which illuminates McNeil's Nebula. In late 2003, V1647 Ori was observed to brighten by around 5 mag to r = 17.7. In early 2006 the star faded back to its quiescent brightness of r ∼ 23, however in mid-2008 it brightened yet again by ∼5 mag. Our new observations, taken in early 2011, show V1647 Ori to be in an elevated photometric state with an optical brightness similar to the value found at the start of the 2003 and 2008 outbursts. Optical images taken between 2008 and 2011 suggest that the star has remained in outburst from mid-2008 to the present. Hα and the far-red Ca ii triplet lines remain in emission with Hα possessing a significant P Cygni profile. A self-consistent study of the accretion luminosity and rate using data taken in 2004, 2007, 2008, and 2011 indicates that when bright, V1647 Ori has values of 16 ± 2 L and (4 ± 2) × 10 −6 M yr −1 , respectively. We support the premise that the accretion luminosity and rate both declined by a factor of 2-3 during the 5 mag fading in 2007. However, a significant part of the fading was due to either variable extinction or dust reformation. We discuss these new observations in relation to previous published data and the classification schemes for young eruptive variables.

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“…Photometry was extracted from the images using the Starlink GAIA package. Similar imaging observations were obtained with Gemini-North/GMOS in 2004 and 2007 (Aspin & Reipurth 2009). …”

Section: Optical Imagingsupporting

confidence: 82%

Section: Optical Imagingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Continuing Outburst of V1647 Orionis: Winter/Spring 2011 Observations

Aspin

2011

The Astronomical Journal

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“…Our spectrum from 2012 April also shows a clear P Cygni profile. This is not unexpected, as a slowly evolving Hα feature was observed for V1057 Cyg (Herbig 1977) and for V1647 Ori (Aspin & Reipurth 2009). Interestingly, Lee et al (2015) found that the wind component disappeared by the end of 2012, and then the line profile exhibited a central absorption with emission wings on both sides.…”

Section: Optical and Near-ir Spectroscopysupporting

confidence: 61%

Multiwavelength study of the low-luminosity outbursting young star HBC 722

Kóspál

Ábrahám

Acosta–Pulido

et al. 2016

A&A

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Context. HBC 722 (V2493 Cyg) is a young eruptive star in outburst since 2010. Spectroscopic evidences suggest that the source is an FU Orionis-type object, with an atypically low outburst luminosity. Aims. Because it was well characterized in the pre-outburst phase, HBC 722 is one of the few FUors where we can learn about the physical changes and processes associated with the eruption, including the role of the circumstellar environment. Methods. We monitored the source in the BVRI JHK S bands from the ground, and at 3.6 and 4.5 µm from space with the Spitzer Space Telescope. We analyzed the light curves and studied how the spectral energy distribution evolved by fitting a series of steady accretion disk models at many epochs covering the outburst. We also analyzed the spectral properties of the source based on our new optical and infrared spectra, comparing our line inventory with those published in the literature for other epochs. We also mapped HBC 722 and its surroundings at millimeter wavelengths. Results. From the light curve analysis we concluded that the first peak of the outburst in 2010 September was mainly due to an abrupt increase of the accretion rate in the innermost part of the system. This was followed after a few months by a long term process, when the brightening of the source was mainly due to a gradual increase of the accretion rate and the emitting area. Our new observations show that the source is currently in a constant "plateau" phase. We found that the optical spectrum was similar both in the first peak and the following periods, but around the peak the continuum was bluer and the Hα profile changed significantly between 2012 and 2013. The source was not detected in the millimeter continuum, but we discovered a flattened molecular gas structure with a diameter of 1700 au and mass of 0.3 M ⊙ centered on HBC 722. Conclusions. While the first brightness peak could be interpreted as a rapid fall of piled-up material from the inner disk onto the star, the later monotonic flux rise suggests the outward expansion of a hot component according to the theory of Bell & Lin (1994). Our study of HBC 722 demonstrated that accretion-related outbursts can occur in young stellar objects even with very low mass disks, in the late Class II phase.

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“…Prominent examples from the literature include V899 Mon, which has had repeated bursts separated by ∼1 year (Ninan et al 2015), and V1647 Ori, which repeats at ∼2 years (Aspin & Reipurth 2009). On even longer timescales, other EXor type stars tend to outburst once or twice per decade.…”

Section: Discussion and Summarymentioning

confidence: 99%

A Continuum of Accretion Burst Behavior in Young Stars Observed by K2

Cody

Hillenbrand

David

et al. 2017

ApJ

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We present 29 likely members of the young ρ Oph or Upper Sco regions of recent star formation that exhibit "accretion burst" type light curves in K2 time series photometry. The bursters were identified by visual examination of their ∼80 day light curves, though all satisfy the M < −0.25 flux asymmetry criterion for burst behavior defined by Cody et al. (2014). The burst sources represent ≈9% of cluster members with strong infrared excess indicative of circumstellar material. Higher amplitude burster behavior is correlated with larger inner disk infrared excesses, as inferred from WISE W 1 − W 2 color. The burst sources are also outliers in their large Hα emission equivalent widths. No distinction between bursters and non-bursters is seen in stellar properties such as multiplicity or spectral type. The frequency of bursters is similar between the younger, more compact ρ Oph region, and the older, more dispersed Upper Sco region. The bursts exhibit a range of shapes, amplitudes (∼10-700%), durations (∼1-10 days), repeat time scales (∼3-80 days), and duty cycles (∼10-100%). Our results provide important input to models of magnetospheric accretion, in particular by elucidating the properties of accretion-related variability in the low state between major longer duration events such as EX Lup and FU Ori type accretion outbursts. We demonstrate the broad continuum of accretion burst behavior in young stars -extending the phenomenon to lower amplitudes and shorter timescales than traditionally considered in the theory of pre-main sequence accretion history.

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V1647 Orionis: Optical Photometric and Spectroscopic Monitoring Through the 2003-2006 Outburst

Cited by 33 publications

References 57 publications

The Continuing Outburst of V1647 Orionis: Winter/Spring 2011 Observations

The Continuing Outburst of V1647 Orionis: Winter/Spring 2011 Observations

Multiwavelength study of the low-luminosity outbursting young star HBC 722

A Continuum of Accretion Burst Behavior in Young Stars Observed by K2

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