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

Aspin, C.

doi:10.1088/0004-6256/142/4/135

Cited by 32 publications

(52 citation statements)

References 56 publications

(113 reference statements)

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“…The observed eruption of V1647 Ori appears to have characteristics similar to those of FUor and EXor, and it is assumed to be inbetween the two types. According to Aspin (2011), the viewing inclination angle of the star/disk system can play a significant role in the observed spectral features. Therefore, it is assumed that the two types of outbursts may be much closer in nature.…”

Section: Resultsmentioning

confidence: 99%

Optical photometric and spectral study of the new FU Orionis object V2493 Cygni (HBC 722)

Semkov

Peneva

Munari

et al. 2012

A&A

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Aims. We present new results from optical photometric and spectroscopic observations of the eruptive pre-main sequence star V2493 Cyg (HBC 722). The object has continued to undergo significant brightness variations over the past few months and is an ideal target for follow-up observations. Methods. We carried out CCD BVRI photometric observations in the field of V2493 Cyg ("Gulf of Mexico") from August 1994 to April 2012, i.e. at the pre-outburst states and during the phases of the outburst. We acquired high, medium, and low resolution spectroscopy of V2493 Cyg during the outburst. To study the pre-outburst variability of the target and construct its historical light curve, we searched for archival observations in photographic plate collections. Both CCD and photographic observations were analyzed using 15 comparison stars in the field of V2493 Cyg. Results. The pre-outburst photographic and CCD photometric observations of V2493 Cyg show low-amplitude light variations typical of T Tauri stars. The recent photometric data show a slow light decrease from October 2010 to June 2011 followed by an increase in brightness that continued until early 2012. The spectral observations of V2493 Cyg are typical of FU Orionis stars absorption spectra with strong P Cyg profiles of Hα and Na I D lines. On the basis of photometric monitoring performed over the past two years, the spectral properties at the maximal light, as well as the shape of long-term light curves, we confirm that the observed outburst of V2493 Cyg is of FU Orionis type.

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Section: Resultsmentioning

confidence: 99%

Optical photometric and spectral study of the new FU Orionis object V2493 Cygni (HBC 722)

Semkov

Peneva

Munari

et al. 2012

A&A

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“…In recent studies, such a scenario is used to explain the light variability of two PMS objects with characteristics similar to those of FUor and EXor -V1647 Ori (Aspin et al 2009b;Aspin 2011) and V2492 Cyg (Hillenbrand et al 2013;Kóspál et al 2013). It seems that the time variable extinction is characteristic not only of some Herbig Ae/Be stars (UXor variables) but is also a common phenomenon during the evolution of all types of PMS stars.…”

Section: Discussionmentioning

confidence: 99%

“…Due to the large-scale optical and infrared monitoring programs carried out in several observatories and the contributions of amateur astronomers, some new objects have been observed to undergo large amplitude outbursts, V733 Cep (Reipurth et al 2007;Peneva et al 2010), A&A 556, A60 (2013) V2493 Cyg Miller et al 2011;Kóspál et al 2011), V2492 Cyg (Aspin 2011;Hillenbrand et al 2013;Kóspál et al 2013), V2494 Cyg (Aspin et al 2009a), V2495 Cyg (Movsessian et al 2006), V900 Mon (Reipurth et al 2012), V2775 Ori (Fischer et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Photometric and spectroscopic variability of the FUor star V582 Aurigae

Semkov¹,

Peneva²,

Munari³

et al. 2013

A&A

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Aims. We present results from optical photometric and spectroscopic observations of the eruptive pre-main sequence star V582 Aur. Variability of the star was reported a few years ago when it was suspected as a possible FU Orionis object. Due to the small number of currently known FUors, a new object of this type is ideal target for follow-up photometric and spectroscopic observations. Methods. We carried out BVRI CCD photometric observations in the field of V582 Aur from 2009 August to 2013 February. We acquired high-, medium-, and low-resolution spectroscopy of V582 Aur during this period. To study the pre-outburst variability of the target and construct its historical light curve, we searched for archival observations in photographic plate collections. Both CCD and photographic observations were analyzed using a sequence of 14 stars in the field of V582 Aur calibrated in BVRI. Results. The pre-outburst photographic observations of V582 Aur show low-amplitude light variations typical of T Tauri stars. Archival photographic observations indicate that the increase in brightness began in late 1984 or early 1985 and the star reached the maximum level of brightness at 1986 January. The spectral type of V582 Aur can be defined as G0I with strong P Cyg profiles of Hα and Na I D lines, which are typical of FU Orionis objects. Our BVRI photometric observations show large amplitude variations (ΔV ∼ 2. m 8) during the 3.5 year period of observations. Most of the time, however, the star remains in a state close to the maximum brightness. The deepest drop in brightness was observed in the spring of 2012, when the brightness of the star fell to a level close to the pre-outburst. The multicolor photometric data show a color reversal during the minimum in brightness, which is typical of UX Ori variables. The corresponding spectral observations show strong variability in the profiles and intensities of the spectral lines (especially Hα), which indicate significant changes in the accretion rate. On the basis of photometric monitoring performed over the past three years, the spectral properties of the maximal light, and the shape of the long-term light curve, we confirm the affiliation of V582 Aur to the group of FU Orionis objects.

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“…Some variability studies, such as the VVV survey and YSOVar, have targeted specific regions in the near-and mid-IR (e.g., Cody et al 2014;Contreras Peña et al 2017). However, these optical/near-IR searches are not sensitive to the most embedded (youngest) objects and include brightness changes related to variability in the line-of-sight extinction (e.g., Aspin 2011;Hillenbrand et al 2013), while submillimeter luminosity should change only as the result of a variation in the protostellar luminosity.…”

Section: Summary and Future Perspectivesmentioning

confidence: 99%

How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions

Herczeg

Johnstone

Mairs

et al. 2017

ApJ

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Most protostars have luminosities that are fainter than expected from steady accretion over the protostellar lifetime. The solution to this problem may lie in episodic mass accretion-prolonged periods of very low accretion punctuated by short bursts of rapid accretion. However, the timescale and amplitude for variability at the protostellar phase is almost entirely unconstrained. In A James Clerk Maxwell Telescope/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions, we are monitoring monthly with SCUBA-2 the submillimeter emission in eight fields within nearby ( 500 < pc) star-forming regions to measure the accretion variability of protostars. The total survey area of ∼1.6 deg 2 includes ∼105 peaks with peaks brighter than 0.5 Jy/ beam (43 associated with embedded protostars or disks) and 237 peaks of 0.125-0.5 Jy/beam (50 with embedded protostars or disks). Each field has enough bright peaks for flux calibration relative to other peaks in the same field, 1 which improves upon the nominal flux calibration uncertainties of submillimeter observations to reach a precision of ∼2%-3% rms, and also provides quantified confidence in any measured variability. The timescales and amplitudes of any submillimeter variation will then be converted into variations in accretion rate and subsequently used to infer the physical causes of the variability. This survey is the first dedicated survey for submillimeter variability and complements other transient surveys at optical and near-IR wavelengths, which are not sensitive to accretion variability of deeply embedded protostars.

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

Cited by 32 publications

References 56 publications

Optical photometric and spectral study of the new FU Orionis object V2493 Cygni (HBC 722)

Optical photometric and spectral study of the new FU Orionis object V2493 Cygni (HBC 722)

Photometric and spectroscopic variability of the FUor star V582 Aurigae

How Do Stars Gain Their Mass? A JCMT/SCUBA-2 Transient Survey of Protostars in Nearby Star-forming Regions

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