TESTING THE BINARY TRIGGER HYPOTHESIS IN FUors

Green, Joel D.; Kraus, Adam L.; Rizzuto, Aaron C.; Ireland, Michael; Dupuy, Trent J.; Mann, Andrew W.; Kuruwita, Rajika

doi:10.3847/0004-637x/830/1/29

Cited by 16 publications

(17 citation statements)

References 49 publications

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“…Binarity and outburst behavior has been examined in several studies (e.g., Bonnell & Bastien 1992;Reipurth et al 2002;Millan-Gabet et al 2006;Green et al 2016). As noted earlier, FU Ori is itself a 0 5 binary, and disk-binary interactions could promote an episodic or burst mode of accretion (Reipurth & Aspin 2004).…”

Section: Discussionmentioning

confidence: 99%

“…"Outside-in" models are those in which gravitationally bound fragments develop at large radii (tens of astronomical units or more) due to infall from a protostellar envelope, then migrate inward through the disk, ultimately generating an outburst when they accrete onto the star (e.g., Vorobyov & Basu 2015). A third option that has been posited is an external perturber-the interaction of the disk with an exterior massive object that alters the balance of accretion and triggers the cascading flow (Bonnell & Bastien 1992), although recent studies suggest the refill rate is too slow to occur on few coorbit timescales (Green et al 2016). The wavelength dependence of any postoutburst variability can distinguish among these classes of models.…”

Section: Introductionmentioning

confidence: 99%

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The Mid-Infrared Evolution of the Fu Orionis Disk

Green

Jones

Keller

et al. 2016

ApJ

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We present new SOFIA-FORCAST observations obtained in 2016 February of the archetypal outbursting lowmassyoung stellar object FU Orionis, and wecompare the continuum, solid-state, and gas properties with midinfrareddata obtained at the same wavelengths in 2004 with Spitzer-IRS. In this study, we conduct the first midinfraredspectroscopic comparison of an FUor over a long time period. Over a 12-year period, UBVR monitoring indicates that FU Orionis has continued its steady decrease in overall brightness by ∼14%. We find that this decrease in luminosity occurs only at wavelengths 20 μm. In particular, the continuum shortward of the silicate emission complex at 10 μm exhibits a ∼12% (∼3σ) drop in flux densitybut no apparent change in slope; both the Spitzer and SOFIA spectra are consistent with a 7200 K blackbody. Additionally, the detection of water absorption is consistent with the Spitzer spectrum. The silicate emission feature at 10 μm continues to be consistent with unprocessed grains, unchanged over 12 years. We conclude that either the accretion rate in FU Orionis has decreased by ∼12-14% over this time baselineorthe inner disk has cooled, but the accretion disk remains in a superheated state outside the innermost region.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Mid-Infrared Evolution of the Fu Orionis Disk

Green

Jones

Keller

et al. 2016

ApJ

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“…As discussed in Sec 4.2, HBC 494 might also be a binary, pending confirmation from higher resolution observations. However, studies trying to connect disc outburst with multiplicity have so far been inconclusive (e.g., Millan-Gabet et al 2006;Green et al 2016) and there is no clear evidence that the multiplicity statistics from outbursting sources are any different from those of non-outbursting young stellar objects. Everything considered (low-disc mass and lack of clear connection with multiplicity), it seems likely that the EXor phenomenon is connected to instabilities of the inner disc (e.g., D Angelo & Spruit 2012) and/or planet-disc interactions (Clarke et al 1990, Lodato & Clarke 2004).…”

Section: Implications For Outburst Mechanismmentioning

confidence: 99%

The ALMA early science view of FUor/EXor objects – V. Continuum disc masses and sizes

Cieza

Ruíz-Rodríguez

Pérez

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Low-mass stars build a significant fraction of their total mass during short outbursts of enhanced accretion known as FUor and EXor outbursts. FUor objects are characterized by a sudden brightening of ∼5 magnitudes at visible wavelengths within one year and remain bright for decades. EXor objects have lower amplitude outbursts on shorter timescales. Here we discuss a 1.3 mm ALMA mini-survey of eight outbursting sources (three FUor, four EXor, and the borderline object V1647 Ori) in the Orion Molecular Cloud. While previous papers in this series discuss the remarkable molecular outflows observed in the three FUor objects and V1647 Ori, here we focus on the continuum data and the differences and similarities between the FUor and EXor populations. We find that FUor discs are significantly more massive (∼80-600 M JU P ) than the EXor objects (∼0.5-40 M JU P ). We also report that the EXor sources lack the prominent outflows seen in the FUor population. Even though our sample is small, the large differences in disc masses and outflow activity suggest that the two types of objects represent different evolutionary stages.The FUor sources seem to be rather compact (R c < 20-40 au) and to have a smaller characteristic radius for a given disc mass when compared to T Tauri stars. V1118 Ori, the only known close binary system in our sample, is shown to host a disc around each one of the stellar components. The disc around HBC 494 is asymmetric, hinting at a structure in the outer disc or the presence of a second disc.

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“…Bonnell & Bastien (1992) initially suggested that FUor outbursts are induced by the tidal effect of the companion object in a binary system. At least some FUors are in binaries (e.g Koresko et al 1991;Green et al 2016…”

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confidence: 99%

The JCMT Transient Survey: Detection of Submillimeter Variability in a Class I Protostar EC 53 in Serpens Main

Yoo

Lee

Mairs

et al. 2017

ApJ

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During the protostellar phase of stellar evolution, accretion onto the star is expected to be variable, but this suspected variability has been difficult to detect because protostars are deeply embedded. In this paper, we describe a sub-mm luminosity burst of the Class I protostar EC 53 in Serpens Main, the first variable found during our dedicated JCMT/SCUBA-2 monitoring program of eight nearby star-forming regions. EC 53 remained quiescent for the first 6 months of our survey, from February to August 2016. The sub-mm emission began to brighten in September 2016, reached a peak brightness of 1.5 times the faint state, and has been decaying slowly since February 2017. The change in submm brightness is interpreted as dust heating in the envelope, generated by a luminosity increase of the protostar of a factor of ≥ 4. The 850 µm lightcurve resembles the historical K-band lightcurve, which varies by a factor of ∼ 6 with a 543 period and is interpreted as accretion variability excited by interactions between the accretion disk and a close binary system. The predictable detections of accretion variability observed at both near-infrared and sub-mm wavelengths make the system a unique test-bed, enabling us to capture the moment of the accretion burst and to study the consequences of the outburst on the protostellar disk and envelope.

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TESTING THE BINARY TRIGGER HYPOTHESIS IN FUors

Cited by 16 publications

References 49 publications

The Mid-Infrared Evolution of the Fu Orionis Disk

The Mid-Infrared Evolution of the Fu Orionis Disk

The ALMA early science view of FUor/EXor objects – V. Continuum disc masses and sizes

The JCMT Transient Survey: Detection of Submillimeter Variability in a Class I Protostar EC 53 in Serpens Main

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