AN ANALYSIS OF THE ENVIRONMENTS OF FU ORIONIS OBJECTS WITH<i>HERSCHEL</i>

Green, Joel D.; Evans, Neal J.; Kóspál, Á.; Herczeg, Gregory J.; Quanz, Sascha P.; Henning, Thomas; Kempen, T. A. van; Lee, Jeong Eun; Dunham, Michael M.; Meeus, G.; Bouwman, J.; Chen, Jo-Hsin; Güdel, M.; Skinner, Stephen L.; Liebhart, A.; Merello, Manuel

doi:10.1088/0004-637x/772/2/117

Cited by 39 publications

(60 citation statements)

References 80 publications

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“…LDN 981 stretches from west to east behind V1331 Cyg, and turns north slightly east of the star. The dark cloud morphology corresponds to what has been seen in emission at coarse resolution with SCUBA (Sandell & Weintraub 2001) and Herschel/SPIRE (Green et al 2013). …”

Section: Gap Extinction Analysis Using Ukidss Imagessupporting

confidence: 69%

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Hubbleimaging of V1331 Cygni: proper motion study of its circumstellar structures

Choudhary

Stecklum

Linz

2016

A&A

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Aims. The young star V1331 Cyg received previous attention because it is surrounded by an optical, arc-like reflection nebula. V1331 Cyg is commonly considered to be a candidate for an object that has undergone an FU-Ori (FUOR) outbreak in the past. This in turn could lead to a time-varying appearance of the dusty arcs that may be revealed by multi-epoch imaging. In particular, a radial colour analysis of the dust arcs can then be attempted to check whether the radial grain size distribution was modified by a previous FUOR wind. Methods. Second-epoch imaging of V1331 Cyg was obtained by us in 2009 using the Hubble Space Telescope (HST). By comparing this to archival HST data from 2000, we studied the time evolution of the circumstellar nebulae. After a point spread function subtraction using model point spread functions, we used customised routines to perform a proper motion analysis. The nebula expansion was derived by deconvolving and correlating the two-epoch radial brightness profiles. Additional data from other facilities -TLS, UKIDSS, Spitzer, and Herschel -were also incorporated to improve our understanding of the star in terms of environment, viewing angle, bipolar outflow length, and the FUOR phenomenon. Results. The outer dust arc is found to be expanding at ≈14.8 ± 3.6 km s −1 on average. The expansion velocity for the inner ring is less consistent, between 0.8 km s −1 and 3.0 km s −1 . The derived radial colour profiles do not indicate a spatial separation of the dust grain sizes. The Herschel 160 µm images show for the first time thermal emission from dust probably residing in the outer arc. By viewing V1331 Cyg almost pole-on, the length of the bipolar outflow exceeds previous estimates by far. Conclusions. The outer arc expansion timescale is consistent with the implantation time of the CO torus, which supports the hypothesis of an outburst that occurred a few thousand years ago. The azimuthal colour variation of the outer arc is probably due to changes of the scattering angle, imposed by a tilt or helical geometry of the dust configuration.

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Section: Gap Extinction Analysis Using Ukidss Imagessupporting

confidence: 69%

“…Green et al 2013). The related observations with the bolometer cameras of PACS (Poglitsch et al 2010) took place on July 22, 2011 (operational day 800) and were contained in the observational IDs 1342225252-55.…”

Section: Herschel Observationsmentioning

confidence: 99%

Hubbleimaging of V1331 Cygni: proper motion study of its circumstellar structures

Choudhary

Stecklum

Linz

2016

A&A

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“…Herschel/ PACS spectra for eightPBRs were later obtained by the HOPS team as part of the Herschel open time (OT) program (Tobin et al 2016). The DIGIT program surveyed 94 young stellar objects in different evolutionary stages with Herschel and obtained far-IR spectra of 24 Herbig Ae/Be stars, 40 T Tauri stars,and 30 protostars in nearby (d  400 pc) star-forming regions (van Kempen et al 2010;Cieza et al 2013;Dionatos et al 2013;Fedele et al 2013;Green et al 2013bGreen et al , 2013aGreen et al , 2016Meeus et al 2013;Sturm et al 2013;Lee et al 2014bLee et al , 2014a. The Herschel/PACS spectra of 30 protostars in the DIGIT sample were presented in Green et al (2013b).…”

Section: The Samplementioning

confidence: 99%

“…Outbursts of varying intensities and frequencies have been observed in several young stars (e.g. , Herbig 1977;Kenyon 1995;Green et al 2006;Reipurth & Aspin 2010;Fischer et al 2012;Green et al 2013a;Audard et al 2014;Safron et al 2015). However, a detailed picture of the time evolution of mass accretion from the early protostellar phase to the late pre-main-sequence phase is still missing.…”

Section: Introductionmentioning

confidence: 99%

The Evolution of Far-Infrared Co Emission From Protostars

Manoj

Green

Megeath

et al. 2016

ApJ

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We investigate the evolution of far-IR CO emission from protostars observed with Herschel/PACS for 50 sources from the combined sample of HOPS and DIGIT Herschel key programs. From the uniformly sampled spectral energy distributions, whose peaks are well sampled, we computed the L bol , T bol ,and L L bol smm for these sources to search for correlations between far-IR CO emission and protostellar properties. We find a strong and tight correlation between far-IR CO luminosity (L CO fir ) and the bolometric luminosity (L bol ) of the protostars with µ L L CO fir bol 0.7 . We, however, do not find a strong correlation between L CO fir and protostellar evolutionary indicators, T bol and L L bol smm . FIRCO emission from protostars traces the currently shocked gas by jets/outflows, and far-IR CO luminosity, L CO fir , is proportional to the instantaneous mass-loss rate,Ṁ out . The correlation between L CO fir and L bol , then, is indicative of instantaneousṀ out tracking instantaneousṀ acc . The lack of acorrelation between L CO fir and evolutionary indicators T bol and L L bol smm suggests thatṀ out and, therefore,Ṁ acc do not show any clear evolutionary trend. These results are consistent with mass accretion/ejection in protostars being episodic. Taken together with the previous finding that the time-averaged mass-ejection/accretion rate declines during the protostellar phase, our results suggest that the instantaneous accretion/ejection rate of protostars is highly time variable and episodic, but the amplitude and/or frequency of this variability decreases with time such that the timeaveraged accretion/ejection rate declines with system age.

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“…Hence, the disk component which emits the near-infrared excess flux is physically coherent with both the disk and stellar components which emit optical light. Green et al (2013) detected 5.3 and 1.3 day periods of 10 −2 mag. amplitude scale.…”

Section: Near-infrared Light Curvementioning

confidence: 94%

Near-Ir Photometric Study of the Fu Orionis Object HBC 722

Sung¹,

Park²,

Yang³

et al. 2013

Journal of The Korean Astronomical Society

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We present near-infrared light curves of HBC 722 after its the September 2010 outburst. We have been monitoring its near-infrared light curves since November 2010 with Korean Astronomy and Space Science Institute Infrared Camera System (KASINICS). HBC 722 exhibits large changes in optical and near-infrared brightness since its outburst. The J, H, and K s light curves over about 2.5 years show that in all observed bands HBC 722 progressively became fainter until around April 2011, down to J ∼10.7, H ∼9.9, K s ∼9.3, but it is getting brighter again. Large scatter in the obtained light curve prevents us from finding whether there is any short timescale variation as reported in other optical observations. The near-infrared color of HBC 722 is becoming bluer since its outburst. The pre-outburst Spectral Energy Distribution (SED) of HBC 722 is consistent with that of a slightly reddened Class II YSO with the exception of the extraordinary IR-excess in the far-infrared region.

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AN ANALYSIS OF THE ENVIRONMENTS OF FU ORIONIS OBJECTS WITHHERSCHEL

Cited by 39 publications

References 80 publications

Hubbleimaging of V1331 Cygni: proper motion study of its circumstellar structures

Hubbleimaging of V1331 Cygni: proper motion study of its circumstellar structures

The Evolution of Far-Infrared Co Emission From Protostars

Near-Ir Photometric Study of the Fu Orionis Object HBC 722

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