HIGHLY VARIABLE EXTINCTION AND ACCRETION IN THE JET-DRIVING CLASS I-TYPE YOUNG STAR PTF 10nvg (V2492 Cyg, IRAS 20496+4354)

Hillenbrand, Lynne A.; Miller, A. A.; Covey, Kevin R.; Carpenter, John M.; Cenko, S. B.; Silverman, J. M.; Muirhead, Philip S.; Fischer, William J.; Crepp, Justin R.; Bloom, J.; Filippenko, A. V.

doi:10.1088/0004-6256/145/3/59

Cited by 65 publications

(89 citation statements)

References 109 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…If the near-infrared magnitude changes were caused by changing extinction, then the difference in A V between the peak of the outburst and our faintest observation in 2011 July would be about 20 mag. We note that Hillenbrand et al (2013) observed the source at an even fainter state, indicating that the full range of extinction changes can be even higher. Remarkably, the faintest colors from 2010−2012 are still significantly different from the quiescent colors measured in 2006.…”

Section: Color−color and Color−magnitude Diagramsmentioning

confidence: 77%

“…On shorter timescales, between 2011 August and December, the source seems to show ≈20-day-long quasiperiodic cycles. Recently, Hillenbrand et al (2013) presented well-sampled JHKs light curves and claimed to have found a 221-day period.…”

Section: Light Curvesmentioning

confidence: 99%

“…This suggests that, as opposed to the H I lines and the CO bandhead, the H 2 lines are not originating from close to the central star, but farther from it, probably from a jet. Hillenbrand et al (2013) present several spectra taken in 2011. Three of them were observed close in time (2011 June 26, July 15, and August 17) to our 2011 August 1 spectrum.…”

Section: Spectroscopymentioning

confidence: 99%

“…This makes V2492 Cyg remarkably similar to V1647 Ori and PV Cep, but with an unprecedentedly large amplitude in the A V changes. Further photometric and spectroscopic monitoring of the object is presented in Hillenbrand et al (2013).…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Exploring the circumstellar environment of the young eruptive star V2492 Cygni

Kóspál

Ábrahám

Acosta–Pulido

et al. 2013

A&A

View full text Add to dashboard Cite

Context. V2492 Cyg is a young eruptive star that went into outburst in 2010. The near-infrared color changes observed since the outburst peak suggest that the source belongs to a newly defined sub-class of young eruptive stars, where time-dependent accretion and variable line-of-sight extinction play a combined role in the flux changes. Aims. In order to learn about the origin of the light variations and to explore the circumstellar and interstellar environment of V2492 Cyg, we monitored the source at ten different wavelengths, between 0.55 μm and 2.2 μm from the ground and between 3.6 μm and 160 μm from space. Methods. We analyze the light curves and study the color−color diagrams via comparison with the standard reddening path. We examine the structure of the molecular cloud hosting V2492 Cyg by computing temperature and optical depth maps from the far-infrared data. Results. We find that the shapes of the light curves at different wavelengths are strictly self-similar and that the observed variability is related to a single physical process, most likely variable extinction. We suggest that the central source is episodically occulted by a dense dust cloud in the inner disk and, based on the invariability of the far-infrared fluxes, we propose that it is a long-lived rather than a transient structure. In some respects, V2492 Cyg can be regarded as a young, embedded analog of UX Orionis-type stars. Conclusions. The example of V2492 Cyg demonstrates that the light variations of young eruptive stars are not exclusively related to changing accretion. The variability provided information on an azimuthally asymmetric structural element in the inner disk. Such an asymmetric density distribution in the terrestrial zone may also have consequences for the initial conditions of planet formation.

show abstract

Section: Color−color and Color−magnitude Diagramsmentioning

confidence: 77%

Section: Light Curvesmentioning

confidence: 99%

Section: Spectroscopymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Exploring the circumstellar environment of the young eruptive star V2492 Cygni

Kóspál

Ábrahám

Acosta–Pulido

et al. 2013

A&A

View full text Add to dashboard Cite

show abstract

“…Objects like this are Hα11, PV Cep, V1647 Ori, and V899 Mon (Kun et al 2011a,b;Mosoni et al 2013;Ninan et al 2015). V346 Nor also resembles the young eruptive star V2492 Cyg in several aspects: the pre-outburst position of V2492 Cyg in the near-IR color-color diagram is close to the point of the 2010 minimum of V346 Nor, it also underwent a large accretion change at the beginning of its outburst, and in the high state, the line-of-sight extinction varies continuously (Kóspál et al 2011(Kóspál et al , 2013Hillenbrand et al 2013). Therefore, the observed variability in both V346 Nor and V2492 Cyg is governed by a combination of changing accretion and extinction.…”

Section: Discussionmentioning

confidence: 99%

Brightness variations of the FUor-type eruptive star V346 Normae

Kóspál

Ábrahám

Westhues

et al. 2017

A&A

View full text Add to dashboard Cite

Decades after the beginning of its FU Orionis-type outburst, V346 Nor unexpectedly underwent a fading event of ∆K = 4.6 mag around 2010. We obtained near-infrared observations and re-analyzed data from the VISTA/VVV survey to outline the brightness evolution. In our VLT/NaCO images, we discovered a halo of scattered light around V346 Nor with a size of about 0 . 04 (30 au). The VISTA data outlined a well-defined minimum in the light curve in late 2010/early 2011, and tentatively revealed a small-amplitude periodic modulation of 58 days. Our latest data points from 2016 demonstrate that the source is still brightening but has not yet reached the 2008 level. We used a simple accretion disk model with varying accretion rate and line-of-sight extinction to reproduce the observed near-infrared magnitudes and colors. We found that the flux changes of V346 Nor before 2008 were caused by a correlated change of extinction and accretion rate, while the minimum around 2010 was mostly due to decreasing accretion. The source reached a highest accretion rate of ≈10 −4 M yr −1 in 1992. A combination of accretion and extinction changes has been invoked in the literature to interpret the flux variations of certain embedded young eruptive stars.

show abstract