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Brightness variations of the FUor-type eruptive star V346 Nor

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Á. Kóspál, P. Ábrahám, Ch. Westhues, M. Haas

Solar and Stellar Astrophysics · Submitted 1 Jan 2017

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We found that before 2008, the flux changes of V346 Nor were caused by a correlated change of extinction and accretion rate, while the minimum around 2010 was mostly due to decreasing accretion.

how it is stated · asserted 1.00 read the record →

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arXiv ID1701.00250 (version 1)
Pith ID3DPOJAHK, Pith's permanent record of this paper and its review
Citation\'A. K\'osp\'al, Ch. Westhues, M. Haas, P. \'Abrah\'am. "Brightness variations of the FUor-type eruptive star V346 Nor." arXiv:1701.00250 (2017). https://pith.science/paper/3DPOJAHK
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The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 7,123 input tokens.

What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.56 · human participants 0.01 · controlled comparison 0.07 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.82 · mentions code or data availability 0.03.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; .

Decades after the beginning of its FU Orionis-type outburst, V346 Nor unexpectedly underwent a fading event of $\Delta{}K$ = 4.6 mag around 2010. We obtained near-infrared observations and re-analysed 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 arcsec (30 au). The VISTA data outlined a well-defined minimum in the light curve at 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 reached the 2008 level yet. 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 before 2008, the flux changes of V346 Nor 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 maximal accretion rate of ${\approx}10^{-4} M_{\odot}$ yr$^{-1}$ in 1992. A combination of accretion and extinction changes was already invoked in the literature to interpret the flux variations of certain embedded young eruptive stars.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 Decades after the beginning of its FU Orionis-type outburst, V346 Nor unexpectedly underwent a fading event of $\Delta{}K$ = 4.6 mag around 2010. background 0.81 0.18 0.08 asserted 1.00
s1 We obtained near-infrared observations and re-analysed data from the VISTA/VVV survey to outline the brightness evolution. method 0.86 0.96 0.03 asserted 0.95
s2 In our VLT/NaCO images, we discovered a halo of scattered light around V346~Nor with a size of about 0.04 arcsec (30 au). result 0.99 0.97 0.05 asserted 1.00
s3 The VISTA data outlined a well-defined minimum in the light curve at late 2010/early 2011, and tentatively revealed a small-amplitude periodic modulation of 58 days. result 1.00 0.95 0.08 hedged possibility 0.75
s4 Our latest data points from 2016 demonstrate that the source is still brightening but has not reached the 2008 level yet. result 1.00 0.92 0.10 asserted 1.00
s5 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. method 1.00 0.96 0.05 asserted 0.98
s6 We found that before 2008, the flux changes of V346 Nor were caused by a correlated change of extinction and accretion rate, while the minimum around 2010 was mostly due to decreasing accretion. interpretation 0.93 0.94 0.66 asserted 1.00
s7 The source reached a maximal accretion rate of ${\approx}10^{-4} M_{\odot}$ yr$^{-1}$ in 1992. result 1.00 0.70 0.05 asserted 1.00
s8 A combination of accretion and extinction changes was already invoked in the literature to interpret the flux variations of certain embedded young eruptive stars. background 1.00 0.04 0.04 asserted 0.97

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.81.

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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

Decades after the beginning of its FU Orionis-type outburst, V346 Nor unexpectedly underwent a fading event of $\Delta{}K$ = 4.6 mag around 2010. We obtained near-infrared observations and re-analysed 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 arcsec (30 au). The VISTA data outlined a well-defined minimum in the light curve at 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 reached the 2008 level yet. 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 before 2008, the flux changes of V346 Nor 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 maximal accretion rate of ${\approx}10^{-4} M_{\odot}$ yr$^{-1}$ in 1992. A combination of accretion and extinction changes was already invoked in the literature to interpret the flux variations of certain embedded young eruptive stars.

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