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Publication . Preprint . Article . 2017

An UXor among FUors: Extinction-related Brightness Variations of the Young Eruptive Star V582 Aur

Péter Ábrahám; Kóspál; M. Kun; O. Fehér; G. Zsidi; J. A. Acosta-Pulido; M. I. Carnerero; +20 Authors
Open Access
Published: 13 Dec 2017 Journal: The Astrophysical Journal, volume 853, issue 1, page 28 (eissn: 1538-4357, Copyright policy )
Country: Hungary

V582 Aur is an FU Ori-type young eruptive star in outburst since $\sim$1985. The eruption is currently in a relatively constant plateau phase, with photometric and spectroscopic variability superimposed. Here we will characterize the progenitor of the outbursting object, explore its environment, and analyse the temporal evolution of the eruption. We are particularly interested in the physical origin of the two deep photometric dips, one occurred in 2012, and one is ongoing since 2016. We collected archival photographic plates, and carried out new optical, infrared, and millimeter wave photometric and spectroscopic observations between 2010 and 2017, with high sampling rate during the current minimum. Beside analysing the color changes during fading, we compiled multiepoch spectral energy distributions, and fitted them with a simple accretion disk model. Based on pre-outburst data and a millimeter continuum measurement, we suggest that the progenitor of the V582 Aur outburst is a low-mass T Tauri star with average properties. The mass of an unresolved circumstellar structure, probably a disk, is 0.04 M$_{\odot}$. The optical and near-infrared spectra demonstrate the presence of hydrogen and metallic lines, show the CO bandhead in absorption, and exhibit a variable H$\alpha$ profile. The color variations strongly indicate that both the $\sim$1 year long brightness dip in 2012, and the current minimum since 2016 are caused by increased extinction along the line of sight. According to our accretion disk models, the reddening changed from $A_V$=4.5 mag to 12.5 mag, while the accretion rate remained practically constant. Similarly to the models of the UXor phenomenon of intermediate and low-mass young stars, orbiting disk structures could be responsible for the eclipses.

Comment: 20 pages, 11 figures, accepted for publication in ApJ

Subjects by Vocabulary

arXiv: Astrophysics::Solar and Stellar Astrophysics Astrophysics::Galaxy Astrophysics Astrophysics::Earth and Planetary Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics::High Energy Astrophysical Phenomena

Microsoft Academic Graph classification: Brightness Physics Astrophysics Star (graph theory) Extinction


Solar and Stellar Astrophysics (astro-ph.SR), FOS: Physical sciences, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astronomy and Astrophysics

47 references, page 1 of 5

Acosta-Pulido, J. A., Kun, M., A´braha´m, P., et al. 2007, AJ, 133, 2020

Ansdell, M., Williams, J. P., van der Marel, N., et al. 2016, ApJ, 828, 46

Aspin, C., & Reipurth, B. 2009, AJ, 138, 1137

Audard, M., A´ braha´m, P., Dunham, M. M., et al. 2014, ArXiv e-prints, arXiv:1401.3368

Beckwith, S. V. W., Sargent, A. I., Chini, R. S., & Guesten, R. 1990, AJ, 99, 924

Bibo, E. A., & The, P. S. 1990, A&A, 236, 155

Bouvier, J., Grankin, K., Ellerbroek, L. E., Bouy, H., & Barrado, D. 2013, A&A, 557, A77

Bouvier, J., Alencar, S. H. P., Boutelier, T., et al. 2007, A&A, 463, 1017

Cardelli, J. A., Clayton, G. C., & Mathis, J. S. 1989, ApJ, 345, 245

Cepa, J., Aguiar-Gonzalez, M., Bland-Hawthorn, J., et al. 2003, in Proc. SPIE, Vol. 4841, Instrument Design and Performance for Optical/Infrared Ground-based Telescopes, ed. M. Iye & A. F. M. Moorwood, 1739-1749

Funded by
Structured ACCREtion Disks: initial conditions for planet formation in the time domain
  • Funder: European Commission (EC)
  • Project Code: 716155
  • Funding stream: H2020 | ERC | ERC-STG
Validated by funder
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