Light curves of the latest FUor: Indication of a close binary

Hackstein, M.; Haas, Martín; Kóspál, Á.; Hambsch, F. J.; Chini, R.; Ábrahám, P.; Moór, A.; Núñez, F. Pozo; Ramolla, M.; Westhues, C.; Kaderhandt, L.; Fein, Ch.; Domínguez, A. Barr; Hodapp, Klaus W.

doi:10.1051/0004-6361/201527127

Cited by 20 publications

(23 citation statements)

References 26 publications

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“…V960 Mon went into outburst in 2014 and shows all the necessary spectral properties of a bona fide FUor (Kóspál et al 2015 andreferences therein, Connelley &Reipurth 2018). Based on periodic oscillations in the outburst light curve, Hackstein et al (2015) suggests that it is a close binary. Kóspál et al (2015) studied the SED of the progenitor and found that it indicates the presence of a moderately flared disk and an outer envelope in the system, whose total mass is between 0.1-0.7 M , if we scale it to the new Gaia distance of 1574 pc from the previously assumed 450 pc.…”

Section: V960 Monmentioning

confidence: 99%

Massive compact disks around FU Orionis-type young eruptive stars revealed by ALMA

Kóspál,

de Miera,

White

et al. 2021

Preprint

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FU Orionis-type objects (FUors) are low-mass pre-main sequence stars undergoing a temporary, but significant increase of mass accretion rate from the circumstellar disk onto the protostar. It is not yet clear what triggers the accretion bursts and whether the disks of FUors are in any way different from disks of non-bursting young stellar objects. Motivated by this, we conducted a 1.3 mm continuum survey of ten FUors and FUor-like objects with ALMA, using both the 7 m array and the 12 m array in two different configurations to recover emission at the widest possible range of spatial scales. We detected all targeted sources and several nearby objects as well. To constrain the disk structure, we fit the data with models of increasing complexity from 2D Gaussian to radiative transfer, enabling comparison with other samples modeled in a similar way. The radiative transfer modeling gives disk masses that are significantly larger than what is obtained from the measured millimeter fluxes assuming optically thin emission, suggesting that the FUor disks are optically thick at this wavelength. In comparison with samples of regular Class II and Class I objects, the disks of FUors are typically a factor of 2.9-4.4 more massive and a factor of 1.5-4.7 smaller in size. A significant fraction of them (65-70%) may be gravitationally unstable.

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Section: V960 Monmentioning

confidence: 99%

Massive compact disks around FU Orionis-type young eruptive stars revealed by ALMA

Kóspál,

de Miera,

White

et al. 2021

Preprint

Self Cite

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“…Results of photometric observations were presented in several studies. According to the result of Hackstein et al (2015), the maximum magnitude of V960 Mon was observed on 2014 October 6, which was 10.8 and 10.2 mag in the Sloan r-and i-bands, respectively. The brightness of V960 Mon gradually decreased by 0.5 -1 mag in the optical wavelength between 2014 October and 2015 April.…”

Section: Introductionmentioning

confidence: 96%

The Spectroscopic Variations of the FU Orionis Object V960 Mon

Takagi

Honda

Arai

et al. 2018

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We present the results of the spectroscopic monitoring of the FU Orionis type star V960 Mon. Spectroscopic variations of a FU Orionis type star will provide valuable information of its physical nature and the mechanism of the outburst. We conducted medium-resolution (R∼10000) spectroscopic observations of V960 Mon with 2m Nayuta telescope at the Nishi-Harima Astronomical Observatory, from 2015 January to 2017 January for 53 nights in total. We focused on Hα line and nearby atomic lines, and detected the strength variations in both absorption and emission lines. The observed variation in the equivalent width of the absorption lines correspond to a decrease in effective temperature and increase in surface gravity. These variations were likely to originate from the luminosity fading of the accretion disk due to the decrease in mass accretion rate.

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“…The information of brightness variation of V960 Mon during the period when the high-resolution spectra were observed is vital for understanding its spectroscopic variations. The brightness of V960 Mon in the r-and i-bands in 2014 October were 2.9 mag brighter than those in the quiescent phase (Hackstein et al 2015). The light curve of V960 Mon during the period when the spectra were collected was created with data of the American Association of Variable Star Observers (AAVSO).…”

Section: Brightness Variationmentioning

confidence: 99%

“…The maximum magnitude was ∼3 mag brighter in the optical wavelength compared to the quiescent phase. V960 Mon gradually faded by 0.5-1 mag between October 2014 and April 2015 (Hackstein et al 2015), and it kept fading with a lower rate. Spectroscopic observations of V960 Mon in the early phase of the outburst demonstrated typical characteristics of FUors.…”

Section: Introductionmentioning

confidence: 98%

Revealing the Spectroscopic Variations of FU Orionis Object V960 Mon with High-resolution Spectroscopy

Takagi

Honda

Arai

et al. 2020

ApJ

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We present the results of the high-resolution spectroscopy of the FU Orionis-type star V960 Mon. The brightness of V960 Mon decreased continuously after the outburst was detected in 2014 November. During this dimming event, we have carried out medium-resolution spectroscopic monitoring observations and found that the equivalent width of the absorption features showed variations. To further investigate the spectroscopic variations, we conducted a highresolution spectroscopic observation of V960 Mon with the Subaru Telescope and the High Dispersion Spectrograph on 2018 January 8 and 2020 February 1. By comparing this spectrum with the archival data of the Keck Observatory and the High Resolution Echelle Spectrometer taken between 2014 and 2017, we found that the absorption profiles changed as V960 Mon faded. The line profile of absorption lines such as Fe I and Ca I can be explained by a sum of the spectra of the disk atmosphere and the central star. The model spectrum created to explain the variations of the line profiles suggests that the effective temperature of the central star is ∼5500 K, which is comparable to that of the pre-outburst phase with a distance of 1.6 kpc with Gaia. The spectrum also shows that the effective temperature of the disk atmosphere decreased as V960 Mon faded. The variations of the Hα and Ca II lines (8498.0 Å, 8542.1 Å) also show that the V960 Mon spectrum became central-star dominant.

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Light curves of the latest FUor: Indication of a close binary

Cited by 20 publications

References 26 publications

Massive compact disks around FU Orionis-type young eruptive stars revealed by ALMA

Massive compact disks around FU Orionis-type young eruptive stars revealed by ALMA

The Spectroscopic Variations of the FU Orionis Object V960 Mon

Revealing the Spectroscopic Variations of FU Orionis Object V960 Mon with High-resolution Spectroscopy

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