INVESTIGATING 2MASS J06593158-0405277: AN FUor BURST IN A TRIPLE SYSTEM?

Garatti, A. Caratti o; Lopez, R. Garcia; Ray, T. P.; Eislöffel, J.; Stecklum, B.; Scholz, Alexander; Kraus, Stefan; Weigelt, G.; Kreplin, Alexander; Шенаврин, В. И.

doi:10.1088/2041-8205/806/1/l4

Cited by 11 publications

(1 citation statement)

References 33 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A final possibility is that the gravitational force of a companion star may perturb the disc and thus enhance accretion (Bonnell & Bastien 1992). This idea is supported by the fact that a number of known eruptive variables are members of binary systems (see e.g., Fedele et al 2007;Reipurth et al 2010;Caratti o Garatti et al 2015). In some of these, both stars in the system are found to have characteristics of strong accretors (e.g.…”

Section: Outburst Mechanismmentioning

confidence: 99%

Determining the recurrence time-scale of long-lasting YSO outbursts

Peña

Naylor

Morrell

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We have determined the rate of large accretion events in class I and II young stellar objects (YSOs) by comparing the all-sky digitised photographic plate surveys provided by SuperCOSMOS with the latest data release from Gaia (DR2). The long mean baseline of 55 years along with a large sample of class II YSOs (≃15,000) allows us to study approximately 1 million YSO-years. We find 139 objects with ∆R ≥ 1 mag, most of which are found at amplitudes between 1 and 3 mag. The majority of YSOs in this group show irregular variability or long-lasting fading events, which is best explained as hot spots due to accretion or by variable extinction. There is a tail of YSOs at ∆R ≥ 3 mag and they seem to represent a different population. Surprisingly many objects in this group show high-amplitude irregular variability over timescales shorter than 10 years, in contrast with the view that high-amplitude objects always have long outbursts. However, we find 6 objects that are consistent with undergoing large, long lasting accretion events, 3 of them previously unknown. This yields an outburst recurrence timescale of 112 kyr, with a 68% confidence interval [74 to 180] kyr. This represents the first robust determination of the outburst rate in class II YSOs and shows that YSOs in their planet-forming stage do in fact undergo large accretion events, and with timescales of ≃100,000 years. In addition, we find that outbursts in the class II stage are ≃10 times less frequent than during the class I stage.

show abstract

Section: Outburst Mechanismmentioning

confidence: 99%

Determining the recurrence time-scale of long-lasting YSO outbursts

Peña

Naylor

Morrell

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

Accretion Bursts from Young Stars

Garatti

Eislöffel

2019

Astrophysics and Space Science Proceedings

View full text Add to dashboard Cite

The past photometric history of the FU Ori-type young eruptive star 2MASS J06593158-0405277 = V960 Mon

Jurdana-Šepić

Munari

2016

New Astronomy

View full text Add to dashboard Cite

The known FU Ori-type young eruptive stars are exceedingly rare (a dozen or so confirmed objects) and 2MASS J06593158-0405277, with its 2014 outburst, is likely the latest addition to the family. All members have displayed just one such eruption in their recorded history, an event lasting for decades. To test the FU Ori nature of 2MASS J06593158-0405277, we have reconstructed its photometric history by measuring its brightness on Harvard photographic plates spanning the time interval . No previous large amplitude eruption similar to that initiated in 2014 has been found, as in bona fide FU Ori-type objects. The median value of the brightness in quiescence of 2MASS J06593158-0405277 is B=15.5, with the time interval 1935-1950 characterized by a large variability (∼1 mag amplitude) that contrasts with the remarkable photometric stability displayed at later epochs. The variability during 1935-1950 can either be ascribed to some T Tau like activity of 2MASS J06593158-0405277 itself or to the also young and fainter star 2MASS J06593168-0405224 that lies 5 arcsec to the north and forms an unresolved pair at the astrometric scale of Harvard photographic plates.

show abstract

INVESTIGATING 2MASS J06593158-0405277: AN FUor BURST IN A TRIPLE SYSTEM?

Cited by 11 publications

References 33 publications

Determining the recurrence time-scale of long-lasting YSO outbursts

Determining the recurrence time-scale of long-lasting YSO outbursts

Accretion Bursts from Young Stars

The past photometric history of the FU Ori-type young eruptive star 2MASS J06593158-0405277 = V960 Mon

Contact Info

Product

Resources

About