Photometric activity of the UX Ori star V1184 Tau in the optical and near-infrared spectral ranges

Гринин, В. П.; Arkharov, A. A.; Barsunova, O. Yu.; Сергеев, С. Г.; Тамбовцева, Л. В.

doi:10.1134/s1063773709020054

Cited by 26 publications

(26 citation statements)

References 19 publications

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“…Based on data from infrared JHK photometry, Grinin et al (2009) propose that the increase in extinction and the drop in star's brightness can be induced by enhanced accretion from the circumstellar disks. The lack of a fall in the K band is explained by a disk model with a puffed up inner rim, whose effective width is increased as a result of enhanced accretion rate.…”

Section: Resultsmentioning

confidence: 99%

“…In Semkov et al (2008), data from archival photographic plates are presented, which proves that an unknown minimum of brightness exists during the approximate period 1980-1985. Optical photometric data obtained at the time of our photometric monitoring have been published in Tackett et al (2003), Barsunova et al (2006), and Grinin et al (2009).…”

Section: Introductionmentioning

confidence: 99%

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The pre-main-sequence star V1184 Tauri (CB 34V) at the end of prolonged eclipse

Semkov

Peneva

Ibryamov

2015

A&A

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Aims. V1184 Tau (CB 34V) lies in the field of the Bok globule CB 34 and was discovered as a large amplitude variable in 1993. According to the first hypothesis of the variability of the star, it is a FU Orionis candidate erupted between 1951 and 1993. During subsequent observations, the star manifests large amplitude variability interpreted as obscuration from circumstellar clouds of dust. We included V1184 Tau (CB 34V) in our target list of highly variable pre-main-sequence stars to determine the reasons for the variations in the brightness of this object. Methods. Data from BVRI photometric observations of the young stellar object V1184 Tau, obtained in the period 2008−2015, are presented in the paper. These data are a continuation of our optical photometric monitoring of the star began in 2000 and continuing to date. The photometric observations of V1184 Tau were performed in two observatories with two medium-sized and two small telescopes. Results. Our results indicate that during periods of maximum light the star shows characteristics typical of T Tauri stars. During the observed deep minimum in brightness, however, V1184 Tau is rather similar to UX Orionis objects. The deep drop in brightness began in 2003 ended in 2015 as the star has returned to maximum light. The light curve during the drop is obviously asymmetric as the decrease in brightness lasts two times longer than the rise. The observed colour reverse on the colour-magnitude diagrams is also confirmation of obscuration from circumstellar clouds of dust as a reason for the large amplitude variability in the brightness.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The pre-main-sequence star V1184 Tauri (CB 34V) at the end of prolonged eclipse

Semkov

Peneva

Ibryamov

2015

A&A

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“…There is also a possibility of a "hybrid" scenario: increase of accretion rate is accompanied by increase of mass-loss, which, in turn, leads to increase in circumstellar extinction. This mechanism was discussed in [46] with reference to V1184 Tau.…”

Section: Discussionmentioning

confidence: 99%

A search for Keplerian periods in the brightness variations of T Tauri and Ae Herbig stars

2010

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Long-term, uniform series of UBVR observations of T Tauri and Herbig Ae stars obtained over 20 yr at the Maidanak Observatory as part of the ROTOR program are analyzed. We find a linear relationship between the characteristic variability time scale and the bolometric luminosity of the star+disk system: the higher the luminosity, the slower the brightness variations. This dependence is valid over a wide range of masses and luminosities, from T Tauri stars to Herbig Ae stars. On average, the variability time scale is one-quarter the Keplerian period at the dust-sublimation radius, which is known from interferometric observations. Some T Tauri stars have periods from 25 to 120 days, which are preserved over several observing seasons. These periods correspond to Keplerian orbits with semi-major axes from 0.14 to 0.52 AU. The results obtained provide indirect evidence for the existence of protoplanets in the gas-dust disks of stars in early stages of their evolution toward the main sequence.

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“…In any case, since optical and near-IR spectroscopic analyses have clearly revealed typical features indicative of ongoing accretion activity, such as veiling, CO bands in emission, and H i emission lines (Kun et al 2011;Antoniucci et al 2014a,b), we speculate that the photometric variations of V1180 Cas are the result of a combination of accretion-related and extinction-driven effects, as proposed in the cases of the pre-main sequence variables V2492 Cyg (Hillenbrand et al 2013) and V1184 Tau (Grinin et al 2009), whose light curves present several similarities with that of V1180 Cas. For the brightness dims of V2492 Cyg, Hillenbrand et al (2013) suggest semi-periodic occultations of the innermost regions by an orbiting dusty clump or disk warp.…”

Section: X-ray Luminosity and Nature Of The High-brightness Statementioning

confidence: 99%

“…For the brightness dims of V2492 Cyg, Hillenbrand et al (2013) suggest semi-periodic occultations of the innermost regions by an orbiting dusty clump or disk warp. Similarly, Grinin et al (2009) hypothesize that the faint states of V1184 Tau are due to obscuration of the central star region by the puffed-up inner rim of the disk, whose height would increase during higher accretion rate phases.…”

Section: X-ray Luminosity and Nature Of The High-brightness Statementioning

confidence: 99%

First X-ray detection of the young variable V1180 Cassiopeiae

Antoniucci

Nucita

Giannini

et al. 2015

A&A

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Context. V1180 Cas is a young variable that has shown strong photometric fluctuations (ΔI ∼ 6 mag) in the recent past, which have been attributed to events of enhanced accretion. The source has entered a new high-brightness state in September 2013, which we have previously analysed through optical and near-infrared spectroscopy. Aims. To investigate the current active phase of V1180 Cas, we performed observations with the Chandra satellite aimed at studying the X-ray emission from the object and its connection to accretion episodes. Methods. Chandra observations were performed in early August 2014. Complementary JHK photometry and J-band spectroscopy were taken at our Campo Imperatore facility to relate the X-ray and near-infrared emission from the target. Results. We observe a peak of X-ray emission at the nominal position of V1180 Cas and estimate that the confidence level of the detection is about 3σ. The observed signal corresponds to an X-ray luminosity L X (0.5−7 keV) in the range 0.8 ÷ 2.2 × 10 30 erg s −1 . Based on the relatively short duration of the dim states in the light curve and on stellar luminosity considerations, we explored the possibility that the brightness minima of V1180 Cas are driven by extinction variations. From the analysis of the spectral energy distribution of the high state we infer a stellar luminosity of 0.8−0.9 L and find that the derived L X is comparable to the average X-ray luminosity values observed in T Tauri objects. Moreover, the X-ray luminosity appears to be lower than the X-ray emission levels around 5 × 10 30 ÷ 1 × 10 31 erg s −1 detected at outbursts in similar low-mass objects. Conclusions. Our analysis suggests that at least part of the photometric fluctuations of V1180 Cas might be extinction effects rather than the result of accretion excess emission. However, because the source displays spectral features indicative of active accretion, we speculate that its photometric variations might be the result of a combination of accretion-induced and extinction-driven effects, as suggested for other young variables, such as V1184 Tau and V2492 Cyg.

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Photometric activity of the UX Ori star V1184 Tau in the optical and near-infrared spectral ranges

Cited by 26 publications

References 19 publications

The pre-main-sequence star V1184 Tauri (CB 34V) at the end of prolonged eclipse

The pre-main-sequence star V1184 Tauri (CB 34V) at the end of prolonged eclipse

A search for Keplerian periods in the brightness variations of T Tauri and Ae Herbig stars

First X-ray detection of the young variable V1180 Cassiopeiae

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